Nodes prefixed with a _ are not valid SPASE, but are included for debugging. Values prefixed with a x_ are not valid SPASE but may considered for addition for completeness.

This file contains numerical moments computed from measurements of the Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., Rev. Sci. Inst., in press 1993]. The moments are presented in s/c coordinates: the z-axis is aligned with the spin axis, which points radially toward the center of the Earth; the x-axis is in the plane containing the spacecraft spin axis and the spin axis of the Earth, with +X generally northward; and the y-axis points generally eastward. Polar angles are measured relative to the spin axis (+Z), and azimuthal angles are measured around the z-axis, with zero along the +X direction. The moments are computed for three 'species': lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 21.5 secs after the ion measurements. Epoch is the measurement time appropriate for the ions. The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined  spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined.  Tperp and Tpara are obtained from diagonalization of the  3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of  the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by  non-zero 'SCALEMIN' values in this file. A quality flag value of 1  indicates that the values are suspect because of unreliable location info. 

More LANL geosynchronous Magnetospheric Plasma Analyzer (MPA) information and plots at

Los Alamos National Laboratory Spacecraft Magnetospheric Plasma Analyzer

Journal of Geophysical Research article on the LANL MPA instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: Mike Henderson at LANL

Instructions for using web services to access this dataset an other other metadata and options for CDAWeb datasets. The ProductKey here corresponds to the query parameter 'dataset' in the tables at the AccessURL in a dataset-related request can be made.

Web service that generates a Python script to access this product.

SPDF/SSCWeb. Please also acknowledge the data producer: Mike Henderson at LANL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Mike Henderson at LANL

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API.

Web Service that generates plots. See https://hapi-server.org/plot/ for the API.

Generated from all.xml/@timerange_start and all.xml/@timerange_stop

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/01a_mpa/2001/a1_k0_mpa_20010831_v02.cdf. The most common cadence, 86016 [ms] = PT1M26.016S, occurred for 69.7674% of the 180 timesteps. 

Los Alamos National Laboratory 2001 (from all.xml/observatory/description/@short)

Magnetospheric plasma analyzer (from all.xml/instrument/description/@short)

Magnetospheric Science (from Master/CDFglobalAttributes/Discipline)

Los Alamos National Laboratory 2001 (from Master/CDFglobalAttributes/Source_name)

Processing level is not available in the master file; it should be there instead of, say, https://github.com/rweigel/cdawmeta-spase/blob/main/ProcessingLevel.json

Zero corresponds to 0000-01-01T00.00.000. See https://spdf.gsfc.nasa.gov/pub/software/cdf/doc/cdf390/cdf390ug.pdf

This variable is in the source CDF file. Not all web services will provide access to this variable in this form (e.g., an ISO 8601 string may be used). If the source of the CDF file is a different file type, it may be have been represented in a different format.

Velocity, 3 comp. in s/c coord., of low energy ions (1-130 eV/e)

Temperatures, parallel & perp. for high energy ions (.13-45 keV/e)

Proton symmetry axis: polar ang. relative to Earth direction, azim. ang. from north

Electron symmetry axis: polar ang. relative to Earth direction azim. ang. from north

[SPECIALIZED USE ONLY] [Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z)

Los Alamos Nation Laboratory spacecraft Magnetospheric Plasma Analyzer

Journal of Geophysical Research Article on the LANL MPA instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/02a_mpa/2003/a2_k0_mpa_20031029_v02.cdf. The most common cadence, 86016 [ms] = PT1M26.016S, occurred for 75.7090% of the 614 timesteps. 

Los Alamos National Laboratory 2002 (from all.xml/observatory/description/@short)

Los Alamos National Laboratory 2002 (from Master/CDFglobalAttributes/Source_name)

ACE attitude direction cosines (hourly values) in GSE and J2000 GCI coordinate systems

Found same URL in master and https://github.com/rweigel/cdawmeta-spase/blob/main/cdawmeta-spase/InformationURL.json; not using master for Name and Description.

The Satellite Situation Center Web, SSCWeb, Service has been developed and is operated jointly by the NASA/GSFC Space Physics Data Facility, SPDF, and the National Space Science Data Center, NSSDC, to support a Range of NASA Science Programs and to fulfill Key International NASA Responsibilities including those of NSSDC and the World Data Center-A for Rockets and Satellites. The Software and associated Database of SSCWeb together form a System to cast Geocentric Spacecraft Location Information into a Framework of Empirical Geophysical Regions and Mappings of Spacecraft Locations along Lines of the Earth's Magnetic Field. This Capability is one Key to Mission Science Planning, both Single Missions and Coordinated Observations of Multiple Spacecraft with Ground-Based Investigations, and to subsequent Multi-Mission Data Analysis.

SPDF/CDAWeb. Please also acknowledge the data producer: E. C. Stone at California Institute of Technology

SPDF/SSCWeb. Please also acknowledge the data producer: E. C. Stone at California Institute of Technology

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: E. C. Stone at California Institute of Technology

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/orbit/level_2_cdaweb/def_at/1997/ac_at_def_19970826_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 3071 timesteps. 

Advanced Composition Explorer (from all.xml/observatory/description/@short)

Interplanetary Studies (from Master/CDFglobalAttributes/Discipline)

Advanced Composition Explorer (from Master/CDFglobalAttributes/Source_name)

MAG - ACE Magnetic Field ExperimentReferences: http://www.srl.caltech.edu/ACE/The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

ACE Science Center site hosting instrument information, data release notes, as well as web utilities for plotting and downloading data

SPDF/CDAWeb. Please also acknowledge the data producer: N. Ness at Bartol Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: N. Ness at Bartol Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: N. Ness at Bartol Research Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_h0/1997/ac_h0_mfi_19970902_v04.cdf. The most common cadence, 16000 [ms] = PT16S, occurred for all 5399 timesteps. 

ACE Magnetic Field Instrument (from all.xml/instrument/description/@short)

SWEPAM - Solar Wind Electron Proton Alpha Monitor References: http://www.srl.caltech.edu/ACE/ The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

SPDF/CDAWeb. Please also acknowledge the data producer: D. J. McComas at SWRI

SPDF/SSCWeb. Please also acknowledge the data producer: D. J. McComas at SWRI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. J. McComas at SWRI

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swepam/level_2_cdaweb/swe_h0/1998/ac_h0_swe_19980204_v06.cdf. The most common cadence, 64000 [ms] = PT1M4S, occurred for all 1349 timesteps. 

ACE Solar Wind Electron Proton Alpha Monitor (from all.xml/instrument/description/@short)

The Electron, Proton, and Alpha Monitor (EPAM) is composed of five telescope apertures of three different types.  Two Low Energy Foil Spectrometers (LEFS) measure the flux and direction of electrons above 30 keV (geometry factor = 0.397 cm2*sr), two Low Energy Magnetic Spectrometers (LEMS) measure the flux  and direction of ions greater than 50 keV (geometry factor = 0.48 cm2*sr), and the Composition Aperture (CA) measures the elemental composition of the ions (geometry factor = 0.24 cm2*sr). The telescopes use the spin of the spacecraft to sweep the full sky. Solid-state detectors are used to measure the energy and composition of the incoming particles. For more information about the EPAM instrument, visit the EPAM Home Page at JHU/APL: http://sd-www.jhuapl.edu/ACE/EPAM/ The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

A web site hosting instrument information, data release notes, as well as web utilities for plotting and downloading data

SPDF/CDAWeb. Please also acknowledge the data producer: R. Gold at JHU/APL

SPDF/SSCWeb. Please also acknowledge the data producer: R. Gold at JHU/APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Gold at JHU/APL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/epam/level_2_cdaweb/epm_h1/1997/ac_h1_epm_19970830_v04.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for 80.0000% of the 64 timesteps. 

ACE Electron Proton Alpha Monitor (from all.xml/instrument/description/@short)

5-minute Level 2 data (from Master/CDFglobalAttributes/Data_type)

P1 LEMS30 (Low Energy Magnetic Spectrometer; 0.047-0.065 MeV Ions), Sector Avg

P2 LEMS30 (Low Energy Magnetic Spectrometer; 0.065-0.112 MeV Ions), Sector Avg

P3 LEMS30 (Low Energy Magnetic Spectrometer; 0.112-0.187 MeV Ions), Sector Avg

P4 LEMS30 (Low Energy Magnetic Spectrometer; 0.187-0.310 MeV Ions), Sector Avg

P5 LEMS30 (Low Energy Magnetic Spectrometer; 0.310-0.580 MeV Ions), Sector Avg

P6 LEMS30 (Low Energy Magnetic Spectrometer; 0.580-1.06 MeV Ions), Sector Avg

P7 LEMS30 (Low Energy Magnetic Spectrometer; 1.06-1.91 MeV Ions), Sector Avg

P8 LEMS30 (Low Energy Magnetic Spectrometer; 1.91-4.75 MeV Ions), Sector Avg

P1 LEMS30 (Low Energy Magnetic Spectrometer; 0.047-0.065 MeV Ions), Uncertainty

P2 LEMS30 (Low Energy Magnetic Spectrometer; 0.065-0.112 MeV Ions), Uncertainty

P3 LEMS30 (Low Energy Magnetic Spectrometer; 0.112-0.187 MeV Ions), Uncertainty

P4 LEMS30 (Low Energy Magnetic Spectrometer; 0.187-0.310 MeV Ions), Uncertainty

P5 LEMS30 (Low Energy Magnetic Spectrometer; 0.310-0.580 MeV Ions), Uncertainty

P6 LEMS30 (Low Energy Magnetic Spectrometer; 0.580-1.06 MeV Ions), Uncertainty

P7 LEMS30 (Low Energy Magnetic Spectrometer; 1.06-1.91 MeV Ions), Uncertainty

P8 LEMS30 (Low Energy Magnetic Spectrometer; 1.91-4.75 MeV Ions), Uncertainty

DE1 DE (Deflected Electrons; 0.038-0.053 MeV Electrons), Sector Avg

DE2 DE (Deflected Electrons; 0.053-0.103 MeV Electrons), Sector Avg

DE3 DE (Deflected Electrons; 0.103-0.175 MeV Electrons), Sector Avg

DE4 DE (Deflected Electrons; 0.175-0.315 MeV Electrons), Sector Avg

DE1 DE (Deflected Electrons; 0.038-0.053 MeV Electrons), Uncertainty

DE2 DE (Deflected Electrons; 0.053-0.103 MeV Electrons), Uncertainty

DE3 DE (Deflected Electrons; 0.103-0.175 MeV Electrons), Uncertainty

DE4 DE (Deflected Electrons; 0.175-0.315 MeV Electrons), Uncertainty

W3 CA60 (Composition Aperture; 0.389-1.28 MeV/nuc. He), Sector Avg

W4 CA60 (Composition Aperture; 1.28-6.98 MeV/nuc. He), Sector Avg

W5 CA60 (Composition Aperture; 0.465-1.71 MeV/nuc. CNO), Sector Avg

W6 CA60 (Composition Aperture; 1.71-19.1 MeV/nuc. CNO), Sector Avg

W7 CA60 (Composition Aperture; 0.239-0.840 MeV/nuc. Fe (9<Z<29)), Sector Avg

W8 CA60 (Composition Aperture; 0.840-92.7 MeV/nuc. Fe (9<Z<29)), Sector Avg

W3 CA60 (Composition Aperture; 0.389-1.28 MeV/nuc. He), Uncertainty

W4 CA60 (Composition Aperture; 1.28-6.98 MeV/nuc. He), Uncertainty

W5 CA60 (Composition Aperture; 0.465-1.71 MeV/nuc. CNO), Uncertainty

W6 CA60 (Composition Aperture; 1.71-19.1 MeV/nuc. CNO), Uncertainty

W7 CA60 (Composition Aperture; 0.239-0.840 MeV/nuc. Fe (9<Z<29)), Uncertainty

W8 CA60 (Composition Aperture; 0.840-92.7 MeV/nuc. Fe (9<Z<29)), Uncertainty

E1p LEFS60 (Low Energy Foil Spectrometer; 0.045-0.062 MeV Electrons (+Ions) ), Sector Avg

E2p LEFS60 (Low Energy Foil Spectrometer; 0.062-0.103 MeV Electrons (+Ions) ), Sector Avg

E3p LEFS60 (Low Energy Foil Spectrometer; 0.103-0.175 MeV Electrons (+Ions) ), Sector Avg

E4p LEFS60 (Low Energy Foil Spectrometer; 0.175-0.312 MeV Electrons (+Ions) ), Sector Avg

FP5p LEFS60 (Low Energy Foil Spectrometer; 0.546-0.761 MeV Ions), Sector Avg

FP6p LEFS60 (Low Energy Foil Spectrometer; 0.761-1.22 MeV Ions), Sector Avg

FP7p LEFS60 (Low Energy Foil Spectrometer; 1.22-4.97 MeV Ions), Sector Avg

E1p LEFS60 (Low Energy Foil Spectrometer; 0.045-0.062 MeV Electrons (+Ions) ), Uncertainty

E2p LEFS60 (Low Energy Foil Spectrometer; 0.062-0.103 MeV Electrons (+Ions) ), Uncertainty

E3p LEFS60 (Low Energy Foil Spectrometer; 0.103-0.175 MeV Electrons (+Ions) ), Uncertainty

E4p LEFS60 (Low Energy Foil Spectrometer; 0.175-0.312 MeV Electrons (+Ions) ), Uncertainty

FP5p LEFS60 (Low Energy Foil Spectrometer; 0.546-0.761 MeV Ions), Uncertainty

FP6p LEFS60 (Low Energy Foil Spectrometer; 0.761-1.22 MeV Ions), Uncertainty

FP7p LEFS60 (Low Energy Foil Spectrometer; 1.22-4.97 MeV Ions), Uncertainty

P1p LEMS120 (Low Energy Magnetic Spectrometer; 0.047-0.066 MeV Ions), Sector Avg

P2p LEMS120 (Low Energy Magnetic Spectrometer; 0.066-0.114 MeV Ions), Sector Avg

P3p LEMS120 (Low Energy Magnetic Spectrometer; 0.114-0.190 MeV Ions), Sector Avg

P4p LEMS120 (Low Energy Magnetic Spectrometer; 0.190-0.310 MeV Ions), Sector Avg

P5p LEMS120 (Low Energy Magnetic Spectrometer; 0.310-0.580 MeV Ions), Sector Avg

P6p LEMS120 (Low Energy Magnetic Spectrometer; 0.580-1.05 MeV Ions), Sector Avg

P7p LEMS120 (Low Energy Magnetic Spectrometer; 1.05-1.89 MeV Ions), Sector Avg

P8p LEMS120 (Low Energy Magnetic Spectrometer; 1.89-4.75 MeV Ions), Sector Avg

P1p LEMS120 (Low Energy Magnetic Spectrometer; 0.047-0.066 MeV Ions), Uncertainty

P2p LEMS120 (Low Energy Magnetic Spectrometer; 0.066-0.114 MeV Ions), Uncertainty

P3p LEMS120 (Low Energy Magnetic Spectrometer; 0.114-0.190 MeV Ions), Uncertainty

P4p LEMS120 (Low Energy Magnetic Spectrometer; 0.190-0.310 MeV Ions), Uncertainty

P5p LEMS120 (Low Energy Magnetic Spectrometer; 0.310-0.580 MeV Ions), Uncertainty

P6p LEMS120 (Low Energy Magnetic Spectrometer; 0.580-1.05 MeV Ions), Uncertainty

P7p LEMS120 (Low Energy Magnetic Spectrometer; 1.05-1.89 MeV Ions), Uncertainty

P8p LEMS120 (Low Energy Magnetic Spectrometer; 1.89-4.75 MeV Ions), Uncertainty

E1 LEFS150 (Low Energy Foil Spectrometer; 0.045-0.062 MeV Electrons (+Ions) ), Sector Avg

E2 LEFS150 (Low Energy Foil Spectrometer; 0.062-0.102 MeV Electrons (+Ions) ), Sector Avg

E3 LEFS150 (Low Energy Foil Spectrometer; 0.102-0.175 MeV Electrons (+Ions) ), Sector Avg

E4 LEFS150 (Low Energy Foil Spectrometer; 0.175-0.312 MeV Electrons (+Ions) ), Sector Avg

FP5  LEFS150 (Low Energy Foil Spectrometer; 0.540-0.765 MeV Ions), Sector Avg

FP6 LEFS150 (Low Energy Foil Spectrometer; 0.765-1.22 MeV Ions), Sector Avg

FP7 LEFS150 (Low Energy Foil Spectrometer; 1.22-4.94 MeV Ions), Sector Avg

E1 LEFS150 (Low Energy Foil Spectrometer; 0.045-0.062 MeV Electrons (+Ions) ), Uncertainty

E2 LEFS150 (Low Energy Foil Spectrometer; 0.062-0.102 MeV Electrons (+Ions) ), Uncertainty

E3 LEFS150 (Low Energy Foil Spectrometer; 0.102-0.175 MeV Electrons (+Ions) ), Uncertainty

E4 LEFS150 (Low Energy Foil Spectrometer; 0.175-0.312 MeV Electrons (+Ions) ), Uncertainty

FP5 LEFS150 (Low Energy Foil Spectrometer; 0.540-0.765 MeV Ions), Uncertainty

FP6 LEFS150 (Low Energy Foil Spectrometer; 0.765-1.22 MeV Ions), Uncertainty

FP7 LEFS150 (Low Energy Foil Spectrometer; 1.22-4.94 MeV Ions), Uncertainty

ACE Magnetic Field (MAG) Instrument Home Page at the University of New Hampshire

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_h1/1997/ac_h1_mfi_19970902_v04.cdf. The most common cadence, 240000 [ms] = PT4M, occurred for all 359 timesteps. 

The Solar Isotope Spectrometer (SIS) is designed to provide high resolution measurements of the isotopic composition of energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to ~100 MeV/nucleon. During large  solar events, when particle fluxes can increase over quiet-time values by factors of up to 10000, SIS measures the isotopic composition of the solar corona, while during solar quiet times SIS measures the isotopes of low-energy Galactic cosmic rays and the composition of the anomalous cosmic rays which are thought to originate in the nearby interstellar medium.  The solar energetic particle measurements are useful to further our understanding of the Sun, while also providing a baseline for comparison with the Galactic cosmic ray measurements carried out by CRIS.  SIS has a geometry factor of ~40 cm2--sr, which is significantly larger than previous satellite solar particle isotope spectrometers. It is also designed to provide excellent mass resolution during the extremely high particle flux conditions which occur during large solar particle events.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/sis/level_2_cdaweb/sis_h1/1997/ac_h1_sis_19970829_v04.cdf. The most common cadence, 256000 [ms] = PT4M16S, occurred for 40.6528% of the 137 timesteps. 

ACE Solar Isotope Spectrometer (from all.xml/instrument/description/@short)

256-sec Level 2 data (from Master/CDFglobalAttributes/Data_type)

The Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer(ACE) spacecraft is intended to be a major step in ascertaining the isotopic composition of the Galactic Cosmic Rays(GCRs) and hence a major step in determining their origin. The GCRs consist, by number, primarily of hydrogen nuclei(~92%) and helium nuclei (~7%). The energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to ~100 MeV/nucleon. During large  solar events, when particle fluxes can increase over quiet-time values by factors of up to 10000, CRIS measures the isotopic composition of the solar corona, while during solar quiet times CRIS measures the isotopes of low-energy Galactic cosmic rays and the composition of the anomalous cosmic rays which are thought to originate in the nearby interstellar medium.  The solar energetic particle measurements are useful to further our understanding of the Sun, while also providing a baseline for comparison with the Galactic cosmic ray measurements carried out by CRIS.  CRIS has a geometry factor of ~40 cm2--sr, which is significantly larger than previous satellite solar particle isotope spectrometers. It is also designed to provide excellent mass resolution during the extremely high particle flux conditions which occur during large solar particle events.

ACE Cosmic Ray Isotope Spectrometer (CRIS) Level 2 data Home Page

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/cris/level_2_cdaweb/cris_h2/1997/ac_h2_cris_19970827_v06.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

ACE Cosmic Ray Isotope Spectrometer (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/epam/level_2_cdaweb/epm_h2/1997/ac_h2_epm_19970830_v06.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 6 timesteps. 

FP5 LEFS150 (Low Energy Foil Spectrometer; (0.540-0.765 MeV Ions), Sector Avg

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_h2/1997/ac_h2_mfi_19970902_v04.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

The SEPICA Instrument on ACE   The Solar Energetic Particle Ionic Charge Analyzer is the sensor on ACE, which is used to determine the charge state distribution of energetic particle distributions.SEPICA is designed to measure the ionic charge state, Q, the kinetic energy, E, and the nuclear charge, Z, of energetic ions above 0.2 MeV/Nuc. This includes ions accelerated in solar flares as well as in  interplanetary space during energetic storm particle (ESP) and co-rotating interaction region (CIR) events. For low mass numbers SEPICA also separates isotopes -- for example, 3He and 4He. For more information about the SEPICA instrument, visit the SEPICA Home Page at University of New Hampshire: http://www.ssg.sr.unh.edu/tof/Missions/Ace/index.html?sepicamain.html The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

ACE Solar Energetic Particle Ionic Charge Analyzer (SEPICA) Instrument Home Page at the University of New Hampshire

SPDF/CDAWeb. Please also acknowledge the data producer: Eberhard Moebius at University of New Hampshire

SPDF/SSCWeb. Please also acknowledge the data producer: Eberhard Moebius at University of New Hampshire

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Eberhard Moebius at University of New Hampshire

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/sepica/level_2_cdaweb/sep_h2/1997/ac_h2_sep_19971008_v05.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

The Solar Energetic Particle Ionic Charge Analyzer (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/sis/level_2_cdaweb/sis_h2/1997/ac_h2_sis_19970829_v07.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

McComas, D.J., Bame, S.J., Barker, P., Feldman, W.C., Phillips, J.L., Riley, P., and J.W. Griffee, Solar Wind Electron Proton Alpha Monitor (SWEPAM) for the Advanced Composition Explorer, Space Sci. Rev., 86, 563–612, 1998

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swepam/level_2_cdaweb/swe_h2/1998/ac_h2_swe_19980204_v06.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

SWICS 1.1 - The Solar Wind Ion Composition Spectrometer prior to August 23 2011 - determines uniquely the chemical and ionic-charge composition of the solar wind, the temperatures and mean speeds of major solar wind ions, at all speeds above 300 km/s (protons) and 170 km/s  (Fe+16), and resolves H and He isotopes of solar and interstellar sources. SWICS 1.1 measures the distribution functions of the interstellar cloud and dust cloud pickup ions up to energies of 100 keV/e.For more information about the SWICS instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

ACE Solar Wind Ion Composition Spectrometer (SWICS) Instrument Home Page at the University of Maryland

SPDF/CDAWeb. Please also acknowledge the data producer: G. Gloeckler at University of Maryland

SPDF/SSCWeb. Please also acknowledge the data producer: G. Gloeckler at University of Maryland

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Gloeckler at University of Maryland

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swics/level_2_cdaweb/swi_h2/1998/ac_h2_swi_19980204_v09.cdf. The most common cadence, 3635000 [ms] = PT1H35S, occurred for 43.4783% of the 10 timesteps. 

Solar Wind Ion Composition Spectrometer 1.1 (from all.xml/instrument/description/@short)

ACE/ULEIS Solar Suprathermal and Energetic Particle Intensities 1-Hour Level 2 Data

The ULEIS Instrument on ACE   The Ultra Low Energy Isotope Spectrometer measures ion fluxes over the charge range from H through Ni from about 20 keV/nucleon to 10 MeV/nucleon, thus covering both suprathermal and energetic particle energy ranges. Exploratory measurements of ultra-heavy species (mass range above Ni) will also be performed in a more limited energy range near 0.5 MeV/nucleon. ULEIS will be studying the elemental and isotopic composition of solar energetic particles, and the mechanisms by which these particles are energized in the solar corona. ULEIS will also investigate mechanisms by which supersonic interplanetary shock waves energize ions.For more information about the ULEIS instrument, visit the ULEIS Home Page at JHU/APL: http://sd-www.jhuapl.edu/ACE/ULEIS/ The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

SPDF/CDAWeb. Please also acknowledge the data producer: G. Mason at University of Maryland

SPDF/SSCWeb. Please also acknowledge the data producer: G. Mason at University of Maryland

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Mason at University of Maryland

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/uleis/level_2_cdaweb/ule_h2/1998/ac_h2_ule_19980220_v04.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

Ultra Low Energy Isotope Spectrometer (from all.xml/instrument/description/@short)

ACE/CRIS Cosmic Ray Isotope Spectrometer Daily-averaged Level 2 Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/cris/level_2_cdaweb/cris_h3/1997/ac_h3_cris_19970827_v04.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 126 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/epam/level_2_cdaweb/epm_h3/1997/ac_h3_epm_19970831_v01.cdf. The most common cadence, 12000 [ms] = PT12S, occurred for 96.2306% of the 6944 timesteps. 

12-second Level 2 data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_h3/1998/ac_h3_mfi_19980101_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 86.4802% of the 74718 timesteps. 

SWICS 2.0 is The Solar Wind Ion Composition Spectrometer after August 23 2011 when a radiation and age-induced hardware anomaly altered the instrument's operational state. It should not be confused with SWICS 1.1, the recalibrated data set extending from launch up to the anomaly. SWICS 2.0 determines uniquely the chemical and ionic-charge composition of the solar wind, and the mean speed of solar wind He ions. For more information about the SWICS instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

Additional details provided by the instrument team. All users of SWICS data should read these notes.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swics/level_2_cdaweb/sw2_h3/2012/ac_h3_sw2_20120601_v03.cdf. The most common cadence, 7206000 [ms] = PT2H6S, occurred for 54.5455% of the 6 timesteps. 

Solar Wind Ion Composition Spectrometer 2.0 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swics/level_2_cdaweb/swi_h3/1998/ac_h3_swi_19980204_v04.cdf. The most common cadence, 7272000 [ms] = PT2H1M12S, occurred for 36.3636% of the 4 timesteps. 

SWICS 1.1 - The Solar Wind Ion Composition Spectrometer prior to August 23 2011 determines uniquely the chemical and ionic-charge composition of the solar wind, the temperatures and mean speeds of major solar wind ions, at all speeds above 300 km/s (protons) and 170 km/s  (Fe+16), and resolves H and He isotopes of solar and interstellar sources. SWICS 1.1 measures the distribution functions of the interstellar cloud and dust cloud pickup ions up to energies of 100 keV/e.For more information about the SWICS instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swics/level_2_cdaweb/swi_h4/1998/ac_h4_swi_19980204_v06.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 15.1057% of the 50 timesteps. 

SWICS 1.1 - The Solar Wind Ion Composition Spectrometer prior to August 23 2011 determines uniquely the chemical and ionic-charge composition of the solar wind, the temperatures and mean speeds of major solar wind ions, at all speeds above 300 km/s (protons) and 170 km/s  (Fe+16), and resolves H and He isotopes of solar and interstellar sources. SWICS measures the distribution functionsof the interstellar cloud and dust cloud pickup ions up to energies of 100 keV/e.For more information about the SWICS instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swics/level_2_cdaweb/swi_h5/1998/ac_h5_swi_19980204_v03.cdf. The most common cadence, 7272000 [ms] = PT2H1M12S, occurred for 36.3636% of the 4 timesteps. 

Solar Wind Ion Composition Spectrometer (from all.xml/instrument/description/@short)

2-hour Level 2 charge-state distributions (from Master/CDFglobalAttributes/Data_type)

Carbon Solar Wind charge state distribution statistical uncrtainty

Oxygen Solar Wind charge state distribution statistical uncertainty

Neon Solar Wind charge state distribution statistical uncertainty

Magnesium Solar Wind charge state distribution statistical uncertainty

Silicon Solar Wind charge state distribution statistical uncertainty

Iron Solar Wind charge state distribution statistical uncertainty

SWICS - The Solar Wind Ion Composition Spectrometer determines uniquely the chemical and ionic-charge composition of the solar wind, the temperatures and mean speeds of major solar wind ions, at all speeds above 300 km/s (protons) and 170 km/s  (Fe+16), and resolves H and He isotopes of solar and interstellar sources. SWICS measures the distribution functions of the interstellar cloud and dust cloud pickup ions up to energies of 100 keV/e.For more information about the SWICS instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.The quality of ACE level 2 data is such that it is suitable for serious scientific study.  However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team membersbefore publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swics/level_2_cdaweb/swi_h6/1998/ac_h6_swi_19980129_v03.cdf. The most common cadence, 726000 [ms] = PT12M6S, occurred for 58.4746% of the 69 timesteps. 

12min Level 2 proton data (from Master/CDFglobalAttributes/Data_type)

EPAM - ACE Electron, Proton, and Alpha MonitorReferences: http://www.srl.caltech.edu/ACE/ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. EPAM Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies. 

ACE Electron, Proton, and Alpha Monitor (EPAM) Instrument Home Page at the Applied Physics Laboratory, Johns Hopkins University

SPDF/CDAWeb. Please also acknowledge the data producer: R. Gold at JHU Applied Physics Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: R. Gold at JHU Applied Physics Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Gold at JHU Applied Physics Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/epam/level_2_cdaweb/epm_k0/2017/ac_k0_epm_20170701_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

ACE Electron, Proton, and Alpha Monitor (from all.xml/instrument/description/@short)

5-Min Key Parameter Data (from Master/CDFglobalAttributes/Data_type)

MAG - ACE Magnetic Field ExperimentReferences: http://www.srl.caltech.edu/ACE/ 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_k0/2017/ac_k0_mfi_20170701_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

5-min Key Parameter [PRELIM] (from Master/CDFglobalAttributes/Data_type)

[PRELIMINARY VALUES - BROWSE USE ONLY] Magnetic Field, Cartesian GSE coord

SIS - ACE Solar Isotope SpectrometerReferences: http://www.srl.caltech.edu/ACE/ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SIS Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/sis/level_2_cdaweb/sis_k0/2017/ac_k0_sis_20170701_v04.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

1-Hr Key Parameter Data (from Master/CDFglobalAttributes/Data_type)

SWEPAM - Solar Wind Electron Proton Alpha Monitor References: http://www.srl.caltech.edu/ACE/ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SWEPAM Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies. 

SPDF/CDAWeb. Please also acknowledge the data producer: D. J. McComas at Southwest Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: D. J. McComas at Southwest Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. J. McComas at Southwest Research Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swepam/level_2_cdaweb/swe_k0/2017/ac_k0_swe_20170701_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

5-Min Key Parameter [PRELIM] (from Master/CDFglobalAttributes/Data_type)

[PRELIMINARY VALUES - BROWSE USE ONLY] Solar Wind Proton Number Density, scalar

[PRELIMINARY VALUES - BROWSE USE ONLY] Percent of Helium++ ions to protons

[PRELIMINARY VALUES - BROWSE USE ONLY] radial component of the proton temperature

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/epam/level_2_cdaweb/epm_k1/2017/ac_k1_epm_20170701_v04.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

MAG - ACE Magnetic Field ExperimentReferences: http:// www.srl.caltech.edu/ACE/ 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_k1/2017/ac_k1_mfi_20170701_v02.cdf. The most common cadence, 16000 [ms] = PT16S, occurred for 99.9815% of the 5398 timesteps. 

16-sec Key Parameter [PRELIM] (from Master/CDFglobalAttributes/Data_type)

[PRELIMINARY VALUES - BROWSE USE ONLY] RMS of Magnetic Field (16 sec period)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/swepam/level_2_cdaweb/swe_k1/2017/ac_k1_swe_20170701_v02.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

1-Hour Key Parameter (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_k2/2017/ac_k2_mfi_20170701_v03.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

1-Hr Key Parameter Data [PRELIM] (from Master/CDFglobalAttributes/Data_type)

ACE orbit data (daily values) in GSE and J2000 GCI coordinate systems

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/orbit/level_2_cdaweb/def_or/1997/ac_or_def_19970826_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 10109 timesteps. 

GROUP 1    Satellite   Resolution   Factor            ace           720         1                                                                                    Coord/            Min/Max   Range Filter       FilterComponent   Output Markers  Minimum  Maximum   Mins/Maxes GSE X        YES      -        -        -           -        -           -   GSE Y        YES      -        -        -           -        -           -   GSE Z        YES      -        -        -           -        -           -   GSE Lat      YES      -        -        -           -        -           -   GSE Lon      YES      -        -        -           -        -           -                                                                                       Addtnl             Min/Max   Range Filter       FilterOptions     Output Markers  Minimum  Maximum   Mins/MaxesdEarth       YES      -        -        -           -                                                                                       Formats and units:                              Day/Time format: YYYY DDD HH:MM    Degrees/Hemisphere format: Decimal degrees with 2 place(s).        Longitude 0 to 360, latitude -90 to 90.    Distance format: Kilometers with 2 place(s).

SPDF/CDAWeb. Please also acknowledge the data producer: SSC/SSCWeb at NASA's GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: SSC/SSCWeb at NASA's GSFC

Web Service to this product. Note that the parameter names in this SPASE record may differ from the parameter names used by this web service and additional parameters may be available.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: SSC/SSCWeb at NASA's GSFC

SPDF/SSCWeb and the HAPI project. Please also acknowledge the data producer: SSC/SSCWeb at NASA's GSFC

Web Service to this product using the HAPI interface. Note that the parameter names in this SPASE record may differ from the parameter names used by this web service and additional parameters may be available.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/orbit/level_2_cdaweb/or_ssc/ac_or_ssc_19970101_v01.cdf. The most common cadence, 720000 [ms] = PT12M, occurred for all 15391 timesteps. 

Satellite Situation Center Ephemeris (from all.xml/instrument/description/@short)

Each AeroCube-6 vechicle carries three dosimeters measuring electrons with energies from about 43 keV to about 830 keV and protons with enegies ranging from 370 keV to 12 MeV. The dataset manager, Dr. Paul O'Brien, can be reached at paul.obrien@aero.org. The data are described in AeroCube-6 Dosimeter Data README (v3.0), Aerospace Report No. TOR-2016-01155, The Aerospace Corporation, March 4, 2016, El Segundo, CA. Also see AeroCube-6 Dosimeter Equivalent Energy Thresholds and Flux Conversion Factors, Aerospace Report No. TOR-2017-02598, The Aerospace Corporation, July 1, 2019, El Segundo, CA.

The AC6 Principal Investigator is Dr. J. Bern Blake. Aerospace and government personnel who contributed to the AeroCube-6 mission: T.P. O'Brien, D. Hinkley, C. Venturini, J. Avrett, D. Mabry, W. Crain, C. Nguyen, B. Hardy, J. Lee, D. Turner, D. Rowen, C. Coffman, B. Barney, P. Doyle, J. Fuller, D. Pedrino, G. Maul, D. Rumsey, A. Chin, R. Stevens, A Schutte, D. Arndt, and E. Mazur.

Those wishing to use AC6 data are strongly urged to notify the PI of the topic of their work. This will enable the AC6 team to assist in use of the data and to track the instrument's utility to the broader community.

SPDF/CDAWeb. Please also acknowledge the data producer: J. B. Blake at The Aerospace Corporation

SPDF/SSCWeb. Please also acknowledge the data producer: J. B. Blake at The Aerospace Corporation

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. B. Blake at The Aerospace Corporation

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/aerocube/aerocube-6/aerocube6-a/dosimeter-cdf/2014/aerocube-6-a_dosimeter_l2_20140621_v1.0.0.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 118 timesteps. 

Magnetospheric Physics (from Master/CDFglobalAttributes/Discipline)

Dose3 rate (>860 keV electrons, 12 MeV protons AC6-A;  >11 MeV protons AC6-B)

bitmap: 0 - data OK, 1 - ground contact transmitter noise, 2- crosslink transmitter noise, 4 - dubious attitude, 8 - TLE ephemeris, 16 - dos3-A noisy day

Solar local time at equatorial crossing of IGRF magnetic field line through vehicle

Invariant latitude (McIlwain L) for locally mirroring particle, IGRF magnetic field

Solar local time at equatorial crossing of OPQ magnetic field line through vehicle

Invariant latitude (McIlwain L) for locally mirroring particle, OPQ magnetic field

0 - trapped, 1 - drift loss cone, 2 - bounce loss cone, -1 = open/unknown, for locally mirroring particles, OPQ magnetic field

Minimum magnetic field strength on field line through vehicle, OPQ magnetic field

Integral invariant for locally mirroring particle, OPQ magnetic field

Kaufmann invariant for locally mirroring particle, OPQ magnetic field

Kaufmann invariant for normally incident particle, OPQ magnetic field

Modified third invariant (L*) for locally mirroring particle, OPQ magnetic field

Modified third invariant (L*) for normally incident particle, OPQ magnetic field

Minimum mirror altitude around drift shell for locally mirroring particle, OPQ magnetic field

Minimum mirror altitude around drift shell for normally incident particle, OPQ magnetic field

Polar angle of near hemisphere loss cone (100 km), OPQ magnetic field

Polar angle of opposite hemisphere loss cone (100 km), OPQ magnetic field

OPQ magnetic field strength at 100 km altitude, northern hemisphere on field line through vehicle

Geodetic latitude at 100 km altitude, northern hemisphere, on OPQ magnetic field line through vehicle

Geodetic longitude at 100 km altitude, northern hemisphere, on OPQ magnetic field line through vehicle

OPQ magnetic field strength at 100 km altitude, southern hemisphere on field line through vehicle

Geodetic latitude at 100 km altitude, southern hemisphere, on OPQ magnetic field line through vehicle

Geodetic longitude at 100 km altitude, southern hemisphere, on OPQ magnetic field line through vehicle

Local pitch angle of normally incident particle, OPQ magnetic field

Local pitch angle of particle moving along spacecraft X axis, OPQ magnetic field

Local pitch angle of particle moving along spacecraft Y axis, OPQ magnetic field

Equatorial pitch angle of normally incident particle, OPQ magnetic field

Gyrophase angle of normally incident particle, OPQ magnetic field

Gyrophase angle of particle moving along spacecraft X axis, OPQ magnetic field

Gyrophase angle of particle moving along spacecraft Y axis, OPQ magnetic field

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/aerocube/aerocube-6/aerocube6-b/dosimeter-cdf/2014/aerocube-6-b_dosimeter_l2_20140621_v1.0.0.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 127 timesteps. 

Alouette-2 Topside Sounder Ionograms over Lima, Peru (Lat=-12, Long=283)

This ionogram was digitized from the original Alouette 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at https://nssdc/space/isis/isis-status.html

ISIS/Alouette Page maintained by NASA GSFC with Science and Instrument Descriptions, Data Access, Software, and Publication Lists

Information about the Swept Frequency Sounder, SFS, Experiment on Alouette 2

SPDF/CDAWeb. Please also acknowledge the data producer: R.F. Benson at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: R.F. Benson at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R.F. Benson at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/ionogram_cdaweb/alouette2/LIM_12S_283E/1966/315/alouette2_av_lim_1966315203408_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 98.6784% of the 224 timesteps. 

International Satellite for Ionosphere Studies 1 (from all.xml/observatory/description/@short)

Ionospheric Science (from Master/CDFglobalAttributes/Discipline)

International Satellite for Ionosphere Studies 1 (from Master/CDFglobalAttributes/Source_name)

Sounder amplitude at 335 virtual heights for fixed & swept frequency (ionogram)

Alouette-2 Topside Sounder Ionogram over Quito, Equador (lat/lon=-1/281)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/ionogram_cdaweb/alouette2/QUI_01S_281E/1965/333/alouette2_av_qui_1965333134739_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 98.7179% of the 231 timesteps. 

Sounder amplitude at 335 virtual heights for fixed & swept frequency

Alouette-2 Topside Sounder Ionogram over Santiago, Chile (lat/lon=-33/298)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/ionogram_cdaweb/alouette2/SNT_33S_298E/1965/333/alouette2_av_snt_1965333134237_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 96.3415% of the 79 timesteps. 

Alouette-2 Topside Sounder Ionogram over Falkland Is., U.K. (lat/lon=-52/302)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/ionogram_cdaweb/alouette2/SOL_52S_302E/1965/335/alouette2_av_sol_1965335013139_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 98.5646% of the 206 timesteps. 

Alouette-2 Topside Sounder Ionogram over Fairbanks, Alaska (lat/long=65/212)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/ionogram_cdaweb/alouette2/ULA_65N_212E/1965/alouette2_av_ula_1965333062012_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 79.8561% of the 111 timesteps. 

Alouette-2 Topside Sounder Ionogram over Winkfield, U.K. (lat/lon=51/359)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/ionogram_cdaweb/alouette2/WNK_51N_359E/1966/089/alouette2_av_wnk_1966089054819_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 943 timesteps. 

This data file contains topside electron density profiles as deduced from Alouette 2 topside sounder measurements. The data processing was done in the seventies at the Communications Research Center in Ottawa, Canada This data set provides data from 1000km down in steps of irregular step size. The x- and o-traces were manually  scaled from the ionograms and the inversion algorithm of J. Jackson was used to compute the density profiles from these traces.

SPDF/CDAWeb. Please also acknowledge the data producer: J. E. Jackson at Communication Research Centre (CRC), Ottawa

SPDF/SSCWeb. Please also acknowledge the data producer: J. E. Jackson at Communication Research Centre (CRC), Ottawa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. E. Jackson at Communication Research Centre (CRC), Ottawa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/alouette/crc_ne_profile_cdf/alouette2/1965/alouette2_neprof_tops_19651215_v01.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 45.4039% of the 163 timesteps. 

International Satellite for Ionosphere Studies 2 (from all.xml/observatory/description/@short)

International Satellite for Ionosphere Studies 2 (from Master/CDFglobalAttributes/Source_name)

IRI-95 value for the natural logarithm of the F2 peak density in cm-3

This dataset contains high time resolution MEPA rate channel data. MEPA is a particle telescope with an ION head and a TOF head. The TOF head can measure species and energy, while the ION head only measures the energy of the ions, which are mostly protons. In fact, the counts in the ION head are all assumed to be protons up to 1830 keV. The ION head has 10 energy channels, and so the first 8 channels (that are all below 1830 keV) are assumed to be all protons, and the 2 channels above this are assumed to be all alphas. The TOF head has 9 energy channels that are generic (ions of any species are counted) and some species specific channels for protons, helium, oxygen, and iron. The AMPTE data was divided into records, with each record holding data from 4 spins. In any record, all the TOF species channels are always present, but only one of either a) the 10 ION head channels or b) 9 TOF generic channels are present. The majority of records have the ION head channels. The AMPTE spacecraft had a spin period of about 6 seconds. The exact spin period varies slightly and is included in the data. MEPA data is sectored into 32 directions per spin. Nearly all channels are reported as sectored values, but to conserve telemetry, many channels are only read out every other spin, or every fourth spin. In this data, all values are summed so that they are reported every fourth spin. Note that in the original AMPTE datesets, there was a timing problem which required that 19.75 seconds (one Major Frame of telemetry) be added to time values extracted from the processing system. This correction has already been made in the particle data in this dataset.

JHUAPL is acknowledged for its role in restoring and providing AMPTE/MEPA data.

SPDF/CDAWeb. Please also acknowledge the data producer: D. McEntire at JHU/APL

SPDF/SSCWeb. Please also acknowledge the data producer: D. McEntire at JHU/APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. McEntire at JHU/APL

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_1, @2 => Epoch_2, @3 => Epoch_3, @4 => Epoch_4.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_1, @2 => Epoch_2, @3 => Epoch_3, @4 => Epoch_4.)

Active Magnetospheric Particle Tracer Explorers Charge Composition Explorer (from all.xml/observatory/description/@short)

Energetic Particles (from all.xml/instrument/description/@short)

Active Magnetospheric Particle Tracer Explorers Charge Composition Explorer (from Master/CDFglobalAttributes/Source_name)

High Resolution data (from Master/CDFglobalAttributes/Data_type)

Zero corresponds to J2000. See https://spdf.gsfc.nasa.gov/pub/software/cdf/doc/cdf390/cdf390ug.pdf

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ampte/h0/1984/amptecce_h0_mepa_19840829_v01.cdf. The most common cadence, 184857845 [ns] = PT0.184858S, occurred for 49.5044% of the 1948 timesteps. 

ION_protons: counts per sector (spectrogram) with each sector being a sum from 4 spins; ION records only; the time given is the SECTOR midpoint in spin 2 out of 0,1,2,3

---> ION_protons: differential intensity per sector (spectrogram)

Actual ION_protons channel midpoint energies at the middle of this day

Actual ION_helium channel midpoint energies at the middle of this day

Counts based on variable 'Epoch_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ampte/h0/1984/amptecce_h0_mepa_19840829_v01.cdf. The most common cadence, 184857845 [ns] = PT0.184858S, occurred for 28.8213% of the 4565 timesteps. 

Micro-channel plate 1:  count rate from counts summed over 4 spins

TOF_protons: counts per sector (spectrogram) with each sector being a sum from 4 spins; either ION or TOF records; the time given is the SECTOR_1 midpoint in spin 2 out of 0,1,2,3

---> TOF_protons: differential intensity per sector (spectrogram)

Actual TOF_protons channel midpoint energies at the middle of this day

TOF_helium: counts per sector (spectrogram) with each sector being a sum from 4 spins; either ION or TOF records; the time given is the SECTOR_1 midpoint in spin 2 out of 0,1,2,3

---> TOF_helium: differential intensity per sector (spectrogram)

Actual TOF_helium channel midpoint energies at the middle of this day

TOF_oxygen: counts per sector (spectrogram) with each sector being a sum from 4 spins; either ION or TOF records; the time given is the SECTOR_1 midpoint in spin 2 out of 0,1,2,3

---> TOF_oxygen: differential intensity per sector (spectrogram)

Actual TOF_oxygen channel midpoint energies at the middle of this day

Actual TOF_iron channel midpoint energies at the middle of this day

Counts based on variable 'Epoch_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ampte/h0/1984/amptecce_h0_mepa_19840829_v01.cdf. The most common cadence, 184859276 [ns] = PT0.184859S, occurred for 22.1541% of the 2637 timesteps. 

TOF_all_ions: counts per sector (spectrogram) with each sector being a sum from 4 spins; TOF records only; the time given is the SECTOR_2 midpoint in spin 2 out of 0,1,2,3

---> TOF_all_ions: differential intensity per sector (spectrogram)

Counts based on variable 'Epoch_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ampte/h0/1984/amptecce_h0_mepa_19840829_v01.cdf. The most common cadence, 184857845 [ns] = PT0.184858S, occurred for 51.4705% of the 8103 timesteps. 

Actual HIRES_ION_protons channel midpoint energies at the middle of this day

Spacecraft spin axis as a unit vector in GSE evaluated once per record

Counts based on variable 'Epoch_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ampte/h0/1984/amptecce_h0_mepa_19840829_v01.cdf. The most common cadence, 23580362797 [ns] = PT23.580363S, occurred for 17.0040% of the 84 timesteps. 

This is the hourly-averaged data from the Apollo 12 Solar Wind  Spectrometer instrument, reformatted by NSSDC for easier access and use.  During the lunarnight there is no solar wind signal so there are data gaps of about 15 dayseach lunation. Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at https://nssdc.gsfc.nasa.gov/nmc/publicationDisplay.do?id=B55381-000A

Please acknowledge Dr. Conway W. Snyder (JPL), and the NSSDC Lunar Data Project for providing these data.

SPDF/CDAWeb. Please also acknowledge the data producer: Conway W. Snyder at Jet Propulsion Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Conway W. Snyder at Jet Propulsion Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Conway W. Snyder at Jet Propulsion Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/apollo/apollo12_cdaweb/sws_1hr/apollo12_sws_1hr_19691119_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.5502% of the 664 timesteps. 

Apollo Lunar Surface Experiment Package (from all.xml/observatory/description/@short)

Solar Wind Spectrometer (from all.xml/instrument/description/@short)

Lunar Surface Environment (from Master/CDFglobalAttributes/Discipline)

Apollo Lunar Surface Experiment Package (from Master/CDFglobalAttributes/Source_name)

This 28-s data set is the highest resolution data set available from the Apollo 12 Solar Wind Spectrometer instrument, and was reformatted by NSSDC for easier access and use.  During the lunar night there is no solar wind signalso there are data gaps of about 15 days each lunation. Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at https://nssdc.gsfc.nasa.gov/nmc/publicationDisplay.do?id=B55381-000A

Please acknowledge Dr. Conway W. Snyder and the NSSDC Lunar Data Restoration Project

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/apollo/apollo12_cdaweb/sws_28s/1969/apollo12_sws_28s_19691119_v01.cdf. The most common cadence, 28000 [ms] = PT28S, occurred for 71.2928% of the 375 timesteps. 

FLAG Word bits not separately shown; packed in low order bits; See Var_Notes. Note: CDF_UINT4 data was converted to HAPI double.

1 means that side cup not next to cup A has more current than cups B or C

This is the hourly-averaged data from the Apollo 15 Solar Wind Spectrometer instrument, reformatted by NSSDC for easier access and use.  During the lunarnight there is no solar wind signal so there are data gaps of about 15 dayseach lunation.Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at https://nssdc.gsfc.nasa.gov/nmc/publicationDisplay.do?id=B55381-000A

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/apollo/apollo15_cdaweb/sws_1hr/apollo15_sws_1hr_19710731_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.4762% of the 2089 timesteps. 

This 28-s data set is the highest resolution data set available from the Apollo 15 Solar Wind Spectrometer instrument, and was reformatted by NSSDC for easier access and use.  During the local lunar night there is no solarwind signal so there are data gaps of about 15 days each lunation.Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at https://nssdc.gsfc.nasa.gov/nmc/publicationDisplay.do?id=B55381-000A

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/apollo/apollo15_cdaweb/sws_28s/1971/apollo15_sws_28s_19710731_v01.cdf. The most common cadence, 28000 [ms] = PT28S, occurred for 73.9910% of the 330 timesteps. 

Atmospheric Waves Experiment (AWE) on the ISS - Mesospheric Temperature Mapper - Swaths

AWE investigates the connection between tropospheric weather and space weather - Visit 'https://www.awemission.org' for more details

SPDF/CDAWeb. Please also acknowledge the data producer: Ludger Scherliess at Utah State University

SPDF/SSCWeb. Please also acknowledge the data producer: Ludger Scherliess at Utah State University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Ludger Scherliess at Utah State University

Atmosphereic Waves Experiment (from all.xml/observatory/description/@short)

Advanced Mesospheric Temperature Mapper (from all.xml/instrument/description/@short)

Atmosphereic Waves Experiment (from Master/CDFglobalAttributes/Source_name)

Machine Learning Cloud array 0=no cloud, 100=most likely cloud presence plain images

Atmospheric Waves Experiment (AWE) on the ISS - Mesospheric Temperature Mapper - Swaths - Q line Radiance

Machine Learning Cloud array - percent cloud chance - plain image

Geographic and magnetic corrdinates. Geographic coordinates are obtained from onboard GPS unit, magnegic coordinates are derived using the IRBEM FORTRAN library. Ephemeris data products (Lat, Long, Alt, and Time) are each returned from the payload once every 4s.

Access to all releases of BARREL data and links to the Science Operation Center tools.

The Balloon Array for Radiation Belt Relativistic Electron Losses, BARREL, Mission official website with embedded links to mission overview, data, news & events, and publications. Hosted by Dartmouth College

Balloon Array for Radiation Belt Relativistic Electron Losses, BARREL, Space Science Reviews overview publication: Millan, R.M., McCarthy, M.P., Sample, J.G., Smith, D.M., Thompson, L.D., McGaw, D.G., Woodger, L.A., Hewitt, J.G., Comess, M.D., Yando, K.B., Liang, A.X., Anderson, B.A., Knezek, N.R., Rexroad, W.Z., Scheiman, J.M., Bowers, G.S., Halford, A.J., Collier, A.B., Clilverd, M.A., Lin, R.P., and M.K. Hudson, The Balloon Array for RBSP Relativistic Electron Losses (BARREL). Space Sci. Rev., 179, 503-530 (2013). https://doi.org/10.1007/s11214-013-9971-z

Annotated BARREL campaign information with balloon release locations along with dates and times of balloon launch and termination of data acquisition. Text file provided by Warren Rexroad

The A.J. Halford BARREL Mission overview website covering the years from 2013 to 2016. The site hosts a list of BARREL related publications, an informative BARREL slideshow, and a youtube video that expounds on the BARREL balloon campaign strategy and goals.

The BARREL Mission status update blog entitled: BARREL - Radiation Belt Science with Balloons. This blog offers offers status reports and links to frequently asked questions, FAQ, page as well as links to two other blogs: the BARREL Dedicated Science Blog and the KeV Blog that list also balloon status reports. All of these blogs document events that occurred during BARREL balloon launch campaigns that took place from late 2012 until the summer of 2016.

The NASA Balloon Array for Radiation Belt Relativistic Electron Losses, BARREL, Mission website with links to a BARREL Mission Overview as well as mission related images, videos, and BARREL related NASA news releases amd media resources.

The International Radiation Belt Environment Modeling, IRBEM, website lists information on how to use the IRBEM fortran library, which was formerly known as the ONERA-DESP library. IRBEM software package can be used to compute magnetic coordinates for any location within the terrestrial magnetic field, to calculate the locus of points defining drift shells, to perform coordinate and time format transformations, to evaluate geophysics/space-physics models, and to propagate orbits in time. All of this functionality can be performed by using various external magnetic field models.

The COSPAR Pannel on Radiation Belt Environment Modeling, PRBEM, International Radiation Belt Environment Modeling, IRBEM, GitHub Website. The site provide access to all components of the IRBEM Library and it is freely distributed under the umbrella of the PRBEM COSPAR panel.

BARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the "BARREL Mission Data Usage Policy" which can be found in the BARREL data repository or obtained by contacting barrelballoons@gmail.com

SPDF/CDAWeb. Please also acknowledge the data producer: Robyn Millan at Dartmouth College

SPDF/SSCWeb. Please also acknowledge the data producer: Robyn Millan at Dartmouth College

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Robyn Millan at Dartmouth College

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/ephem/bar_1a_l2_ephm_20130128_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.6460% of the 3528 timesteps. 

Data Quality Flag. Note: CDF_UINT4 data was converted to HAPI double.

Fast time resolution Bremsstrahlung X-ray spectrum from NaI Scintillator, four channels at 20 MHz.

BARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the "BARREL Mission Data Usage Policy" which can be found here: http://www.dartmouth.edu/~barrel/documents/data.use.policy.pdf.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/fspc/bar_1a_l2_fspc_20130128_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3454% of the 550591 timesteps. 

Voltage, temperature, current, and payload status values returned every 40s. NOTE: The analog sensor data in these records are based on the nominal BARREL housekeeping layout. Some payloads may have small differences that are not reflected here. If there is specific sensor data that you need, but looks questionable, contact the BARREL team for clarification.

BARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the "BARREL Mission Data Usage Policy" which can be found here: http://www.dartmouth.edu/~barrel/documents/data.use.policy.pdf

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/hkpg/bar_1a_l2_hkpg_20130128_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 78.5441% of the 615 timesteps. 

Three axis magnetometer reading with nominal conversion. Data are neither gain corrected nor despun.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/magn/bar_1a_l2_magn_20130128_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7269% of the 107215 timesteps. 

Bremsstrahlung X-ray spectra made of 48 transmitted over 4 frames and accumulated for 4 seconds.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/mspc/bar_1a_l2_mspc_20130128_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.4928% of the 3484 timesteps. 

Rate counters record interrupt, low level, peak detect, and high level. Each value is a four second accumulation

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/rcnt/bar_1a_l2_rcnt_20130128_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.6460% of the 3528 timesteps. 

Bremsstrahlung X-ray spectra each made of 256 energy channels transmitted over 32 frames.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1a/sspc/bar_1a_l2_sspc_20130128_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 81.7043% of the 652 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/ephem/bar_1b_l2_ephm_20130102_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 63.3776% of the 6256 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/fspc/bar_1b_l2_fspc_20130102_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.5384% of the 783705 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/hkpg/bar_1b_l2_hkpg_20130102_v10.cdf. The most common cadence, 39996000000 [ns] = PT39.996S, occurred for 56.8885% of the 607 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/magn/bar_1b_l2_magn_20130102_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.6922% of the 153833 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/mspc/bar_1b_l2_mspc_20130102_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 63.3806% of the 6217 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/rcnt/bar_1b_l2_rcnt_20130102_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 63.3776% of the 6256 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1b/sspc/bar_1b_l2_sspc_20130102_v10.cdf. The most common cadence, 31997000000 [ns] = PT31.997S, occurred for 82.1336% of the 947 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/ephem/bar_1c_l2_ephm_20130116_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 54.0606% of the 2230 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/fspc/bar_1c_l2_fspc_20130116_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4251% of the 327910 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/hkpg/bar_1c_l2_hkpg_20130116_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 55.8962% of the 237 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/magn/bar_1c_l2_magn_20130116_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.1256% of the 64065 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/mspc/bar_1c_l2_mspc_20130116_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 54.0928% of the 2227 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/rcnt/bar_1c_l2_rcnt_20130116_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 54.0606% of the 2230 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1c/sspc/bar_1c_l2_sspc_20130116_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 65.0198% of the 329 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/ephem/bar_1d_l2_ephm_20130104_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 58.2581% of the 2582 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/fspc/bar_1d_l2_fspc_20130104_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4719% of the 350919 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/hkpg/bar_1d_l2_hkpg_20130104_v10.cdf. The most common cadence, 39996000000 [ns] = PT39.996S, occurred for 78.6139% of the 397 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/magn/bar_1d_l2_magn_20130104_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.3595% of the 68693 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/mspc/bar_1d_l2_mspc_20130104_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 58.2403% of the 2555 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/rcnt/bar_1d_l2_rcnt_20130104_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 58.2581% of the 2582 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1d/sspc/bar_1d_l2_sspc_20130104_v10.cdf. The most common cadence, 31997000000 [ns] = PT31.997S, occurred for 65.6000% of the 328 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/ephem/bar_1g_l2_ephm_20130114_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.3445% of the 4577 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/fspc/bar_1g_l2_fspc_20130114_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4033% of the 694861 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/hkpg/bar_1g_l2_hkpg_20130114_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 74.4108% of the 663 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/magn/bar_1g_l2_magn_20130114_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0166% of the 135635 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/mspc/bar_1g_l2_mspc_20130114_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.3542% of the 4570 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/rcnt/bar_1g_l2_rcnt_20130114_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.3445% of the 4577 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1g/sspc/bar_1g_l2_sspc_20130114_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 79.2015% of the 853 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/ephem/bar_1h_l2_ephm_20130119_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.8148% of the 2588 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/fspc/bar_1h_l2_fspc_20130119_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3821% of the 404202 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/hkpg/bar_1h_l2_hkpg_20130119_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 87.8327% of the 462 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/magn/bar_1h_l2_magn_20130119_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9106% of the 78830 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/mspc/bar_1h_l2_mspc_20130119_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.7783% of the 2577 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/rcnt/bar_1h_l2_rcnt_20130119_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.8148% of the 2588 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1h/sspc/bar_1h_l2_sspc_20130119_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 89.5330% of the 556 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/ephem/bar_1i_l2_ephm_20130109_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.4556% of the 1414 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/fspc/bar_1i_l2_fspc_20130109_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3363% of the 217324 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/hkpg/bar_1i_l2_hkpg_20130109_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 74.9164% of the 224 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/magn/bar_1i_l2_magn_20130109_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.6815% of the 42303 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/mspc/bar_1i_l2_mspc_20130109_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3950% of the 1400 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/rcnt/bar_1i_l2_rcnt_20130109_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.4556% of the 1414 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1i/sspc/bar_1i_l2_sspc_20130109_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 79.3750% of the 254 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/ephem/bar_1j_l2_ephm_20130101_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.0817% of the 1838 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/fspc/bar_1j_l2_fspc_20130101_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3369% of the 288831 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/hkpg/bar_1j_l2_hkpg_20130101_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 81.4118% of the 346 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/magn/bar_1j_l2_magn_20130101_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.6845% of the 56223 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/mspc/bar_1j_l2_mspc_20130101_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.0277% of the 1806 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/rcnt/bar_1j_l2_rcnt_20130101_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.0817% of the 1838 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1j/sspc/bar_1j_l2_sspc_20130101_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 82.0449% of the 329 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/ephem/bar_1k_l2_ephm_20130105_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.1882% of the 2385 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/fspc/bar_1k_l2_fspc_20130105_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3947% of the 361438 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/hkpg/bar_1k_l2_hkpg_20130105_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 72.1992% of the 348 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/magn/bar_1k_l2_magn_20130105_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9736% of the 70526 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/mspc/bar_1k_l2_mspc_20130105_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.1710% of the 2367 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/rcnt/bar_1k_l2_rcnt_20130105_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.1882% of the 2385 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1k/sspc/bar_1k_l2_sspc_20130105_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 76.8946% of the 416 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/ephem/bar_1m_l2_ephm_20130106_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.6861% of the 1773 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/fspc/bar_1m_l2_fspc_20130106_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3736% of the 275899 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/hkpg/bar_1m_l2_hkpg_20130106_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 82.9457% of the 321 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/magn/bar_1m_l2_magn_20130106_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8682% of the 53788 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/mspc/bar_1m_l2_mspc_20130106_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.6505% of the 1752 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/rcnt/bar_1m_l2_rcnt_20130106_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.6861% of the 1773 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1m/sspc/bar_1m_l2_sspc_20130106_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 82.3980% of the 323 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/ephm/bar_1n_l2_ephm_20130108_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.0059% of the 4239 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/fspc/bar_1n_l2_fspc_20130108_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3419% of the 646871 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/hkpg/bar_1n_l2_hkpg_20130108_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 75.0293% of the 640 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/magn/bar_1n_l2_magn_20130108_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7097% of the 125946 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/mspc/bar_1n_l2_mspc_20130108_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.0182% of the 4227 timesteps. 

Rate counters are diagnostic fields, have uncalibrated energy ranges, and wrap near or above 16384 counts/second. Values are stored as 4 second accumulations of counts.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/rcnt/bar_1n_l2_rcnt_20130108_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.0059% of the 4239 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1n/sspc/bar_1n_l2_sspc_20130108_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 79.8990% of the 791 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/ephem/bar_1o_l2_ephm_20130109_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 53.0645% of the 3342 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/fspc/bar_1o_l2_fspc_20130109_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4105% of the 499811 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/hkpg/bar_1o_l2_hkpg_20130109_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 64.0060% of the 425 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/magn/bar_1o_l2_magn_20130109_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0524% of the 97591 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/mspc/bar_1o_l2_mspc_20130109_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 53.0228% of the 3324 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/rcnt/bar_1o_l2_rcnt_20130109_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 53.0645% of the 3342 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1o/sspc/bar_1o_l2_sspc_20130109_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 70.5570% of the 532 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/ephem/bar_1q_l2_ephm_20130120_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.2243% of the 1046 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/fspc/bar_1q_l2_fspc_20130120_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3904% of the 162383 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/hkpg/bar_1q_l2_hkpg_20130120_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 83.8095% of the 176 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/magn/bar_1q_l2_magn_20130120_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9518% of the 31679 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/mspc/bar_1q_l2_mspc_20130120_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.2255% of the 1045 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/rcnt/bar_1q_l2_rcnt_20130120_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.2243% of the 1046 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1q/sspc/bar_1q_l2_sspc_20130120_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 88.4000% of the 221 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/ephem/bar_1r_l2_ephm_20130121_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.8176% of the 1031 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/fspc/bar_1r_l2_fspc_20130121_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4087% of the 155175 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/hkpg/bar_1r_l2_hkpg_20130121_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 68.6869% of the 136 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/magn/bar_1r_l2_magn_20130121_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0435% of the 30296 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/mspc/bar_1r_l2_mspc_20130121_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.8234% of the 1029 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/rcnt/bar_1r_l2_rcnt_20130121_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.8176% of the 1031 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1r/sspc/bar_1r_l2_sspc_20130121_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 74.7899% of the 178 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/ephem/bar_1s_l2_ephm_20130122_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3666% of the 3270 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/fspc/bar_1s_l2_fspc_20130122_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3543% of the 505769 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/hkpg/bar_1s_l2_hkpg_20130122_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 83.4365% of the 539 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/magn/bar_1s_l2_magn_20130122_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7715% of the 98524 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/mspc/bar_1s_l2_mspc_20130122_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3841% of the 3267 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/rcnt/bar_1s_l2_rcnt_20130122_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3666% of the 3270 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1s/sspc/bar_1s_l2_sspc_20130122_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 86.7853% of the 683 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/ephem/bar_1t_l2_ephm_20130124_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 49.8397% of the 1866 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/fspc/bar_1t_l2_fspc_20130124_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3638% of the 295357 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/hkpg/bar_1t_l2_hkpg_20130124_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 79.5402% of the 346 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/magn/bar_1t_l2_magn_20130124_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8191% of the 57558 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/mspc/bar_1t_l2_mspc_20130124_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 49.7293% of the 1837 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/rcnt/bar_1t_l2_rcnt_20130124_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 49.8397% of the 1866 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1t/sspc/bar_1t_l2_sspc_20130124_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 81.9071% of the 335 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/ephem/bar_1u_l2_ephm_20130126_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8592% of the 2859 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/fspc/bar_1u_l2_fspc_20130126_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3484% of the 437882 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/hkpg/bar_1u_l2_hkpg_20130126_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 79.6820% of the 451 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/magn/bar_1u_l2_magn_20130126_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7419% of the 85278 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/mspc/bar_1u_l2_mspc_20130126_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8169% of the 2852 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/rcnt/bar_1u_l2_rcnt_20130126_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8592% of the 2859 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1u/sspc/bar_1u_l2_sspc_20130126_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 83.4564% of the 565 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/ephem/bar_1v_l2_ephm_20130130_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.3970% of the 2481 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/fspc/bar_1v_l2_fspc_20130130_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3414% of the 376034 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/hkpg/bar_1v_l2_hkpg_20130130_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 74.5833% of the 358 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/magn/bar_1v_l2_magn_20130130_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7070% of the 73212 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/mspc/bar_1v_l2_mspc_20130130_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.3689% of the 2476 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/rcnt/bar_1v_l2_rcnt_20130130_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.3970% of the 2481 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/1v/sspc/bar_1v_l2_sspc_20130130_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 78.9292% of the 457 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/ephem/bar_2a_l2_ephm_20140116_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.6264% of the 4243 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/fspc/bar_2a_l2_fspc_20140116_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3814% of the 666114 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/hkpg/bar_2a_l2_hkpg_20140116_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 91.9717% of the 779 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/magn/bar_2a_l2_magn_20140116_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9072% of the 129906 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/mspc/bar_2a_l2_mspc_20140116_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.6151% of the 4238 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/rcnt/bar_2a_l2_rcnt_20140116_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.6264% of the 4243 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2a/sspc/bar_2a_l2_sspc_20140116_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 93.1533% of the 966 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/ephem/bar_2b_l2_ephm_20140117_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.6586% of the 1644 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/fspc/bar_2b_l2_fspc_20140117_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4072% of the 248366 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/hkpg/bar_2b_l2_hkpg_20140117_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 72.2930% of the 227 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/magn/bar_2b_l2_magn_20140117_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0362% of the 48488 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/mspc/bar_2b_l2_mspc_20140117_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.6603% of the 1643 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/rcnt/bar_2b_l2_rcnt_20140117_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.6586% of the 1644 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2b/sspc/bar_2b_l2_sspc_20140117_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 77.9221% of the 300 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/ephem/bar_2c_l2_ephm_20140120_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.0873% of the 1647 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/fspc/bar_2c_l2_fspc_20140120_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3947% of the 250408 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/hkpg/bar_2c_l2_hkpg_20140120_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 69.7605% of the 233 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/magn/bar_2c_l2_magn_20140120_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9734% of the 48861 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/mspc/bar_2c_l2_mspc_20140120_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.1158% of the 1638 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/rcnt/bar_2c_l2_rcnt_20140120_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.0873% of the 1647 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2c/sspc/bar_2c_l2_sspc_20140120_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 75.0678% of the 277 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/ephem/bar_2d_l2_ephm_20140127_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.3454% of the 2946 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/fspc/bar_2d_l2_fspc_20140127_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4003% of the 446505 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/hkpg/bar_2d_l2_hkpg_20140127_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 73.0104% of the 422 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/magn/bar_2d_l2_magn_20140127_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0013% of the 87145 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/mspc/bar_2d_l2_mspc_20140127_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.2816% of the 2933 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/rcnt/bar_2d_l2_rcnt_20140127_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.3454% of the 2946 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2d/sspc/bar_2d_l2_sspc_20140127_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 78.6451% of the 534 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/ephem/bar_2e_l2_ephm_20140130_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 53.7105% of the 3199 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/fspc/bar_2e_l2_fspc_20140130_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3258% of the 473048 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/hkpg/bar_2e_l2_hkpg_20140130_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 61.1296% of the 368 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/magn/bar_2e_l2_magn_20140130_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.6289% of the 92040 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/mspc/bar_2e_l2_mspc_20140130_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 53.6807% of the 3194 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/rcnt/bar_2e_l2_rcnt_20140130_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 53.7105% of the 3199 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2e/sspc/bar_2e_l2_sspc_20140130_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 68.7924% of the 507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/ephem/bar_2f_l2_ephm_20140201_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 57.1096% of the 3185 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/fspc/bar_2f_l2_fspc_20140201_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.2769% of the 441534 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/hkpg/bar_2f_l2_hkpg_20140201_v10.cdf. The most common cadence, 39994000000 [ns] = PT39.994S, occurred for 72.3592% of the 411 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/magn/bar_2f_l2_magn_20140201_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.3845% of the 85734 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/mspc/bar_2f_l2_mspc_20140201_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 57.1043% of the 3171 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/rcnt/bar_2f_l2_rcnt_20140201_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 57.1096% of the 3185 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2f/sspc/bar_2f_l2_sspc_20140201_v10.cdf. The most common cadence, 31995000000 [ns] = PT31.995S, occurred for 56.9527% of the 385 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/ephem/bar_2i_l2_ephm_20131231_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.2068% of the 5028 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/fspc/bar_2i_l2_fspc_20131231_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3896% of the 780533 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/hkpg/bar_2i_l2_hkpg_20131231_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 86.4919% of the 858 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/magn/bar_2i_l2_magn_20131231_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9478% of the 152271 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/mspc/bar_2i_l2_mspc_20131231_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.1976% of the 5023 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/rcnt/bar_2i_l2_rcnt_20131231_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.2068% of the 5028 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2i/sspc/bar_2i_l2_sspc_20131231_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 88.7057% of the 1076 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/ephem/bar_2k_l2_ephm_20140104_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.3478% of the 4724 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/fspc/bar_2k_l2_fspc_20140104_v10.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 4.3903% of the 32301 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/hkpg/bar_2k_l2_hkpg_20140104_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 84.2333% of the 780 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/magn/bar_2k_l2_magn_20140104_v10.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 21.9515% of the 32301 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/mspc/bar_2k_l2_mspc_20140104_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.3058% of the 4715 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/rcnt/bar_2k_l2_rcnt_20140104_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.3043% of the 4720 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2k/sspc/bar_2k_l2_sspc_20140104_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 86.6960% of the 984 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/ephem/bar_2l_l2_ephm_20140106_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.6816% of the 2770 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/fspc/bar_2l_l2_fspc_20140106_v10.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 4.3397% of the 18259 timesteps. 

Voltage, temperature, current, and payload status values returned every 40s.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/hkpg/bar_2l_l2_hkpg_20140106_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 71.8868% of the 381 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/magn/bar_2l_l2_magn_20140106_v10.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 21.6989% of the 18259 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/mspc/bar_2l_l2_mspc_20140106_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.6916% of the 2770 timesteps. 

Rate counters record interrupt, low level, peak detect, and high level. Each value is a 4 second accumulation.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/rcnt/bar_2l_l2_rcnt_20140106_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 52.6816% of the 2770 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2l/sspc/bar_2l_l2_sspc_20140106_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 77.7607% of the 507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/ephem/bar_2m_l2_ephm_20140111_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 53.6211% of the 5516 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/fspc/bar_2m_l2_fspc_20140111_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4191% of the 817761 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/hkpg/bar_2m_l2_hkpg_20140111_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 62.8599% of the 655 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/magn/bar_2m_l2_magn_20140111_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0956% of the 159729 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/mspc/bar_2m_l2_mspc_20140111_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 53.6006% of the 5508 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/rcnt/bar_2m_l2_rcnt_20140111_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 53.6211% of the 5516 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2m/sspc/bar_2m_l2_sspc_20140111_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 69.5515% of the 884 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/ephem/bar_2n_l2_ephm_20140118_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.5307% of the 4326 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/fspc/bar_2n_l2_fspc_20140118_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3525% of the 666889 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/hkpg/bar_2n_l2_hkpg_20140118_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 82.8839% of the 707 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/magn/bar_2n_l2_magn_20140118_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7627% of the 129901 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/mspc/bar_2n_l2_mspc_20140118_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.4906% of the 4318 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/rcnt/bar_2n_l2_rcnt_20140118_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.5307% of the 4326 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2n/sspc/bar_2n_l2_sspc_20140118_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 86.2802% of the 893 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/ephem/bar_2o_l2_ephm_20140126_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.8804% of the 2405 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/fspc/bar_2o_l2_fspc_20140126_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4102% of the 361704 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/hkpg/bar_2o_l2_hkpg_20140126_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 69.1304% of the 318 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/magn/bar_2o_l2_magn_20140126_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0510% of the 70624 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/mspc/bar_2o_l2_mspc_20140126_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.8829% of the 2403 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/rcnt/bar_2o_l2_rcnt_20140126_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.8804% of the 2405 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2o/sspc/bar_2o_l2_sspc_20140126_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 75.2228% of the 422 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/ephem/bar_2p_l2_ephm_20140130_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.7878% of the 4384 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/fspc/bar_2p_l2_fspc_20140130_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3821% of the 685953 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/hkpg/bar_2p_l2_hkpg_20140130_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 89.5216% of the 786 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/magn/bar_2p_l2_magn_20140130_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9104% of the 133778 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/mspc/bar_2p_l2_mspc_20140130_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.7830% of the 4378 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/rcnt/bar_2p_l2_rcnt_20140130_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.7878% of the 4384 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2p/sspc/bar_2p_l2_sspc_20140130_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 91.7448% of the 978 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/ephem/bar_2q_l2_ephm_20140202_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.2418% of the 3636 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/fspc/bar_2q_l2_fspc_20140202_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3770% of the 575161 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/hkpg/bar_2q_l2_hkpg_20140202_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 94.2701% of the 691 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/magn/bar_2q_l2_magn_20140202_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8847% of the 112147 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/mspc/bar_2q_l2_mspc_20140202_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.2420% of the 3633 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/rcnt/bar_2q_l2_rcnt_20140202_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.2418% of the 3636 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2q/sspc/bar_2q_l2_sspc_20140202_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 94.7309% of the 845 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/ephem/bar_2t_l2_ephm_20131227_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.6198% of the 4557 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/fspc/bar_2t_l2_fspc_20131227_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3919% of the 700087 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/hkpg/bar_2t_l2_hkpg_20131227_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 80.8250% of the 725 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/magn/bar_2t_l2_magn_20131227_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9597% of the 136591 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/mspc/bar_2t_l2_mspc_20131227_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.5455% of the 4536 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/rcnt/bar_2t_l2_rcnt_20131227_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.6198% of the 4557 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2t/sspc/bar_2t_l2_sspc_20131227_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 83.9402% of the 899 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/ephem/bar_2w_l2_ephm_20131231_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.4051% of the 2364 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/fspc/bar_2w_l2_fspc_20131231_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3666% of the 372579 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/hkpg/bar_2w_l2_hkpg_20131231_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 92.1941% of the 437 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/magn/bar_2w_l2_magn_20131231_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8329% of the 72615 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/mspc/bar_2w_l2_mspc_20131231_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3949% of the 2361 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/rcnt/bar_2w_l2_rcnt_20131231_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.4051% of the 2364 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2w/sspc/bar_2w_l2_sspc_20131231_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 93.6097% of the 542 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/ephem/bar_2x_l2_ephm_20140104_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3916% of the 1588 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/fspc/bar_2x_l2_fspc_20140104_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3531% of the 245577 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/hkpg/bar_2x_l2_hkpg_20140104_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 81.6456% of the 258 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/magn/bar_2x_l2_magn_20140104_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7654% of the 47836 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/mspc/bar_2x_l2_mspc_20140104_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.4091% of the 1587 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/rcnt/bar_2x_l2_rcnt_20140104_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3916% of the 1588 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2x/sspc/bar_2x_l2_sspc_20140104_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 85.7520% of the 325 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/ephem/bar_2y_l2_ephm_20140111_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.6890% of the 1545 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/fspc/bar_2y_l2_fspc_20140111_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3618% of the 241951 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/hkpg/bar_2y_l2_hkpg_20140111_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 90.9091% of the 280 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/magn/bar_2y_l2_magn_20140111_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8091% of the 47147 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/mspc/bar_2y_l2_mspc_20140111_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.6242% of the 1541 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/rcnt/bar_2y_l2_rcnt_20140111_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.6890% of the 1545 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/2y/sspc/bar_2y_l2_sspc_20140111_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 92.4731% of the 344 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/ephem/bar_3a_l2_ephm_20150810_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 56.2283% of the 2758 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/fspc/bar_3a_l2_fspc_20150810_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.2922% of the 389403 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/hkpg/bar_3a_l2_hkpg_20150810_v10.cdf. The most common cadence, 39994000000 [ns] = PT39.994S, occurred for 62.9482% of the 316 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/magn/bar_3a_l2_magn_20150810_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.4608% of the 75659 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/mspc/bar_3a_l2_mspc_20150810_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 56.2615% of the 2754 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/rcnt/bar_3a_l2_rcnt_20150810_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 56.2283% of the 2758 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3a/sspc/bar_3a_l2_sspc_20150810_v10.cdf. The most common cadence, 31995000000 [ns] = PT31.995S, occurred for 50.4983% of the 304 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/ephem/bar_3b_l2_ephm_20150813_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.0899% of the 5446 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/fspc/bar_3b_l2_fspc_20150813_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.4002% of the 831144 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/hkpg/bar_3b_l2_hkpg_20150813_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 77.4621% of the 818 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/magn/bar_3b_l2_magn_20150813_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 97.0012% of the 162216 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/mspc/bar_3b_l2_mspc_20150813_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.0770% of the 5441 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/rcnt/bar_3b_l2_rcnt_20150813_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.0899% of the 5446 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3b/sspc/bar_3b_l2_sspc_20150813_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 82.0849% of the 1063 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/ephem/bar_3c_l2_ephm_20150817_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3759% of the 4690 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/fspc/bar_3c_l2_fspc_20150817_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3670% of the 739716 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/hkpg/bar_3c_l2_hkpg_20150817_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 93.0453% of the 883 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/magn/bar_3c_l2_magn_20150817_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8351% of the 144173 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/mspc/bar_3c_l2_mspc_20150817_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3763% of the 4685 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/rcnt/bar_3c_l2_rcnt_20150817_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3759% of the 4690 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3c/sspc/bar_3c_l2_sspc_20150817_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 94.5217% of the 1087 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/ephem/bar_3d_l2_ephm_20150819_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.8165% of the 2614 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/fspc/bar_3d_l2_fspc_20150819_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3849% of the 408769 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/hkpg/bar_3d_l2_hkpg_20150819_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 89.9614% of the 466 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/magn/bar_3d_l2_magn_20150819_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9243% of the 79729 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/mspc/bar_3d_l2_mspc_20150819_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.7884% of the 2609 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/rcnt/bar_3d_l2_rcnt_20150819_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.8165% of the 2614 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3d/sspc/bar_3d_l2_sspc_20150819_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 91.6404% of the 581 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/ephem/bar_3e_l2_ephm_20150821_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.5298% of the 7010 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/fspc/bar_3e_l2_fspc_20150821_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3805% of the 1102144 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/hkpg/bar_3e_l2_hkpg_20150821_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 91.8977% of the 1293 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/magn/bar_3e_l2_magn_20150821_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.9026% of the 214932 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/mspc/bar_3e_l2_mspc_20150821_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.5124% of the 6999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/rcnt/bar_3e_l2_rcnt_20150821_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.5298% of the 7010 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3e/sspc/bar_3e_l2_sspc_20150821_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 92.6815% of the 1583 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/ephem/bar_3f_l2_ephm_20150825_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.1276% of the 6733 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/fspc/bar_3f_l2_fspc_20150825_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3569% of the 1046327 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/hkpg/bar_3f_l2_hkpg_20150825_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 86.0570% of the 1148 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/magn/bar_3f_l2_magn_20150825_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.7847% of the 203847 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/mspc/bar_3f_l2_mspc_20150825_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.1441% of the 6728 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/rcnt/bar_3f_l2_rcnt_20150825_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.1276% of the 6733 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3f/sspc/bar_3f_l2_sspc_20150825_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 88.6839% of the 1442 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/ephem/bar_3g_l2_ephm_20150825_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3440% of the 5562 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/fspc/bar_3g_l2_fspc_20150825_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3673% of the 877889 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/hkpg/bar_3g_l2_hkpg_20150825_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 93.9394% of the 1054 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/magn/bar_3g_l2_magn_20150825_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 96.8364% of the 171105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/mspc/bar_3g_l2_mspc_20150825_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3669% of the 5559 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/rcnt/bar_3g_l2_rcnt_20150825_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3440% of the 5562 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/3g/sspc/bar_3g_l2_sspc_20150825_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 95.0808% of the 1295 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/ephem/bar_4a_l2_ephm_20160813_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3448% of the 146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/fspc/bar_4a_l2_fspc_20160813_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3703% of the 23199 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/hkpg/bar_4a_l2_hkpg_20160813_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 92.8571% of the 26 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/mspc/bar_4a_l2_mspc_20160813_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3448% of the 146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/rcnt/bar_4a_l2_rcnt_20160813_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.3448% of the 146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/sspc/bar_4a_l2_sspc_20160813_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 97.0588% of the 33 timesteps. 

Bremsstrahlung X-ray spectra each made of 30 raw enery channels. Each record is a 10ms accumulation. The energy levels for bins in each record are tracked in the 'energy' support data variable. NOTE: Unlike other BARREL products, these data are not filtered by altitude (i.e. data below 25km are not removed). Altitude should be checked in the EPHM file for the time period you are interested in before use.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/uspc/bar_4a_l2_uspc_20160813_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9503% of the 358031 timesteps. 

Bremsstrahlung X-ray spectra made of 30 standardized bins with each sample accumulated for 50ms. The energy levels are constant and set in the 'energy' support data variable. NOTE: Unlike other BARREL products, these data are not filtered by altitude (i.e. data below 25km are not removed). Altitude should be checked in the EPHM file for the time period you are interested in before use

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4a/xspc/bar_4a_l2_xspc_20160813_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.1973% of the 68740 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/ephem/bar_4b_l2_ephm_20160816_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.7970% of the 1225 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/fspc/bar_4b_l2_fspc_20160816_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3973% of the 188182 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/hkpg/bar_4b_l2_hkpg_20160816_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 81.7021% of the 192 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/mspc/bar_4b_l2_mspc_20160816_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.7970% of the 1225 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/rcnt/bar_4b_l2_rcnt_20160816_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.7970% of the 1225 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/sspc/bar_4b_l2_sspc_20160816_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 85.7143% of the 252 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/uspc/bar_4b_l2_uspc_20160816_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9499% of the 1198722 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4b/xspc/bar_4b_l2_xspc_20160816_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.1260% of the 230075 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/ephem/bar_4c_l2_ephm_20160821_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3918% of the 5557 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/fspc/bar_4c_l2_fspc_20160821_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3568% of the 859606 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/hkpg/bar_4c_l2_hkpg_20160821_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 85.5556% of the 924 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/mspc/bar_4c_l2_mspc_20160821_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3918% of the 5557 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/rcnt/bar_4c_l2_rcnt_20160821_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.3918% of the 5557 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/sspc/bar_4c_l2_sspc_20160821_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 88.4359% of the 1193 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/uspc/bar_4c_l2_uspc_20160821_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9484% of the 3850832 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4c/xspc/bar_4c_l2_xspc_20160821_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.0065% of the 738104 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/ephem/bar_4d_l2_ephm_20160821_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.8197% of the 2170 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/fspc/bar_4d_l2_fspc_20160821_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3649% of the 339512 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/hkpg/bar_4d_l2_hkpg_20160821_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 91.2941% of the 388 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/mspc/bar_4d_l2_mspc_20160821_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.8197% of the 2170 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/rcnt/bar_4d_l2_rcnt_20160821_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 50.8197% of the 2170 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/sspc/bar_4d_l2_sspc_20160821_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 93.0451% of the 495 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/uspc/bar_4d_l2_uspc_20160821_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9497% of the 1899929 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4d/xspc/bar_4d_l2_xspc_20160821_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.1114% of the 364554 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/ephem/bar_4e_l2_ephm_20160824_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8102% of the 2533 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/fspc/bar_4e_l2_fspc_20160824_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3523% of the 388711 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/hkpg/bar_4e_l2_hkpg_20160824_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 81.9302% of the 399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/mspc/bar_4e_l2_mspc_20160824_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8102% of the 2533 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/rcnt/bar_4e_l2_rcnt_20160824_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8102% of the 2533 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/sspc/bar_4e_l2_sspc_20160824_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 85.5501% of the 521 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/uspc/bar_4e_l2_uspc_20160824_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9499% of the 2123998 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4e/xspc/bar_4e_l2_xspc_20160824_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.1427% of the 407704 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/ephem/bar_4f_l2_ephm_20160828_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.1454% of the 1987 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/fspc/bar_4f_l2_fspc_20160828_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3892% of the 309027 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/hkpg/bar_4f_l2_hkpg_20160828_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 87.8866% of the 341 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/mspc/bar_4f_l2_mspc_20160828_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.1454% of the 1987 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/rcnt/bar_4f_l2_rcnt_20160828_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.1454% of the 1987 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/sspc/bar_4f_l2_sspc_20160828_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 90.4959% of the 438 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/uspc/bar_4f_l2_uspc_20160828_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9485% of the 1732755 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4f/xspc/bar_4f_l2_xspc_20160828_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 90.9978% of the 332140 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/ephem/bar_4g_l2_ephm_20160829_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.9357% of the 1905 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/fspc/bar_4g_l2_fspc_20160829_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3984% of the 291782 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/hkpg/bar_4g_l2_hkpg_20160829_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 80.3279% of the 294 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/mspc/bar_4g_l2_mspc_20160829_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.9357% of the 1905 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/rcnt/bar_4g_l2_rcnt_20160829_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 51.9357% of the 1905 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/sspc/bar_4g_l2_sspc_20160829_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 84.4639% of the 386 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/uspc/bar_4g_l2_uspc_20160829_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9493% of the 1639459 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4g/xspc/bar_4g_l2_xspc_20160829_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.0608% of the 314431 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/ephem/bar_4h_l2_ephm_20160830_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8326% of the 2192 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/fspc/bar_4h_l2_fspc_20160830_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 99.3518% of the 336273 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/hkpg/bar_4h_l2_hkpg_20160830_v10.cdf. The most common cadence, 39995000000 [ns] = PT39.995S, occurred for 81.0427% of the 342 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/mspc/bar_4h_l2_mspc_20160830_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8326% of the 2192 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/rcnt/bar_4h_l2_rcnt_20160830_v10.cdf. The most common cadence, 3999000000 [ns] = PT3.999S, occurred for 51.8326% of the 2192 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/sspc/bar_4h_l2_sspc_20160830_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 85.0095% of the 448 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/uspc/bar_4h_l2_uspc_20160830_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 98.9510% of the 1852018 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/4h/xspc/bar_4h_l2_xspc_20160830_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 91.2140% of the 355743 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/ephem/bar_5a_l2_ephm_20180625_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.5579% of the 11106 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/fspc/bar_5a_l2_fspc_20180625_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 49.7394% of the 840886 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/hkpg/bar_5a_l2_hkpg_20180625_v10.cdf. The most common cadence, 39994999936 [ns] = PT39.995S, occurred for 36.8197% of the 778 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/mspc/bar_5a_l2_mspc_20180625_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.5603% of the 11106 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/rcnt/bar_5a_l2_rcnt_20180625_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 52.5579% of the 11106 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/sspc/bar_5a_l2_sspc_20180625_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 78.9015% of the 2083 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/uspc/bar_5a_l2_uspc_20180625_v10.cdf. The most common cadence, 10000000 [ns] = PT0.01S, occurred for 49.4256% of the 3973603 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/5a/xspc/bar_5a_l2_xspc_20180625_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 45.4533% of the 761592 timesteps. 

Geographic and magnetic coordinates. Geographic coordinates are obtained from an onboard GPS unit, magnetic coordinates are derived using the IRBEM FORTRAN library. Ephemeris data products (Lat, Long, Alt, and Time) are each returned from the payload once every 4s.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/ephem/bar_6a_l2_ephm_20181209_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 48.4951% of the 1144 timesteps. 

Six channels of fast time resolution (50ms) Bremsstrahlung X-rays detected with a NaI Scintillator. Each channel is separated in its own variable (e.g. FSPC1, FSPC2, etc). Nominal energy range covered by the 6 channels is 0 - 1.5MeV.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/fspc/bar_6a_l2_fspc_20181209_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 49.7952% of the 93971 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/hkpg/bar_6a_l2_hkpg_20181209_v10.cdf. The most common cadence, 39994999936 [ns] = PT39.995S, occurred for 43.5146% of the 104 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/magn/bar_6a_l2_magn_20181209_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 48.5044% of the 18307 timesteps. 

48 channels (0 - 4MeV) of medium time resolution (4s) Bremsstrahlung X-rays detected with a NaI Scintillator. All channels are combined to a single variable (MSPC). 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/mspc/bar_6a_l2_mspc_20181209_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 48.4938% of the 1143 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/rcnt/bar_6a_l2_rcnt_20181209_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 48.4951% of the 1144 timesteps. 

256 channels (0-10Mev) of slow time resolution (32s) Bremsstrahlung X-rays detected with a NaI Scintillator. All channels are combined to a single variable (SSPC).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/6a/sspc/bar_6a_l2_sspc_20181209_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 86.5979% of the 252 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/ephem/bar_7a_l2_ephm_20191229_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.3433% of the 3886 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/fspc/bar_7a_l2_fspc_20191229_v10.cdf. The most common cadence, 50000000 [ns] = PT0.05S, occurred for 49.7226% of the 307072 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/hkpg/bar_7a_l2_hkpg_20191229_v10.cdf. The most common cadence, 39995000064 [ns] = PT39.995S, occurred for 48.1865% of the 372 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/magn/bar_7a_l2_magn_20191229_v10.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 48.4803% of the 59880 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/mspc/bar_7a_l2_mspc_20191229_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.3369% of the 3885 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/rcnt/bar_7a_l2_rcnt_20191229_v10.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 50.3433% of the 3886 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/barrel/l2/7a/sspc/bar_7a_l2_sspc_20191229_v10.cdf. The most common cadence, 31996000000 [ns] = PT31.996S, occurred for 96.5661% of the 928 timesteps. 

Heliocentric trajectories for selected spacecraft, planets, and comets, HelioWeb data service, hosted by NASA GSFC

Heliocentric Trajectories HelioWeb Data Service Usage Instructions, NASA GSFC

Instructions for using the Heliocentric Trajectories HelioWeb data service, hosted by NASA GSFC

Heliocentric Trajectories HelioWeb Data Service Usage via CURL or WGET Commands, NASA GSFC

Instructions for using the Heliocentric Trajectories HelioWeb data service via CURL or WGET commands, hosted by NASA GSFC

Definitions for the Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinate Systems, hosted by NASA GSFC

HORIZONS Web Interface, a web page that provides limited access to the JPL HORIZONS system which can be used to generate ephemerides for solar system bodies

SPDF/CDAWeb. Please also acknowledge the data producer: Natalia Papitashvili at NASA/GSFC/SPDF

SPDF/SSCWeb. Please also acknowledge the data producer: Natalia Papitashvili at NASA/GSFC/SPDF

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Natalia Papitashvili at NASA/GSFC/SPDF

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/bepicolombo/helio1day/bepicolombo_helio1day_position_20181021_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 3065 timesteps. 

Heliospheric Physics (from Master/CDFglobalAttributes/Discipline)

1 Day Time Resolution from heliowebweb (from Master/CDFglobalAttributes/Data_type)

Deprecated version of this SPASE record which has a daily cadence.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/bepicolombo/helio1hr/bepicolombo_helio1hr_position_20181021_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 73583 timesteps. 

1 Hour Time Resolution from helioweb (from Master/CDFglobalAttributes/Data_type)

The spacecraft is in earth-trailing heliocentric orbit and carries a Linear Energy Transfer Spectrometer LETS to capture energetic particle dose rates.

NASA's BioSentinel is a 6U CubeSat launched on Artemis I that is studying the biological effects of the deep space radiation environment. The spacecraft is in earth-trailing heliocentric orbit and carries a Linear Energy Transfer Spectrometer LETS to capture energetic particle dose rates.NASA's first biological study in interplanetary deep space: (a) Combines bio studies with autonomous capability & dosimetry beyond Low Earth Orbit (LEO); (b) Beyond the protection of Earth's magnetosphere; (c) Compare radiation environments (deep space, LEO, Earth)

Please acknowledge the BioSentinel Mission Principal Investigators, Dr. Sergio Santa Maria and Dr. Stuart George

The BioSentinel Release 1 data are archived as fully citable. Please consult BioSentinel team publications and personnel for further details on production, processing and usage of these data 

SPDF/CDAWeb. Please also acknowledge the data producer: Sergio Santa Maria, Stuart George at NASA

SPDF/SSCWeb. Please also acknowledge the data producer: Sergio Santa Maria, Stuart George at NASA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Sergio Santa Maria, Stuart George at NASA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/biosentinel/let_lets/2022/biosentinel_let_lets_20221117_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Linear Energy Transfer Spectrometer (from all.xml/instrument/description/@short)

Linear Energy Transfer Spectrum (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/borrelly_helio1day_position_19960101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 8400 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/borrelly_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

Cluster Ion Spectrometry.The CIS (Cluster Ion Spectrometry) experiment is a comprehensiveionic plasma spectrometry package onboard the Cluster spacecraft,capable of obtaining full three-dimentional ion distributions(about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec)and with mass-per-charge composition determination.The CIS package consists of two different instruments,a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1)and a Hot Ion Analyser (HIA, or CIS-2).

Please acknowledge the CIS team and ESA Cluster Science Archive when using this data.

SPDF/CDAWeb. Please also acknowledge the data producer: Iannis Dandouras at IRAP

SPDF/SSCWeb. Please also acknowledge the data producer: Iannis Dandouras at IRAP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Iannis Dandouras at IRAP

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_H1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/proton_omni/2001/c1_cp_cis-codif_h1_1d_pef_20010111_v20151107.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 28.1853% of the 146 timesteps. 

Cluster Satellite No 1 (from all.xml/observatory/description/@short)

Cluster Satellite No 1 (from Master/CDFglobalAttributes/Source_name)

CIS-CODIF 1D Helium+ distributions on C1 in Particle_Energy_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_He1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/heplus_omni/2001/c1_cp_cis-codif_he1_1d_pef_20010111_v20151107.cdf. The most common cadence, 32007 [ms] = PT32.007S, occurred for 17.7326% of the 61 timesteps. 

CIS-CODIF 3D Proton distributions on C1, High-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_H1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/proton_3ddist_highsens_diffenergyflux/2001/c1_cp_cis-codif_hs_h1_pef_20010111_v20151020.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 28.1853% of the 146 timesteps. 

CIS-CODIF 3D Proton distributions on C1, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/proton_3ddist_highsens_diffparticleflux/2001/c1_cp_cis-codif_hs_h1_pf_20010111_v20151020.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 28.1853% of the 146 timesteps. 

CIS-CODIF 3D Proton distributions on C1, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_H1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/proton_3ddist_highsens_phasespacedens/2001/c1_cp_cis-codif_hs_h1_psd_20010111_v20151020.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 28.1853% of the 146 timesteps. 

CIS-CODIF 3D Helium+ distributions on C1, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/heplus_3ddist_highsens_diffparticleflux/2001/c1_cp_cis-codif_hs_he1_pf_20010111_v20151020.cdf. The most common cadence, 32007 [ms] = PT32.007S, occurred for 17.7326% of the 61 timesteps. 

CIS-CODIF 3D Helium+ distributions on C1, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_He1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/heplus_3ddist_highsens_phasespacedens/2001/c1_cp_cis-codif_hs_he1_psd_20010111_v20151020.cdf. The most common cadence, 32007 [ms] = PT32.007S, occurred for 17.7326% of the 61 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C1, High-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_O1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/oplus_3ddist_highsens_diffenergyflux/2001/c1_cp_cis-codif_hs_o1_pef_20010111_v20151022.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 14.7971% of the 62 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C1, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/oplus_3ddist_highsens_diffparticleflux/2001/c1_cp_cis-codif_hs_o1_pf_20010111_v20151022.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 14.7971% of the 62 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C1, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_HS_O1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/oplus_3ddist_highsens_phasespacedens/2001/c1_cp_cis-codif_hs_o1_psd_20010111_v20151022.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 14.7971% of the 62 timesteps. 

CIS-CODIF 1D Oxygen+ distributions on C1 in Particle_Energy_Flux

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_O1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/oplus_omni/2001/c1_cp_cis-codif_o1_1d_pef_20010111_v20151107.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 14.7971% of the 62 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_PAD_HS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/proton_pitchangle_highsens_diffparticleflux/2001/c1_cp_cis-codif_pad_hs_h1_pf_20010131_v20220812.cdf. The most common cadence, 3995 [ms] = PT3.995S, occurred for 14.7021% of the 1145 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_PAD_HS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/heplus_pitchangle_highsens_diffparticleflux/2001/c1_cp_cis-codif_pad_hs_he1_pf_20010131_v20220812.cdf. The most common cadence, 3995 [ms] = PT3.995S, occurred for 22.1705% of the 1142 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_CODIF_PAD_HS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-codif/oplus_pitchangle_highsens_diffparticleflux/2001/c1_cp_cis-codif_pad_hs_o1_pf_20010131_v20220812.cdf. The most common cadence, 3995 [ms] = PT3.995S, occurred for 21.4729% of the 1143 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_omni_highsens/2001/c1_cp_cis-hia_hs_1d_pef_20010110_v20090718.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 10.4287% of the 90 timesteps. 

3D Ion distributions for CIS-HIA, High-Sensitivity, Magnetospheric Mode

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_MAG_IONS_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_magmode_highsens_diffenergyflux/2001/c1_cp_cis-hia_hs_mag_ions_pef_20010111_v20220803.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 12.4902% of the 159 timesteps. 

CIS-HIA 3D Ion distributions on C1, High-Sensitivity, Magnetospheric Mode, in Differential_Particle_Flux

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_MAG_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_magmode_highsens_diffparticleflux/2001/c1_cp_cis-hia_hs_mag_ions_pf_20010111_v20220803.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 12.4902% of the 159 timesteps. 

CIS-HIA 3D Ion distributions on C1, High-Sensitivity, Magnetospheric Mode, in Phase_Space_Density

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_MAG_IONS_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_magmode_highsens_phasespacedens/2001/c1_cp_cis-hia_hs_mag_ions_psd_20010111_v20220803.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 12.4902% of the 159 timesteps. 

3D Ion distributions for CIS-HIA, High-Sensitivity, Solar-Wind Mode

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_SW_IONS_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_swmode_highsens_diffenergyflux/2001/c1_cp_cis-hia_hs_sw_ions_pef_20010110_v20220805.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 10.4287% of the 90 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_SW_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_swmode_highsens_diffparticleflux/2001/c1_cp_cis-hia_hs_sw_ions_pf_20010110_v20220805.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 10.4287% of the 90 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_HS_SW_IONS_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_swmode_highsens_phasespacedens/2001/c1_cp_cis-hia_hs_sw_ions_psd_20010110_v20220805.cdf. The most common cadence, 12002 [ms] = PT12.002S, occurred for 10.4287% of the 90 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_LS_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_omni_lowsens/2001/c1_cp_cis-hia_ls_1d_pef_20010110_v20090718.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 13.9241% of the 55 timesteps. 

3D Ion distributions for CIS-HIA, Low-Sensitivity, Solar Wind mode

Counts based on variable 'time_tags__C1_CP_CIS_HIA_LS_SW_IONS_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_swmode_lowsens_diffenergyflux/2001/c1_cp_cis-hia_ls_sw_ions_pef_20010110_v20220803.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 13.9241% of the 55 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_LS_SW_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_swmode_lowsens_diffparticleflux/2001/c1_cp_cis-hia_ls_sw_ions_pf_20010110_v20220803.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 13.9241% of the 55 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_LS_SW_IONS_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_3ddist_swmode_lowsens_phasespacedens/2001/c1_cp_cis-hia_ls_sw_ions_psd_20010110_v20220803.cdf. The most common cadence, 16004 [ms] = PT16.004S, occurred for 13.9241% of the 55 timesteps. 

Counts based on variable 'time_tags__C1_CP_CIS_HIA_PAD_HS_MAG_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cis-hia/ions_pitchangle_magmode_highsens_diffparticleflux/2001/c1_cp_cis-hia_pad_hs_mag_ions_pf_20010131_v20220812.cdf. The most common cadence, 3995 [ms] = PT3.995S, occurred for 22.1235% of the 1419 timesteps. 

Electron Drift InstrumentElectric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field

Please acknowledge the EDI team and ESA Cluster Active Archive in any publication based upon use of this data

SPDF/CDAWeb. Please also acknowledge the data producer: Goetz Paschmann at University of New Hampshire

SPDF/SSCWeb. Please also acknowledge the data producer: Goetz Paschmann at University of New Hampshire

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Goetz Paschmann at University of New Hampshire

Counts based on variable 'time_tags__C1_CP_EDI_AEDC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/edi/ambientelectron_counts_passivemode_mixedreso/2004/c1_cp_edi_aedc_20041014_v20191220.cdf. The most common cadence, 62 [ms] = PT0.062S, occurred for 50.0357% of the 558972 timesteps. 

Electron Drift Instrument (from all.xml/instrument/description/@short)

Cluster C1, corrected ambient electron counts GDU1 PA=180 degree

Cluster C1, corrected ambient electron counts GDU2 PA=180 degree

Counts based on variable 'time_tags__C1_CP_EDI_MP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/edi/electron_driftvelo_efield_3dvect_bestreso/2001/c1_cp_edi_mp_20010202_v20180807.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 40.2196% of the 1172 timesteps. 

Counts based on variable 'time_tags__C1_CP_EDI_QZC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/edi/backgroundelectron_counts_activemode_mixedreso/2001/c1_cp_edi_qzc_20010202_v20220630.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 99.5930% of the 462220 timesteps. 

Counts based on variable 'time_tags__C1_CP_EDI_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/edi/electron_driftvelo_efield_3dvect_spinreso/2001/c1_cp_edi_spin_20010202_v20220322.cdf. The most common cadence, 4002 [ms] = PT4.002S, occurred for 29.9894% of the 568 timesteps. 

The EFW (Electric Field and Wave) instrument consists of four sphericalprobes deployed orthogonally on 44-meter-long wire booms in the spinplane of the spacecraft. The potential differences between opposingprobes, separated by 88 m tip-to-tip, are measured to provide electricfield measurements in two directions, thus providing the full electricfield vector in the spin plane of the spacecraft. Additionally, thepotential differences between each of the probes and the spacecraft aremeasured, providing an estimate of the spacecraft potential relativeto the plasma, which can be used as a proxy for the ambient electrondensity. The output analogue signals from the preamplifiers connectedto the spherical probes are also provided to the wave instruments(STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.

Please acknowledge the EFW team and the ESA Cluster Active Archive in any

SPDF/CDAWeb. Please also acknowledge the data producer: Mats Andre at IRFU

SPDF/SSCWeb. Please also acknowledge the data producer: Mats Andre at IRFU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Mats Andre at IRFU

Counts based on variable 'time_tags__C1_CP_EFW_L3_E3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/efw/efield_3dvect_spinreso_l3_inertialframe/2000/c1_cp_efw_l3_e3d_inert_20001205_v20221114.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 1264 timesteps. 

Electric field double probe antenna (from all.xml/instrument/description/@short)

Zero corresponds to 0000-01-01T00.00.000.000.000.000. See https://spdf.gsfc.nasa.gov/pub/software/cdf/doc/cdf390/cdf390ug.pdf

Counts based on variable 'time_tags__C1_CP_EFW_L3_P' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/efw/scpotential_spinreso_l3/2000/c1_cp_efw_l3_p_20001205_v20221111.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 1263 timesteps. 

Please acknowledge the ESA Cluster Active Archive in any publication based upon this data

Counts based on variable 'time_tags__C1_CP_EFW_L3_V3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/efw/driftvelo_3dvect_spinreso_l3_inertialframe/2000/c1_cp_efw_l3_v3d_inert_20001205_v20221114.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 1264 timesteps. 

Each Cluster spacecraft carries an identical FGM instrument(Fluxgate Magnetometer) to measure the DC magnetic fieldvector. Each instrument, in turn, consists of two triaxialfluxgate magnetometers and an onboard data processing unit.The instrument samples the magnetic field at a cadence of 22 Hz(67 Hz in Burst mode). In order to minimise the magnetic background of the spacecraft, one of the magnetometer sensors (the outboard, or OB sensor) is located at the end of one of the two 5 m radial booms of the spacecraft, the other (the inboard, or IB sensor) at 1.5 m inboard from the end of the boom. Since the start of the scientific operations on February 1, 2001, only the outboard sensor on each satellite has been used.

Please acknowledge the FGM team and ESA Cluster Active Archive in any publication based upon use of this data

SPDF/CDAWeb. Please also acknowledge the data producer: Chris Carr at Imperial College

SPDF/SSCWeb. Please also acknowledge the data producer: Chris Carr at Imperial College

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Chris Carr at Imperial College

Counts based on variable 'time_tags__C1_CP_FGM_5VPS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/fgm/mfield_3dvect_5vectpersec/2000/c1_cp_fgm_5vps_20001202_v20150131.cdf. The most common cadence, 200 [ms] = PT0.2S, occurred for 99.9963% of the 80759 timesteps. 

FluxGate Magnetometer (from all.xml/instrument/description/@short)

Cluster Spacecraft 1 FluxGate Magnetometer (FGM) Spin-Resolution Parameters

NSSDC Master Catalog listing for Cluster Rumba Fluxgate Magnetometer (FGM)

This site provides information concerning the Cluster Rumba Fluxgate Magnetometer Instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: Andre Balogh>a.balogh@imperial.ac.uk & Elizabeth Lucek>e.lucek@imperial.ac.uk & ESA CAA at Imperial College

SPDF/SSCWeb. Please also acknowledge the data producer: Andre Balogh>a.balogh@imperial.ac.uk & Elizabeth Lucek>e.lucek@imperial.ac.uk & ESA CAA at Imperial College

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Andre Balogh>a.balogh@imperial.ac.uk & Elizabeth Lucek>e.lucek@imperial.ac.uk & ESA CAA at Imperial College

Counts based on variable 'time_tags__C1_CP_FGM_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/cp/2001/c1_cp_fgm_spin_20010130_v01.cdf. The most common cadence, 4003 [ms] = PT4.003S, occurred for 51.5385% of the 536 timesteps. 

Cluster spacecraft 1 (from all.xml/observatory/description/@short)

Fluxgate Magnetometer Spin Resolution (from all.xml/instrument/description/@short)

Cluster spacecraft 1 (from Master/CDFglobalAttributes/Source_name)

Research with Adaptive Particle Imaging Detectors (RAPID)The RAPID spectrometer for the Cluster mission is anadvanced particle detector for the analysis of suprathermalplasma distributions in the energy range from 39-400 keVfor electrons, 28-1500 keV (4000 keV) for hydrogen,and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.

SPDF/CDAWeb. Please also acknowledge the data producer: Berend Wilken at MPS

SPDF/SSCWeb. Please also acknowledge the data producer: Berend Wilken at MPS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Berend Wilken at MPS

Counts based on variable 'Time_tags__C1_CP_RAP_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-ies/electron_3ddist_bestreso/2000/c1_cp_rap_e3dd_20001201_v20230309.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 46.6899% of the 402 timesteps. 

Energetic electron and ion spectrometer (from all.xml/instrument/description/@short)

Counts based on variable 'Time_tags__C1_CP_RAP_ESPCT6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-ies/electron_omni_spinreso/2000/c1_cp_rap_espct6_20001201_v20230309.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 47.1822% of the 3801 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_HSPCT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/proton_omni_spinreso/2000/c1_cp_rap_hspct_20001203_v20230309.cdf. The most common cadence, 4001 [ms] = PT4.001S, occurred for 51.3411% of the 2699 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_I3DM_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/cno_3ddist_stdreso/2000/c1_cp_rap_i3dm_cno_20001203_v20230309.cdf. The most common cadence, 128018 [ms] = PT2M8.018S, occurred for 26.8908% of the 64 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_I3DM_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/proton_3ddist_stdreso/2000/c1_cp_rap_i3dm_h_20001203_v20230309.cdf. The most common cadence, 128018 [ms] = PT2M8.018S, occurred for 26.8908% of the 64 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_I3DM_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/he_3ddist_stdreso/2000/c1_cp_rap_i3dm_he_20001203_v20230309.cdf. The most common cadence, 128018 [ms] = PT2M8.018S, occurred for 26.8908% of the 64 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_ISPCT_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/cno_omni_spinreso/2000/c1_cp_rap_ispct_cno_20001203_v20230309.cdf. The most common cadence, 32005 [ms] = PT32.005S, occurred for 46.6361% of the 305 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_ISPCT_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/he_omni_spinreso/2000/c1_cp_rap_ispct_he_20001203_v20230309.cdf. The most common cadence, 32005 [ms] = PT32.005S, occurred for 46.6361% of the 305 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-ies/electron_3ddist_2echannels_stdreso/2004/c1_cp_rap_l3dd_20040420_v20210208.cdf. The most common cadence, 4040 [ms] = PT4.04S, occurred for 68.9922% of the 89 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_PAD_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/cno_pitchangle_stdreso/2000/c1_cp_rap_pad_cno_20001203_v20230309.cdf. The most common cadence, 128018 [ms] = PT2M8.018S, occurred for 26.8908% of the 64 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_PAD_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-ies/electron_pitchangle_bestreso/2000/c1_cp_rap_pad_e3dd_20001203_v20230309.cdf. The most common cadence, 4001 [ms] = PT4.001S, occurred for 51.4029% of the 458 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_PAD_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/proton_pitchangle_stdreso/2000/c1_cp_rap_pad_h_20001203_v20230309.cdf. The most common cadence, 128018 [ms] = PT2M8.018S, occurred for 26.8908% of the 64 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_PAD_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-iims/he_pitchangle_stdreso/2000/c1_cp_rap_pad_he_20001203_v20230309.cdf. The most common cadence, 128018 [ms] = PT2M8.018S, occurred for 26.8908% of the 64 timesteps. 

Counts based on variable 'Time_tags__C1_CP_RAP_PAD_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/rap-ies/electron_pitchangle_2echannels_stdreso/2004/c1_cp_rap_pad_l3dd_20040420_v20210208.cdf. The most common cadence, 4040 [ms] = PT4.04S, occurred for 68.9922% of the 89 timesteps. 

STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC).The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz  - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).

Please acknowledge the STAFF team and the ESA Cluster Archive in any publication based upon use of this data.

Digital Object Identifier for the STAFF archive: doi.org/10.5270/esa-yrzyijm

SPDF/CDAWeb. Please also acknowledge the data producer: Patrick Canu at LPP

SPDF/SSCWeb. Please also acknowledge the data producer: Patrick Canu at LPP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Patrick Canu at LPP

Counts based on variable 'Time__C1_CP_STA_CWF_GSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/sta/mfield_calibwaveform_gse/2000/c1_cp_sta_cwf_gse_20000908_v20220603.cdf. The most common cadence, 39999000000 [ps] = PT0.039999S, occurred for 94.7568% of the 408020 timesteps. 

Search coil magnetometer and spectrum analyzer (from all.xml/instrument/description/@short)

Counts based on variable 'Time__C1_CP_STA_PPP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/sta/polarization_propagation/2000/c1_cp_sta_ppp_20001203_v20160526.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 87.3915% of the 4831 timesteps. 

Polar Angle of the direction of propagation in MFA coordinate system (SVD).

Azimuthal Angle of the direction of propagation in MFA coordinate system (SVD).

Parallel component of the Poynting vector normalized by its standard deviation.

Counts based on variable 'Time__C1_CP_STA_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/sta/powerspectraldensity/2000/c1_cp_sta_psd_20000908_v20220608.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for 97.2873% of the 789 timesteps. 

Power spectrum 8-4000 Hz of the B-field components along the SR2 coordinate axes

Power spectrum 8-4000 Hz of the E-field components along the SR2 coordinate axes

Counts based on variable 'Time__C1_CP_STA_SM' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/sta/crossspectralmatrice/2000/c1_cp_sta_sm_20000908_v20220608.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 89.1089% of the 180 timesteps. 

Cross-spectral matrix of the magnetic field at 27 frequencies from 8 Hz to 4 kHz

Cross-spectral matrix of the electric field at 27 frequencies from 8 Hz to 4 kHz

Electromagnetic cross-spectral ExB products at 27 frequencies from 8 Hz to 4 kHz

The Wave of HIgh frequency and Sounder for Probing of Electron densityby Relaxation (WHISPER) performs the measurement of the electron densityon the four satellites of the CLUSTER project. The two main purposes ofthe WHISPER experiment are to record the natural waves and to make adiagnostic of the electron density using the sounding technique.The various working modes and the fourier transforms calculated on boardprovide a good frequency resolution obtained in the bandwidth 2-83 kHz.Onboard data compression by the Digital Wave Processing (DWP) intrumentallows a good dynamic and level resolution of the electric signal amplitude.

Please acknowledge the WHISPER team and the ESA Cluster Archive in any publication based upon use of this data.

Digital Object Identifier for the WHISPER archive: https://doi.org/10.5270/esa-6stdo07

SPDF/CDAWeb. Please also acknowledge the data producer: Pierre Henri at LPC2E

SPDF/SSCWeb. Please also acknowledge the data producer: Pierre Henri at LPC2E

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Pierre Henri at LPC2E

Counts based on variable 'time_tags__C1_CP_WHI_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/whi/efield_spectralpowerdensity_soundingmode/2000/c1_cp_whi_active_20000908_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 39.4737% of the 120 timesteps. 

Counts based on variable 'time_tags__C1_CP_WHI_ELECTRON_DENSITY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/whi/electron_density/2001/c1_cp_whi_electron_density_20010204_v20160311.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 37.9404% of the 140 timesteps. 

Counts based on variable 'time_tags__C1_CP_WHI_NATURAL' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/whi/efield_spectralpowerdensity_naturalmode/2000/c1_cp_whi_natural_20000908_v20150715.cdf. The most common cadence, 853 [ms] = PT0.853S, occurred for 54.0541% of the 60 timesteps. 

Counts based on variable 'time_tags__C1_CP_WHI_PASSIVE_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/whi/efield_passivespectralpowerdensity_soundingmode/2000/c1_cp_whi_passive_active_20000908_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 47.2441% of the 120 timesteps. 

Counts based on variable 'time_tags__C1_CP_WHI_WAVE_FORM_ENERGY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/whi/efield_integratedpowerdensity_naturalmode/2000/c1_cp_whi_wave_form_energy_20000908_v20150715.cdf. The most common cadence, 853 [ms] = PT0.853S, occurred for 63.1579% of the 60 timesteps. 

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)

Web Page for access to High-Time Resolution Data from the Cluster and Double Star Missions

The Cluster Science Working Team along with the ESA Cluster Project Team have established the Cluster Science Data System, CSDS, a distributed Set of Data Centres, most of which are associated with one or more of the Cluster Experiments. With Software provided by the Experiment Team, each Data Centre processes the Data and then exchanges them with all the other Centres to obtain a full Data Set in a standard Format.

SPDF/CDAWeb. Please also acknowledge the data producer: M. Hapgood at RAL

SPDF/SSCWeb. Please also acknowledge the data producer: M. Hapgood at RAL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M. Hapgood at RAL

Counts based on variable 'Epoch__C1_JP_PMP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/jp/pmp/2000/c1_jp_pmp_20000814_v04.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 4936 timesteps. 

Predicted Magnetic Position (from all.xml/instrument/description/@short)

JSOC catalogue Parameter (from Master/CDFglobalAttributes/Data_type)

Spacecraft invariant Latitude (Null/will not plot outside magnetosphere)

Predicted magnetic field magnitude (Null/will not plot outside magnetosphere)

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)AP _ ApogeeCY 1 Start of visibility window at Canberra (5 deg elevation)CY 2 Start of visibility window at Canberra (5 deg elevation)CY 3 Start of visibility window at Canberra (5 deg elevation)CZ 1 End of visibility window at Canberra (5 deg elevation)CZ 2 End of visibility window at Canberra (5 deg elevation)CZ 3 End of visibility window at Canberra (5 deg elevation)CZ 4 End of visibility window at Canberra (5 deg elevation)DY 1 Start of visibility window at Vilspa (5 deg elevation)DY 2 Start of visibility window at Vilspa (5 deg elevation)DY 3 Start of visibility window at Vilspa (5 deg elevation)DY 4 Start of visibility window at Vilspa (5 deg elevation)DY 5 Start of visibility window at Vilspa (5 deg elevation)DZ 1 End of visibility window at Vilspa (5 deg elevation)DZ 2 End of visibility window at Vilspa (5 deg elevation)DZ 3 End of visibility window at Vilspa (5 deg elevation)DZ 4 End of visibility window at Vilspa (5 deg elevation)GY 1 Start of visibility window at Goldstone (5 deg elevation)GY 2 Start of visibility window at Goldstone (5 deg elevation)GY 3 Start of visibility window at Goldstone (5 deg elevation)GY 4 Start of visibility window at Goldstone (5 deg elevation)GZ 1 End of visibility window at Goldstone (5 deg elevation)GZ 2 End of visibility window at Goldstone (5 deg elevation)GZ 3 End of visibility window at Goldstone (5 deg elevation)JY 1 Start of visibility window at Maspalomas (5 deg elevation)JY 2 Start of visibility window at Maspalomas (5 deg elevation)JY 3 Start of visibility window at Maspalomas (5 deg elevation)JY 4 Start of visibility window at Maspalomas (5 deg elevation)JZ 1 End of visibility window at Maspalomas (5 deg elevation)JZ 2 End of visibility window at Maspalomas (5 deg elevation)JZ 3 End of visibility window at Maspalomas (5 deg elevation)KA 1 Start of visibility window at Kourou (5 deg elevation)KA 2 Start of visibility window at Kourou (5 deg elevation)KA 3 Start of visibility window at Kourou (5 deg elevation)KA 4 Start of visibility window at Kourou (5 deg elevation)KL 1 End of visibility window at Kourou (5 deg elevation)KL 2 End of visibility window at Kourou (5 deg elevation)KL 3 End of visibility window at Kourou (5 deg elevation)KL 4 End of visibility window at Kourou (5 deg elevation)MY 1 Start of visibility window at Madrid (5 deg elevation)MY 2 Start of visibility window at Madrid (5 deg elevation)MY 3 Start of visibility window at Madrid (5 deg elevation)MY 4 Start of visibility window at Madrid (5 deg elevation)MZ 1 End of visibility window at Madrid (5 deg elevation)MZ 2 End of visibility window at Madrid (5 deg elevation)MZ 3 End of visibility window at Madrid (5 deg elevation)NS S Southbound neutral sheetNT I Enter north tail lobe from inner magnetospherePA 1 Start of visibility window at Perth (5 deg elevation)PA 2 Start of visibility window at Perth (5 deg elevation)PA 3 Start of visibility window at Perth (5 deg elevation)PA 4 Start of visibility window at Perth (5 deg elevation)PE _ PerigeePL 1 End of visibility window at Perth (5 deg elevation)PL 2 End of visibility window at Perth (5 deg elevation)PL 3 End of visibility window at Perth (5 deg elevation)PL 4 End of visibility window at Perth (5 deg elevation)PL 5 End of visibility window at Perth (5 deg elevation)QL I Inbound critical L value for auroral zoneQL O Outbound critical L value for auroral zoneRA 1 Start of visibility window at Redu (5 deg elevation)RA 2 Start of visibility window at Redu (5 deg elevation)RA 3 Start of visibility window at Redu (5 deg elevation)RA 4 Start of visibility window at Redu (5 deg elevation)RL 1 End of visibility window at Redu (5 deg elevation)RL 2 End of visibility window at Redu (5 deg elevation)RL 3 End of visibility window at Redu (5 deg elevation)RL 4 End of visibility window at Redu (5 deg elevation)RL 5 End of visibility window at Redu (5 deg elevation)ST O Leave south tail lobe for inner magnetosphereTL I Inbound radiation belt entry for WECTL O Outbound radiation belt exit for WECVL I Inbound critical L value for EDIVL O Outbound critical L value for EDIXL I Inbound critical L value for PEACEXL O Outbound critical L value for PEACEYL I Inbound critical L value for RAPIDYL O Outbound critical L value for RAPIDZL I Inbound critical L value for CISZL O Outbound critical L value for CIS

Counts based on variable 'Epoch__C1_JP_PSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/jp/pse/2000/c1_jp_pse_20000801_v07.cdf. The most common cadence, 1 [ms] = PT0.001S, occurred for 11.5830% of the 30 timesteps. 

Predicted Scientific Events (from all.xml/instrument/description/@short)

Orbit phase, fractional part of orbit number (non-event times do not plot)

Predicted gse Latitude of sc, Angle from Ecliptic Plane (non-event times do not plot)

Predicted magnetic local time of satellite (non-event times do not plot)

Spacecraft position at predicted event (non-event times do not plot)

NSSDC's Master Catalog on the Active Spacecraft Potential Control (ASPOC)

Introduction to the Active Spacecraft Potential Control (ASPOC) on Cluster II Rumba

SPDF/CDAWeb. Please also acknowledge the data producer: W. Riedler at IWF-OAW

SPDF/SSCWeb. Please also acknowledge the data producer: W. Riedler at IWF-OAW

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: W. Riedler at IWF-OAW

Counts based on variable 'Epoch__C1_PP_ASP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/pp/asp/2000/c1_pp_asp_20001209_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9814% of the 21532 timesteps. 

Active Spacecraft Potential Control (from all.xml/instrument/description/@short)

NSSDC Master Catalog listing for Cluster II Rumba Cluster Ion Spectrometry (CIS)

This site provides information concerning the Cluster II Rumba Cluster Ion Spectrometry Instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: H. Reme at CESR

SPDF/SSCWeb. Please also acknowledge the data producer: H. Reme at CESR

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: H. Reme at CESR

Cluster Ion Spectrometry (from all.xml/instrument/description/@short)

Information about the Digital Wave Processor (DWP) experiment on the Cluster 2/FM5 Rumba mission.

SPDF/CDAWeb. Please also acknowledge the data producer: H. Alleyne at Univ-Sheff

SPDF/SSCWeb. Please also acknowledge the data producer: H. Alleyne at Univ-Sheff

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: H. Alleyne at Univ-Sheff

Counts based on variable 'Epoch__C1_PP_DWP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/pp/dwp/2000/c1_pp_dwp_20001101_v01.cdf. The most common cadence, 3999 [ms] = PT3.999S, occurred for 58.1422% of the 12550 timesteps. 

Digital Wave Processor (from all.xml/instrument/description/@short)

NSSDC Master Catalog listing for the Cluster II Rumba Electron Drift Instrument (EDI)

This site provides information concerning the Cluster II Rumba Electron Drift Instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: G. Paschmann at MPE

SPDF/SSCWeb. Please also acknowledge the data producer: G. Paschmann at MPE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Paschmann at MPE

NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)

This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: G. Gustafsson at IRFU

SPDF/SSCWeb. Please also acknowledge the data producer: G. Gustafsson at IRFU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Gustafsson at IRFU

Counts based on variable 'Epoch__C1_PP_EFW' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/pp/efw/2000/c1_pp_efw_20001209_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9363% of the 10989 timesteps. 

Electric Fields and Waves (from all.xml/instrument/description/@short)

E-field spectral density, Freq range 0.3-10 Hz, from EFW waveform

E-field spectral density, Freq range 10-180 Hz, from EFW waveform

NSSDC Master Catalog listing for Cluster II Rumba Plasma Electron and Current Experiment (PEACE)

This site provides information concerning the Cluster II Rumba Plasma Electron and Current Experiment Instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: A. Fazakerley at MSSL

SPDF/SSCWeb. Please also acknowledge the data producer: A. Fazakerley at MSSL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Fazakerley at MSSL

Plasma Electron and Current Experiment (from all.xml/instrument/description/@short)

NSSDC Master Catalog listing for Cluster II Rumba Research with Adaptive Particle Imaging Detectors (RAPID)

This site provides information concerning the Cluster II Rumba Research with Adaptive Particle Imaging Detectors Instrument.

Energetic Electron and Ion Fluxes and Field-Aligned Anisotropies>1 spin averages

SPDF/CDAWeb. Please also acknowledge the data producer: B. Wilken and P. Daly at MPAe

SPDF/SSCWeb. Please also acknowledge the data producer: B. Wilken and P. Daly at MPAe

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: B. Wilken and P. Daly at MPAe

Counts based on variable 'Epoch__C1_PP_RAP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/pp/rap/2000/c1_pp_rap_20001209_v01.cdf. The most common cadence, 4001 [ms] = PT4.001S, occurred for 77.8141% of the 8558 timesteps. 

Research with Adaptive Particle Imaging Detectors (from all.xml/instrument/description/@short)

Ion Flux (m>4, E>100 kev), Integral heavy ion flux averaged over 4 pi

Ion Flux (m>4, E>300 kev), Integral heavy ion flux averaged over 4 pi

Field-aligned electron anisotropy (E>30 kev, (J(0)-J(180))/(J(0)+J(180))

Field-aligned proton anisotropy (E>30 kev, (J(0)-J(180))/(J(0)+J(180))

NSSDC Master Catalog listing for Cluster II Rumba Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF)

This site provides information concerning the Cluster II Rumba Spatio-Temporal Analysis of Magnetic Field Fluctuations Instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: N. Cornilleau-Wehrlin at CETP

SPDF/SSCWeb. Please also acknowledge the data producer: N. Cornilleau-Wehrlin at CETP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: N. Cornilleau-Wehrlin at CETP

Counts based on variable 'Epoch__C1_PP_STA' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/pp/sta/2000/c1_pp_sta_20001209_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 73.3679% of the 7226 timesteps. 

Spatio-Temporal Analysis of Field Fluctuations (from all.xml/instrument/description/@short)

E-field Spectral Density, Frequency Range 10 - 180 Hz from STAFF Spectrum analyser

E-field Spectral Density, Frequency Range 180 - 4000 Hz from STAFF Spectrum Analyser

NSSDC Master Catalog listing for Cluster II Rumba Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER)

This site provides information concerning the Cluster II Rumba Waves of HF and Sounder for Probing Electron Density by Relaxation Instrument.

WHISPER/E-Power>4-80 kHz/Electron Density from Relaxation Sounding

SPDF/CDAWeb. Please also acknowledge the data producer: P.M.E. Decreau at LPCE

SPDF/SSCWeb. Please also acknowledge the data producer: P.M.E. Decreau at LPCE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: P.M.E. Decreau at LPCE

Counts based on variable 'Epoch__C1_PP_WHI' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/pp/whi/2000/c1_pp_whi_20001210_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9599% of the 12450 timesteps. 

Waves of High Frequency and Sounder for Probing of Density by Relaxation (from all.xml/instrument/description/@short)

Preliminary electron density derived from plasma frequency recognition (consult quality flag and PI before use)

Quality of the resonance recognition, Degree of confidence between 0 and 100

E-field Spectral Density, Freq range 4-10 kHz from WHISPER natural noise analyser

E-field spectral density, Freq range 10-20 kHz from WHISPER natural noise analyser

E-field spectral density, Freq range 20-80 kHz from WHISPER natural nopise analyser

Normalized standard deviation of E power in 2-80 kHz range from time samples

Cluster Spacecraft 1, FluxGate Magnetometer (FGM) Unvalidated Prime Parameters

A. Balogh et al, The Cluster Magnetic Field InvestigationSpace Sci. Rev., 79,  pp 65 - 92, 1997)

Note:  Cluster active archive Parameter FGM data (CP_FGM_SPIN) when possible should be used in preference to these FGM Prime Parameter or Summary data.

SPDF/CDAWeb. Please also acknowledge the data producer: A. Balogh at ICSTM

SPDF/SSCWeb. Please also acknowledge the data producer: A. Balogh at ICSTM

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Balogh at ICSTM

Counts based on variable 'Epoch__C1_UP_FGM' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/up/fgm/2019/c1_up_fgm_20190201_v01.cdf. The most common cadence, 4299 [ms] = PT4.299S, occurred for 77.9588% of the 15598 timesteps. 

Fluxgate Magnetometer (from all.xml/instrument/description/@short)

Unvalidated Prime Parameter (from Master/CDFglobalAttributes/Data_type)

FGM DC magnetic field, interval centred data from primary sensor

Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data

High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor.  The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system....CALIBRATION:...The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'cluster_wbd_calibration.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255.  Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number....CONVERSION TO FREQUENCY DOMAIN:...In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out:  1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any....Bandwidth   Sample Rate---------   ------------9.5 kHz      27.443 kHz 19 kHz       54.886 kHz 77 kHz      219.544 kHz ...COORDINATE SYSTEM USED:...One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane....

Users of the Cluster WBD data are encouraged to acknowledge NASA Goddard Space Flight Center and The University of Iowa as the source of the data in any publication.

Overview and high time resolution spectrograms, documentation, and data coverage files

High time resolution spectrograms, documentation, and data coverage files

Cluster WBD Instrument page maintained by the University of Iowa with links to instrument descriptions and team members, publications, lists of coordinated observing times, science data availability catalogs, data, data interpretation and caveat descriptions as well as data analysis tools.

Cluster WBD documentation with links to lists of coordinated observing times, science data availability catalogs, WBD User Guide, WBD Calibration Report, WBD Interface Control Document, and data interpretation and caveat descriptions.

Cluster WBD data are open to everyone.  However, users of these data are encouraged to contact the PI Institute should questions arise.

SPDF/CDAWeb. Please also acknowledge the data producer: 2006 - Current:  J. S. Pickett; 1988 - 2006:  D. A. Gurnett at The University of  Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: 2006 - Current:  J. S. Pickett; 1988 - 2006:  D. A. Gurnett at The University of  Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: 2006 - Current:  J. S. Pickett; 1988 - 2006:  D. A. Gurnett at The University of  Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/wbd/2001/01/c1_waveform_wbd_200101041530_v01.cdf. The most common cadence, 36439104 [ps] = PT0.000036439S, occurred for 58.3486% of the 6207082 timesteps. 

Wide Band Data Plasma Wave Receiver (from all.xml/instrument/description/@short)

Base freq. of freq. bandwidth (0.0, 125.454, 250.908, and 501.816 kHz)

Number of bits used when digitizing waveform (8-bit, 4-bit, or 1-bit)

Total angle between antenna used for WBD measurement and measured B field direction

Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane

DC Offset used when converting from raw digital values to calibrated data

Data Quality: 0 = OK, 1 = clipped or questionable, 2 = bad data point.

High time resolution calibrated waveform data sampled in one of 3 frequency bandwidths in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor.  The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system....CALIBRATION:...The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'CAA_EST_CR_WBD_v20.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255.  Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number....CONVERSION TO FREQUENCY DOMAIN:...In order to convert the WBD data to the frequency domain via an FFT, see 'CAA_EST_CR_WBD_v20.pdf'. The steps for converting are briefly outlined below: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth VAR_NOTES for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table in VAR_NOTES of the 'BM_Mode' variable for the appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any;7) if Translation is not equal to 0, add the appropriate translation frequency to each frequency component (see Translation CATDESC for the exact values)....COORDINATE SYSTEM USED:...One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane....

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c1/wbd_bm2/2000/09/c1_waveform_wbd_bm2_200009080350_v01.cdf. The most common cadence, 4554888 [ps] = PT0.000004555S, occurred for 58.0066% of the 3057033 timesteps. 

Wide Band Data Plasma Wave Receiver Burst Mode(BM2) (from all.xml/instrument/description/@short)

BM_Mode (0=Duty Cycled 9.5 kHz, 1-in-3,1 = Duty Cycled 9.5 kHz, 1-in-4, 2 = Duty Cycled 19 kHz, 1-in-3, 3 = Duty Cycled 19 kHz, 1-in-4, 4 = Duty Cycled 77 kHz, 1-in-3, 5 = Duty Cycled 77 kHz, 1-in-4, 6 = Digital Filtered 9.5 kHz, 1-in-3,      roll-off at 3.2 kHz 7 = Digital Filtered 9.5 kHz, 1-in-3,      optimized roll-off at 4.2 kHz 8 = Digital Filtered 9.5 kHz, 1-in-4,      roll-off at 2.5 kHz 9 = Digital Filtered 9.5 kHz, 1-in-4,      optimized roll-off at 3.1 kHz)

Counts based on variable 'time_tags__C2_CP_EDI_AEDC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/edi/ambientelectron_counts_passivemode_mixedreso/2004/c2_cp_edi_aedc_20041014_v20191220.cdf. The most common cadence, 62 [ms] = PT0.062S, occurred for 50.0218% of the 686923 timesteps. 

Cluster Satellite No 2 (from all.xml/observatory/description/@short)

Cluster Satellite No 2 (from Master/CDFglobalAttributes/Source_name)

Cluster C2, corrected ambient electron counts GDU1 PA=180 degree

Cluster C2, corrected ambient electron counts GDU2 PA=180 degree

Counts based on variable 'time_tags__C2_CP_EDI_MP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/edi/electron_driftvelo_efield_3dvect_bestreso/2001/c2_cp_edi_mp_20010202_v20180117.cdf. The most common cadence, 2009 [ms] = PT2.009S, occurred for 11.8426% of the 322 timesteps. 

Counts based on variable 'time_tags__C2_CP_EDI_QZC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/edi/backgroundelectron_counts_activemode_mixedreso/2001/c2_cp_edi_qzc_20010202_v20220630.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 98.6560% of the 447246 timesteps. 

Counts based on variable 'time_tags__C2_CP_EDI_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/edi/electron_driftvelo_efield_3dvect_spinreso/2001/c2_cp_edi_spin_20010202_v20220316.cdf. The most common cadence, 4018 [ms] = PT4.018S, occurred for 27.2810% of the 299 timesteps. 

Counts based on variable 'time_tags__C2_CP_EFW_L3_E3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/efw/efield_3dvect_spinreso_l3_inertialframe/2000/c2_cp_efw_l3_e3d_inert_20001202_v20221114.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 428 timesteps. 

Counts based on variable 'time_tags__C2_CP_EFW_L3_P' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/efw/scpotential_spinreso_l3/2000/c2_cp_efw_l3_p_20001201_v20221111.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 99.9821% of the 5600 timesteps. 

Counts based on variable 'time_tags__C2_CP_EFW_L3_V3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/efw/driftvelo_3dvect_spinreso_l3_inertialframe/2000/c2_cp_efw_l3_v3d_inert_20001202_v20221114.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 428 timesteps. 

Counts based on variable 'time_tags__C2_CP_FGM_5VPS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/fgm/mfield_3dvect_5vectpersec/2000/c2_cp_fgm_5vps_20001202_v20151004.cdf. The most common cadence, 200 [ms] = PT0.2S, occurred for all 9118 timesteps. 

Cluster Spacecraft 2 FluxGate Magnetometer (FGM) Spin-Resolution Parameters

Counts based on variable 'time_tags__C2_CP_FGM_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/cp/2001/c2_cp_fgm_spin_20010130_v01.cdf. The most common cadence, 4017 [ms] = PT4.017S, occurred for 91.7595% of the 824 timesteps. 

Cluster spacecraft 2 (from all.xml/observatory/description/@short)

FluxGate Magnetometer Spin Resolution (from all.xml/instrument/description/@short)

Cluster spacecraft 2 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Time_tags__C2_CP_RAP_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-ies/electron_3ddist_bestreso/2000/c2_cp_rap_e3dd_20001216_v20230309.cdf. The most common cadence, 4015 [ms] = PT4.015S, occurred for 72.1469% of the 4792 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_ESPCT6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-ies/electron_omni_spinreso/2000/c2_cp_rap_espct6_20001207_v20230309.cdf. The most common cadence, 4015 [ms] = PT4.015S, occurred for 49.9306% of the 7554 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_HSPCT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/proton_omni_spinreso/2000/c2_cp_rap_hspct_20001207_v20230309.cdf. The most common cadence, 4015 [ms] = PT4.015S, occurred for 49.9534% of the 7503 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_I3DM_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/cno_3ddist_stdreso/2000/c2_cp_rap_i3dm_cno_20001207_v20230309.cdf. The most common cadence, 128465 [ms] = PT2M8.465S, occurred for 50.8621% of the 236 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_I3DM_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/proton_3ddist_stdreso/2000/c2_cp_rap_i3dm_h_20001207_v20230309.cdf. The most common cadence, 128465 [ms] = PT2M8.465S, occurred for 50.8621% of the 236 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_I3DM_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/he_3ddist_stdreso/2000/c2_cp_rap_i3dm_he_20001207_v20230309.cdf. The most common cadence, 128465 [ms] = PT2M8.465S, occurred for 50.8621% of the 236 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_ISPCT_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/cno_omni_spinreso/2000/c2_cp_rap_ispct_cno_20001207_v20230309.cdf. The most common cadence, 32116 [ms] = PT32.116S, occurred for 56.5618% of the 1043 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_ISPCT_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/he_omni_spinreso/2000/c2_cp_rap_ispct_he_20001207_v20230309.cdf. The most common cadence, 32116 [ms] = PT32.116S, occurred for 56.5618% of the 1043 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-ies/electron_3ddist_2echannels_stdreso/2004/c2_cp_rap_l3dd_20040513_v20210208.cdf. The most common cadence, 3835 [ms] = PT3.835S, occurred for 55.5088% of the 3824 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_PAD_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-ies/electron_pitchangle_bestreso/2000/c2_cp_rap_pad_e3dd_20001216_v20230309.cdf. The most common cadence, 4015 [ms] = PT4.015S, occurred for 72.1344% of the 4789 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_PAD_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/proton_pitchangle_stdreso/2000/c2_cp_rap_pad_h_20001207_v20230309.cdf. The most common cadence, 128465 [ms] = PT2M8.465S, occurred for 50.8621% of the 236 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_PAD_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-iims/he_pitchangle_stdreso/2000/c2_cp_rap_pad_he_20001207_v20230309.cdf. The most common cadence, 128465 [ms] = PT2M8.465S, occurred for 50.8621% of the 236 timesteps. 

Counts based on variable 'Time_tags__C2_CP_RAP_PAD_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/rap-ies/electron_pitchangle_2echannels_stdreso/2004/c2_cp_rap_pad_l3dd_20040513_v20210208.cdf. The most common cadence, 3835 [ms] = PT3.835S, occurred for 55.5088% of the 3824 timesteps. 

Counts based on variable 'Time__C2_CP_STA_CWF_GSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/sta/mfield_calibwaveform_gse/2000/c2_cp_sta_cwf_gse_20000905_v20220603.cdf. The most common cadence, 39999000000 [ps] = PT0.039999S, occurred for 56.5884% of the 21185 timesteps. 

Counts based on variable 'Time__C2_CP_STA_PPP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/sta/polarization_propagation/2000/c2_cp_sta_ppp_20001202_v20160526.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 92.9360% of the 421 timesteps. 

Azymuthal Angle of the direction of propagation in MFA coordinate system (SVD).

Counts based on variable 'Time__C2_CP_STA_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/sta/powerspectraldensity/2000/c2_cp_sta_psd_20000905_v20220608.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for 97.9038% of the 794 timesteps. 

Counts based on variable 'Time__C2_CP_STA_SM' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/sta/crossspectralmatrice/2000/c2_cp_sta_sm_20000905_v20220608.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 91.5842% of the 185 timesteps. 

Counts based on variable 'time_tags__C2_CP_WHI_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/whi/efield_spectralpowerdensity_soundingmode/2000/c2_cp_whi_active_20000905_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 40.6557% of the 124 timesteps. 

Counts based on variable 'time_tags__C2_CP_WHI_ELECTRON_DENSITY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/whi/electron_density/2001/c2_cp_whi_electron_density_20010207_v20160311.cdf. The most common cadence, 214 [ms] = PT0.214S, occurred for 21.2913% of the 3400 timesteps. 

Counts based on variable 'time_tags__C2_CP_WHI_NATURAL' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/whi/efield_spectralpowerdensity_naturalmode/2000/c2_cp_whi_natural_20000905_v20150715.cdf. The most common cadence, 856 [ms] = PT0.856S, occurred for 52.2523% of the 58 timesteps. 

Counts based on variable 'time_tags__C2_CP_WHI_PASSIVE_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/whi/efield_passivespectralpowerdensity_soundingmode/2000/c2_cp_whi_passive_active_20000905_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 48.6275% of the 124 timesteps. 

Counts based on variable 'time_tags__C2_CP_WHI_WAVE_FORM_ENERGY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/whi/efield_integratedpowerdensity_naturalmode/2000/c2_cp_whi_wave_form_energy_20000905_v20150715.cdf. The most common cadence, 856 [ms] = PT0.856S, occurred for 61.0526% of the 58 timesteps. 

Counts based on variable 'Epoch__C2_JP_PMP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/jp/pmp/2000/c2_jp_pmp_20000814_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 4936 timesteps. 

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)AP _ ApogeeCY 1 Start of visibility window at Canberra (5 deg elevation)CY 2 Start of visibility window at Canberra (5 deg elevation)CY 3 Start of visibility window at Canberra (5 deg elevation)CZ 1 End of visibility window at Canberra (5 deg elevation)CZ 2 End of visibility window at Canberra (5 deg elevation)CZ 3 End of visibility window at Canberra (5 deg elevation)CZ 4 End of visibility window at Canberra (5 deg elevation)DY 1 Start of visibility window at Vilspa (5 deg elevation)DY 2 Start of visibility window at Vilspa (5 deg elevation)DY 3 Start of visibility window at Vilspa (5 deg elevation)DY 4 Start of visibility window at Vilspa (5 deg elevation)DZ 1 End of visibility window at Vilspa (5 deg elevation)DZ 2 End of visibility window at Vilspa (5 deg elevation)DZ 3 End of visibility window at Vilspa (5 deg elevation)GY 1 Start of visibility window at Goldstone (5 deg elevation)GY 2 Start of visibility window at Goldstone (5 deg elevation)GY 3 Start of visibility window at Goldstone (5 deg elevation)GY 4 Start of visibility window at Goldstone (5 deg elevation)GZ 1 End of visibility window at Goldstone (5 deg elevation)GZ 2 End of visibility window at Goldstone (5 deg elevation)GZ 3 End of visibility window at Goldstone (5 deg elevation)JY 1 Start of visibility window at Maspalomas (5 deg elevation)JY 2 Start of visibility window at Maspalomas (5 deg elevation)JY 3 Start of visibility window at Maspalomas (5 deg elevation)JY 4 Start of visibility window at Maspalomas (5 deg elevation)JZ 1 End of visibility window at Maspalomas (5 deg elevation)JZ 2 End of visibility window at Maspalomas (5 deg elevation)JZ 3 End of visibility window at Maspalomas (5 deg elevation)KA 1 Start of visibility window at Kourou (5 deg elevation)KA 2 Start of visibility window at Kourou (5 deg elevation)KA 3 Start of visibility window at Kourou (5 deg elevation)KA 4 Start of visibility window at Kourou (5 deg elevation)KL 1 End of visibility window at Kourou (5 deg elevation)KL 2 End of visibility window at Kourou (5 deg elevation)KL 3 End of visibility window at Kourou (5 deg elevation)KL 4 End of visibility window at Kourou (5 deg elevation)MY 1 Start of visibility window at Madrid (5 deg elevation)MY 2 Start of visibility window at Madrid (5 deg elevation)MY 3 Start of visibility window at Madrid (5 deg elevation)MY 4 Start of visibility window at Madrid (5 deg elevation)MZ 1 End of visibility window at Madrid (5 deg elevation)MZ 2 End of visibility window at Madrid (5 deg elevation)MZ 3 End of visibility window at Madrid (5 deg elevation)NS S Southbound neutral sheetNT I Enter north tail lobe from inner magnetospherePA 1 Start of visibility window at Perth (5 deg elevation)PA 2 Start of visibility window at Perth (5 deg elevation)PA 3 Start of visibility window at Perth (5 deg elevation)PE _ PerigeePL 1 End of visibility window at Perth (5 deg elevation)PL 2 End of visibility window at Perth (5 deg elevation)PL 3 End of visibility window at Perth (5 deg elevation)PL 4 End of visibility window at Perth (5 deg elevation)QL I Inbound critical L value for auroral zoneQL O Outbound critical L value for auroral zoneRA 1 Start of visibility window at Redu (5 deg elevation)RA 2 Start of visibility window at Redu (5 deg elevation)RA 3 Start of visibility window at Redu (5 deg elevation)RA 4 Start of visibility window at Redu (5 deg elevation)RL 1 End of visibility window at Redu (5 deg elevation)RL 2 End of visibility window at Redu (5 deg elevation)RL 3 End of visibility window at Redu (5 deg elevation)RL 4 End of visibility window at Redu (5 deg elevation)ST O Leave south tail lobe for inner magnetosphereTL I Inbound radiation belt entry for WECTL O Outbound radiation belt exit for WECVL I Inbound critical L value for EDIVL O Outbound critical L value for EDIWL I Inbound critical L value for ASPOCWL O Outbound critical L value for ASPOCXL I Inbound critical L value for PEACEXL O Outbound critical L value for PEACEYL I Inbound critical L value for RAPIDYL O Outbound critical L value for RAPIDZL I Inbound critical L value for CISZL O Outbound critical L value for CIS

Counts based on variable 'Epoch__C2_JP_PSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/jp/pse/2000/c2_jp_pse_20000801_v06.cdf. The most common cadence, 1 [ms] = PT0.001S, occurred for 10.9489% of the 30 timesteps. 

Introduction to the Active Spacecraft Potential Control (ASPOC) on Cluster II Salsa

Counts based on variable 'Epoch__C2_PP_ASP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/pp/asp/2000/c2_pp_asp_20001209_v01.cdf. The most common cadence, 4014 [ms] = PT4.014S, occurred for 99.9441% of the 21453 timesteps. 

Information about the Digital Wave Processor (DWP) experiment on the Cluster 2/FM5 Salsa mission.

Counts based on variable 'Epoch__C2_PP_DWP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/pp/dwp/2000/c2_pp_dwp_20001101_v01.cdf. The most common cadence, 4013 [ms] = PT4.013S, occurred for 95.6530% of the 20574 timesteps. 

NSSDC Master Catalog listing for the Cluster II Salsa Electron Drift Instrument (EDI)

This site provides information concerning the Cluster II Salsa Electron Drift Instrument.

NSSDC Master Catalog listing for Cluster II Salsa Electric Field and Waves (EFW)

This site provides information concerning the Cluster II Salsa Electric Field and Waves Instrument.

Counts based on variable 'Epoch__C2_PP_EFW' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/pp/efw/2024/c2_pp_efw_20240531_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9768% of the 21579 timesteps. 

NSSDC Master Catalog listing for Cluster II Salsa Plasma Electron and Current Experiment (PEACE)

This site provides information concerning the Cluster II Salsa Plasma Electron and Current Experiment Instrument.

NSSDC Master Catalog listing for Cluster II Salsa Research with Adaptive Particle Imaging Detectors (RAPID)

This site provides information concerning the Cluster II Salsa Research with Adaptive Particle Imaging Detectors Instrument.

Counts based on variable 'Epoch__C2_PP_RAP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/pp/rap/2000/c2_pp_rap_20001209_v01.cdf. The most common cadence, 4015 [ms] = PT4.015S, occurred for 60.8148% of the 7240 timesteps. 

NSSDC Master Catalog listing for Cluster II Salsa Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF)

This site provides information concerning the Cluster II Salsa Spatio-Temporal Analysis of Magnetic Field Fluctuations Instrument.

Counts based on variable 'Epoch__C2_PP_STA' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/pp/sta/2000/c2_pp_sta_20001209_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 79.3831% of the 7824 timesteps. 

NSSDC Master Catalog listing for Cluster II Salsa Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER)

This site provides information concerning the Cluster II Salsa Waves of HF and Sounder for Probing Electron Density by Relaxation Instrument.

Counts based on variable 'Epoch__C2_PP_WHI' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/pp/whi/2000/c2_pp_whi_20001210_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9759% of the 12450 timesteps. 

Preliminary electron Density derived from plasma frequency recognition (consult quality flag and PI before use)

Cluster Spacecraft 2, FluxGate Magnetometer (FGM) Unvalidated Prime Parameters

NSSDC Master Catalog listing for Cluster II Salsa Fluxgate Magnetometer (FGM)

This site provides information concerning the Cluster II Salsa Fluxgate Magnetometer Instrument.

Counts based on variable 'Epoch__C2_UP_FGM' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/up/fgm/2019/c2_up_fgm_20190201_v01.cdf. The most common cadence, 4201 [ms] = PT4.201S, occurred for 99.3650% of the 20344 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/wbd/2001/01/c2_waveform_wbd_200101041510_v01.cdf. The most common cadence, 36439099 [ps] = PT0.000036439S, occurred for 64.6398% of the 6230092 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c2/wbd_bm2/2000/09/c2_waveform_wbd_bm2_200009052350_v01.cdf. The most common cadence, 18219550 [ps] = PT0.000018220S, occurred for 30.8399% of the 795005 timesteps. 

This dataset contains CIS-CODIF Proton omni-directional distributions

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_H1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/proton_omni/2001/c3_cp_cis-codif_h1_1d_pef_20010110_v20151107.cdf. The most common cadence, 16009 [ms] = PT16.009S, occurred for 33.3333% of the 2 timesteps. 

Cluster Satellite No 3 (from all.xml/observatory/description/@short)

Cluster Satellite No 3 (from Master/CDFglobalAttributes/Source_name)

This dataset contains CIS-CODIF Helium+ omni-directional distributions

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_He1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/heplus_omni/2001/c3_cp_cis-codif_he1_1d_pef_20010110_v20151107.cdf. The most common cadence, 16020 [ms] = PT16.02S, occurred for 50.0000% of the 4 timesteps. 

CIS-CODIF 3D Proton distributions on C3, High-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_H1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/proton_3ddist_highsens_diffenergyflux/2001/c3_cp_cis-codif_hs_h1_pef_20010110_v20151026.cdf. The most common cadence, 16009 [ms] = PT16.009S, occurred for 33.3333% of the 2 timesteps. 

for the High-Sensitivity side of spacecraft C3, in Differential_Particle_Flux units

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/proton_3ddist_highsens_diffparticleflux/2001/c3_cp_cis-codif_hs_h1_pf_20010110_v20151026.cdf. The most common cadence, 16009 [ms] = PT16.009S, occurred for 33.3333% of the 2 timesteps. 

CIS-CODIF 3D Proton distributions on C3, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_H1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/proton_3ddist_highsens_phasespacedens/2001/c3_cp_cis-codif_hs_h1_psd_20010110_v20151026.cdf. The most common cadence, 16009 [ms] = PT16.009S, occurred for 33.3333% of the 2 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/heplus_3ddist_highsens_diffparticleflux/2001/c3_cp_cis-codif_hs_he1_pf_20010110_v20151027.cdf. The most common cadence, 16020 [ms] = PT16.02S, occurred for 50.0000% of the 4 timesteps. 

CIS-CODIF 3D Helium+ distributions on C3, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_He1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/heplus_3ddist_highsens_phasespacedens/2001/c3_cp_cis-codif_hs_he1_psd_20010110_v20151028.cdf. The most common cadence, 16020 [ms] = PT16.02S, occurred for 50.0000% of the 4 timesteps. 

for the High-Sensitivity side of spacecraft C3, in Particle_Energy_Flux units

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_O1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/oplus_3ddist_highsens_diffenergyflux/2001/c3_cp_cis-codif_hs_o1_pef_20010110_v20151104.cdf. The most common cadence, 16020 [ms] = PT16.02S, occurred for 25.0000% of the 2 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C3, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/oplus_3ddist_highsens_diffparticleflux/2001/c3_cp_cis-codif_hs_o1_pf_20010110_v20151104.cdf. The most common cadence, 16020 [ms] = PT16.02S, occurred for 25.0000% of the 2 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C3, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_HS_O1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/oplus_3ddist_highsens_phasespacedens/2001/c3_cp_cis-codif_hs_o1_psd_20010110_v20151106.cdf. The most common cadence, 16020 [ms] = PT16.02S, occurred for 25.0000% of the 2 timesteps. 

CIS-CODIF 1D Oxygen+ distributions on C3 in Particle_Energy_Flux

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_O1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/oplus_omni/2005/c3_cp_cis-codif_o1_1d_pef_20050122_v20151107.cdf. The most common cadence, 16522 [ms] = PT16.522S, occurred for 12.9390% of the 501 timesteps. 

CIS-CODIF Proton Pitch-Angle Distribution, High-sensitivity side, in Differential_Particle_Flux

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_PAD_HS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/proton_pitchangle_highsens_diffparticleflux/2001/c3_cp_cis-codif_pad_hs_h1_pf_20010131_v20220812.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 17.1652% of the 1360 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_PAD_HS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/heplus_pitchangle_highsens_diffparticleflux/2001/c3_cp_cis-codif_pad_hs_he1_pf_20010131_v20220812.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 26.0937% of the 1342 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_CODIF_PAD_HS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-codif/oplus_pitchangle_highsens_diffparticleflux/2001/c3_cp_cis-codif_pad_hs_o1_pf_20010131_v20220812.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 25.1192% of the 1317 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_omni_highsens/2001/c3_cp_cis-hia_hs_1d_pef_20010110_v20090720.cdf. The most common cadence, 12014 [ms] = PT12.014S, occurred for 20.0000% of the 2 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_MAG_IONS_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_magmode_highsens_diffenergyflux/2001/c3_cp_cis-hia_hs_mag_ions_pef_20010110_v20220805.cdf. The most common cadence, 12014 [ms] = PT12.014S, occurred for 20.0000% of the 2 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_MAG_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_magmode_highsens_diffparticleflux/2001/c3_cp_cis-hia_hs_mag_ions_pf_20010110_v20220805.cdf. The most common cadence, 12014 [ms] = PT12.014S, occurred for 20.0000% of the 2 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_MAG_IONS_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_magmode_highsens_phasespacedens/2001/c3_cp_cis-hia_hs_mag_ions_psd_20010110_v20220805.cdf. The most common cadence, 12014 [ms] = PT12.014S, occurred for 20.0000% of the 2 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_SW_IONS_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_swmode_highsens_diffenergyflux/2001/c3_cp_cis-hia_hs_sw_ions_pef_20010112_v20220804.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 36.0491% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_SW_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_swmode_highsens_diffparticleflux/2001/c3_cp_cis-hia_hs_sw_ions_pf_20010112_v20220804.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 36.0491% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_HS_SW_IONS_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_swmode_highsens_phasespacedens/2001/c3_cp_cis-hia_hs_sw_ions_psd_20010112_v20220804.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 36.0491% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_LS_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_omni_lowsens/2001/c3_cp_cis-hia_ls_1d_pef_20010112_v20090720.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 27.7889% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_LS_SW_IONS_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_swmode_lowsens_diffenergyflux/2001/c3_cp_cis-hia_ls_sw_ions_pef_20010112_v20220804.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 27.7889% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_LS_SW_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_swmode_lowsens_diffparticleflux/2001/c3_cp_cis-hia_ls_sw_ions_pf_20010112_v20220804.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 27.7889% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_LS_SW_IONS_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_3ddist_swmode_lowsens_phasespacedens/2001/c3_cp_cis-hia_ls_sw_ions_psd_20010112_v20220804.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 27.7889% of the 969 timesteps. 

Counts based on variable 'time_tags__C3_CP_CIS_HIA_PAD_HS_MAG_IONS_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cis-hia/ions_pitchangle_magmode_highsens_diffparticleflux/2001/c3_cp_cis-hia_pad_hs_mag_ions_pf_20010131_v20220812.cdf. The most common cadence, 4010 [ms] = PT4.01S, occurred for 24.2665% of the 1373 timesteps. 

Counts based on variable 'time_tags__C3_CP_EDI_AEDC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/edi/ambientelectron_counts_passivemode_mixedreso/2004/c3_cp_edi_aedc_20041014_v20191220.cdf. The most common cadence, 62 [ms] = PT0.062S, occurred for 50.0217% of the 567295 timesteps. 

Cluster C3, corrected ambient electron counts GDU1 PA=180 degree

Cluster C3, corrected ambient electron counts GDU2 PA=180 degree

Counts based on variable 'time_tags__C3_CP_EDI_MP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/edi/electron_driftvelo_efield_3dvect_bestreso/2001/c3_cp_edi_mp_20010202_v20180117.cdf. The most common cadence, 2003 [ms] = PT2.003S, occurred for 17.6414% of the 546 timesteps. 

Counts based on variable 'time_tags__C3_CP_EDI_QZC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/edi/backgroundelectron_counts_activemode_mixedreso/2001/c3_cp_edi_qzc_20010202_v20220630.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 98.3163% of the 440168 timesteps. 

Counts based on variable 'time_tags__C3_CP_EDI_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/edi/electron_driftvelo_efield_3dvect_spinreso/2001/c3_cp_edi_spin_20010202_v20220316.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 43.5801% of the 465 timesteps. 

Counts based on variable 'time_tags__C3_CP_EFW_L3_E3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/efw/efield_3dvect_spinreso_l3_inertialframe/2000/c3_cp_efw_l3_e3d_inert_20001202_v20221114.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 473 timesteps. 

Counts based on variable 'time_tags__C3_CP_EFW_L3_P' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/efw/scpotential_spinreso_l3/2000/c3_cp_efw_l3_p_20001201_v20221111.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 99.9641% of the 5573 timesteps. 

Counts based on variable 'time_tags__C3_CP_EFW_L3_V3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/efw/driftvelo_3dvect_spinreso_l3_inertialframe/2000/c3_cp_efw_l3_v3d_inert_20001202_v20221114.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for all 473 timesteps. 

Counts based on variable 'time_tags__C3_CP_FGM_5VPS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/fgm/mfield_3dvect_5vectpersec/2000/c3_cp_fgm_5vps_20001202_v20150131.cdf. The most common cadence, 200 [ms] = PT0.2S, occurred for 99.9394% of the 9891 timesteps. 

Cluster Spacecraft 3 FluxGate Magnetometer (FGM) Spin-Resolution Parameters

Counts based on variable 'time_tags__C3_CP_FGM_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/cp/2001/c3_cp_fgm_spin_20010130_v01.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 70.3668% of the 729 timesteps. 

Cluster spacecraft 3 (from all.xml/observatory/description/@short)

Cluster spacecraft 3 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Time_tags__C3_CP_RAP_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-ies/electron_3ddist_bestreso/2000/c3_cp_rap_e3dd_20001207_v20230309.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 82.3191% of the 4721 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_ESPCT6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-ies/electron_omni_spinreso/2000/c3_cp_rap_espct6_20001205_v20230309.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 79.7357% of the 181 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_HSPCT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/proton_omni_spinreso/2000/c3_cp_rap_hspct_20001207_v20230309.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 79.8415% of the 6650 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_I3DM_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/cno_3ddist_stdreso/2000/c3_cp_rap_i3dm_cno_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 59.6424% of the 467 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_I3DM_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/proton_3ddist_stdreso/2000/c3_cp_rap_i3dm_h_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 59.6424% of the 467 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_I3DM_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/he_3ddist_stdreso/2000/c3_cp_rap_i3dm_he_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 59.6424% of the 467 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_ISPCT_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/cno_omni_spinreso/2000/c3_cp_rap_ispct_cno_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 65.6615% of the 675 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_ISPCT_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/he_omni_spinreso/2000/c3_cp_rap_ispct_he_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 65.6615% of the 675 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-ies/electron_3ddist_2echannels_stdreso/2004/c3_cp_rap_l3dd_20040430_v20210208.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 72.5685% of the 10804 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_PAD_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/cno_pitchangle_stdreso/2000/c3_cp_rap_pad_cno_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 59.6424% of the 467 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_PAD_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-ies/electron_pitchangle_bestreso/2000/c3_cp_rap_pad_e3dd_20001207_v20230309.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 82.3529% of the 4718 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_PAD_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/proton_pitchangle_stdreso/2000/c3_cp_rap_pad_h_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 59.6424% of the 467 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_PAD_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-iims/he_pitchangle_stdreso/2000/c3_cp_rap_pad_he_20001207_v20230309.cdf. The most common cadence, 32032 [ms] = PT32.032S, occurred for 59.6424% of the 467 timesteps. 

Counts based on variable 'Time_tags__C3_CP_RAP_PAD_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/rap-ies/electron_pitchangle_2echannels_stdreso/2004/c3_cp_rap_pad_l3dd_20040430_v20210208.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 72.5685% of the 10804 timesteps. 

Counts based on variable 'Time__C3_CP_STA_CWF_GSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/sta/mfield_calibwaveform_gse/2000/c3_cp_sta_cwf_gse_20001009_v20220610.cdf. The most common cadence, 40000000000 [ps] = PT0.04S, occurred for 69.5271% of the 20863 timesteps. 

Counts based on variable 'Time__C3_CP_STA_PPP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/sta/polarization_propagation/2000/c3_cp_sta_ppp_20001207_v20160526.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for 79.7146% of the 11506 timesteps. 

Azymuthal angle of the direction of propagation in MFA coordinate system (SVD).

Counts based on variable 'Time__C3_CP_STA_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/sta/powerspectraldensity/2000/c3_cp_sta_psd_20001009_v20220608.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for all 3 timesteps. 

Counts based on variable 'time_tags__C3_CP_WHI_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/whi/efield_spectralpowerdensity_soundingmode/2000/c3_cp_whi_active_20001011_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 40.9241% of the 124 timesteps. 

Counts based on variable 'time_tags__C3_CP_WHI_ELECTRON_DENSITY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/whi/electron_density/2001/c3_cp_whi_electron_density_20010207_v20160311.cdf. The most common cadence, 214 [ms] = PT0.214S, occurred for 16.1621% of the 2178 timesteps. 

Counts based on variable 'time_tags__C3_CP_WHI_NATURAL' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/whi/efield_spectralpowerdensity_naturalmode/2000/c3_cp_whi_natural_20001011_v20150715.cdf. The most common cadence, 856 [ms] = PT0.856S, occurred for 49.5495% of the 55 timesteps. 

Counts based on variable 'time_tags__C3_CP_WHI_PASSIVE_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/whi/efield_passivespectralpowerdensity_soundingmode/2000/c3_cp_whi_passive_active_20001011_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 49.0119% of the 124 timesteps. 

Counts based on variable 'time_tags__C3_CP_WHI_WAVE_FORM_ENERGY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/whi/efield_integratedpowerdensity_naturalmode/2000/c3_cp_whi_wave_form_energy_20001011_v20150715.cdf. The most common cadence, 856 [ms] = PT0.856S, occurred for 57.8947% of the 55 timesteps. 

Counts based on variable 'Epoch__C3_JP_PMP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/jp/pmp/2000/c3_jp_pmp_20000814_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 4936 timesteps. 

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)AP _ ApogeeCY 1 Start of visibility window at Canberra (5 deg elevation)CY 2 Start of visibility window at Canberra (5 deg elevation)CY 3 Start of visibility window at Canberra (5 deg elevation)CZ 1 End of visibility window at Canberra (5 deg elevation)CZ 2 End of visibility window at Canberra (5 deg elevation)CZ 3 End of visibility window at Canberra (5 deg elevation)CZ 4 End of visibility window at Canberra (5 deg elevation)DY 1 Start of visibility window at Vilspa (5 deg elevation)DY 2 Start of visibility window at Vilspa (5 deg elevation)DY 3 Start of visibility window at Vilspa (5 deg elevation)DZ 1 End of visibility window at Vilspa (5 deg elevation)DZ 2 End of visibility window at Vilspa (5 deg elevation)DZ 3 End of visibility window at Vilspa (5 deg elevation)GY 1 Start of visibility window at Goldstone (5 deg elevation)GY 2 Start of visibility window at Goldstone (5 deg elevation)GY 3 Start of visibility window at Goldstone (5 deg elevation)GY 4 Start of visibility window at Goldstone (5 deg elevation)GZ 1 End of visibility window at Goldstone (5 deg elevation)GZ 2 End of visibility window at Goldstone (5 deg elevation)GZ 3 End of visibility window at Goldstone (5 deg elevation)JY 1 Start of visibility window at Maspalomas (5 deg elevation)JY 2 Start of visibility window at Maspalomas (5 deg elevation)JY 3 Start of visibility window at Maspalomas (5 deg elevation)JY 4 Start of visibility window at Maspalomas (5 deg elevation)JZ 1 End of visibility window at Maspalomas (5 deg elevation)JZ 2 End of visibility window at Maspalomas (5 deg elevation)JZ 3 End of visibility window at Maspalomas (5 deg elevation)KA 1 Start of visibility window at Kourou (5 deg elevation)KA 2 Start of visibility window at Kourou (5 deg elevation)KA 3 Start of visibility window at Kourou (5 deg elevation)KA 4 Start of visibility window at Kourou (5 deg elevation)KL 1 End of visibility window at Kourou (5 deg elevation)KL 2 End of visibility window at Kourou (5 deg elevation)KL 3 End of visibility window at Kourou (5 deg elevation)KL 4 End of visibility window at Kourou (5 deg elevation)MY 1 Start of visibility window at Madrid (5 deg elevation)MY 2 Start of visibility window at Madrid (5 deg elevation)MY 3 Start of visibility window at Madrid (5 deg elevation)MY 4 Start of visibility window at Madrid (5 deg elevation)MZ 1 End of visibility window at Madrid (5 deg elevation)MZ 2 End of visibility window at Madrid (5 deg elevation)MZ 3 End of visibility window at Madrid (5 deg elevation)NS S Southbound neutral sheetNT I Enter north tail lobe from inner magnetospherePA 1 Start of visibility window at Perth (5 deg elevation)PA 2 Start of visibility window at Perth (5 deg elevation)PA 3 Start of visibility window at Perth (5 deg elevation)PE _ PerigeePL 1 End of visibility window at Perth (5 deg elevation)PL 2 End of visibility window at Perth (5 deg elevation)PL 3 End of visibility window at Perth (5 deg elevation)PL 4 End of visibility window at Perth (5 deg elevation)QL I Inbound critical L value for auroral zoneQL O Outbound critical L value for auroral zoneRA 1 Start of visibility window at Redu (5 deg elevation)RA 2 Start of visibility window at Redu (5 deg elevation)RA 3 Start of visibility window at Redu (5 deg elevation)RA 4 Start of visibility window at Redu (5 deg elevation)RL 1 End of visibility window at Redu (5 deg elevation)RL 2 End of visibility window at Redu (5 deg elevation)RL 3 End of visibility window at Redu (5 deg elevation)ST O Leave south tail lobe for inner magnetosphereTL I Inbound radiation belt entry for WECTL O Outbound radiation belt exit for WECVL I Inbound critical L value for EDIVL O Outbound critical L value for EDIWL I Inbound critical L value for ASPOCWL O Outbound critical L value for ASPOCXL I Inbound critical L value for PEACEXL O Outbound critical L value for PEACEYL I Inbound critical L value for RAPIDYL O Outbound critical L value for RAPIDZL I Inbound critical L value for CISZL O Outbound critical L value for CIS

Counts based on variable 'Epoch__C3_JP_PSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/jp/pse/2000/c3_jp_pse_20000801_v06.cdf. The most common cadence, 1 [ms] = PT0.001S, occurred for 10.9489% of the 30 timesteps. 

Introduction to the Active Spacecraft Potential Control (ASPOC) on Cluster II Samba

Counts based on variable 'Epoch__C3_PP_ASP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/pp/asp/2000/c3_pp_asp_20001209_v01.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 99.9815% of the 21573 timesteps. 

NSSDC Master Catalog listing for Cluster II Samba Cluster Ion Spectrometry (CIS)

This site provides information concerning the Cluster II Samba Cluster Ion Spectrometry Instrument.

Counts based on variable 'Epoch__C3_PP_CIS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/pp/cis/2000/c3_pp_cis_20001209_v01.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 32.4248% of the 3224 timesteps. 

NSSDC Master Catalog listing for the Cluster II Samba Electron Drift Instrument (EDI)

This site provides information concerning the Cluster II Samba Electron Drift Instrument.

NSSDC Master Catalog listing for Cluster II Samba Electric Field and Waves (EFW)

This site provides information concerning the Cluster II Samba Electric Field and Waves Instrument.

Counts based on variable 'Epoch__C3_PP_EFW' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/pp/efw/2024/c3_pp_efw_20240531_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9815% of the 21582 timesteps. 

NSSDC Master Catalog listing for Cluster II Samba Plasma Electron and Current Experiment (PEACE)

This site provides information concerning the Cluster II Samba Plasma Electron and Current Experiment Instrument.

NSSDC Master Catalog listing for Cluster II Samba Research with Adaptive Particle Imaging Detectors (RAPID)

This site provides information concerning the Cluster II Samba Research with Adaptive Particle Imaging Detectors Instrument.

Counts based on variable 'Epoch__C3_PP_RAP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/pp/rap/2000/c3_pp_rap_20001209_v01.cdf. The most common cadence, 4004 [ms] = PT4.004S, occurred for 90.6667% of the 9044 timesteps. 

NSSDC Master Catalog listing for Cluster II Samba Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF)

This site provides information concerning the Cluster II Samba Spatio-Temporal Analysis of Magnetic Field Fluctuations Instrument.

Counts based on variable 'Epoch__C3_PP_STA' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/pp/sta/2000/c3_pp_sta_20001209_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 78.7385% of the 7777 timesteps. 

NSSDC Master Catalog listing for Cluster II Samba Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER)

This site provides information concerning the Cluster II Samba Waves of HF and Sounder for Probing Electron Density by Relaxation Instrument.

Counts based on variable 'Epoch__C3_PP_WHI' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/pp/whi/2000/c3_pp_whi_20001210_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9731% of the 11129 timesteps. 

Cluster Spacecraft 3, FluxGate Magnetometer (FGM) Unvalidated Prime Parameters

NSSDC Master Catalog listing for Cluster II Samba Fluxgate Magnetometer (FGM)

This site provides information concerning the Cluster II Samba Fluxgate Magnetometer Instrument.

Counts based on variable 'Epoch__C3_UP_FGM' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/up/fgm/2019/c3_up_fgm_20190201_v01.cdf. The most common cadence, 4230 [ms] = PT4.23S, occurred for 86.5277% of the 17598 timesteps. 

High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor.  The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system....CALIBRATION:...The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'cluster_wbd_calibration.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255.  Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number....CONVERSION TO FREQUENCY DOMAIN:...In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out:  1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any....Bandwidth   Sample Rate---------   ------------9.5 kHz      27.443 kHz 19 kHz       54.886 kHz 77 kHz      219.544 kHz ...COORDINATE SYSTEM USED:...One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane....

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/wbd/2001/01/c3_waveform_wbd_200101041500_v01.cdf. The most common cadence, 36439103 [ps] = PT0.000036439S, occurred for 83.8669% of the 8362262 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c3/wbd_bm2/2000/10/c3_waveform_wbd_bm2_200010120000_v01.cdf. The most common cadence, 18219552 [ps] = PT0.000018220S, occurred for 31.3848% of the 683846 timesteps. 

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_H1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_omni/2001/c4_cp_cis-codif_h1_1d_pef_20010109_v20151107.cdf. The most common cadence, 12026 [ms] = PT12.026S, occurred for 16.7293% of the 356 timesteps. 

Cluster Satellite No 4 (from all.xml/observatory/description/@short)

Cluster Satellite No 4 (from Master/CDFglobalAttributes/Source_name)

CIS-CODIF 1D Helium+ distributions on C4 in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_He1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_omni/2001/c4_cp_cis-codif_he1_1d_pef_20010109_v20151108.cdf. The most common cadence, 64112 [ms] = PT1M4.112S, occurred for 15.5172% of the 81 timesteps. 

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_He1_DENSITY_CORRECTED' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_density/2001/c4_cp_cis-codif_he1_density_corrected_20010301_v20111208.cdf. The most common cadence, 32088 [ms] = PT32.088S, occurred for 27.2727% of the 3 timesteps. 

CIS-CODIF 3D Proton distributions on C4, High-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_H1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_3ddist_highsens_diffenergyflux/2001/c4_cp_cis-codif_hs_h1_pef_20010109_v20151106.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 22.6667% of the 34 timesteps. 

CIS-CODIF 3D Proton distributions on C4, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_3ddist_highsens_diffparticleflux/2001/c4_cp_cis-codif_hs_h1_pf_20010109_v20151106.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 22.6667% of the 34 timesteps. 

CIS-CODIF 3D Proton distributions on C4, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_H1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_3ddist_highsens_phasespacedens/2001/c4_cp_cis-codif_hs_h1_psd_20010109_v20151107.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 22.6667% of the 34 timesteps. 

CIS-CODIF 3D Helium+ distributions on C4, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_3ddist_highsens_diffparticleflux/2001/c4_cp_cis-codif_hs_he1_pf_20010109_v20151107.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 28.3784% of the 42 timesteps. 

CIS-CODIF 3D Helium+ distributions on C4, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_He1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_3ddist_highsens_phasespacedens/2001/c4_cp_cis-codif_hs_he1_psd_20010109_v20151108.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 28.3784% of the 42 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C4, High-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_O1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_3ddist_highsens_diffenergyflux/2001/c4_cp_cis-codif_hs_o1_pef_20010109_v20151029.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 23.7500% of the 38 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C4, High-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_3ddist_highsens_diffparticleflux/2001/c4_cp_cis-codif_hs_o1_pf_20010109_v20151110.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 23.7500% of the 38 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C4, High-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_HS_O1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_3ddist_highsens_phasespacedens/2001/c4_cp_cis-codif_hs_o1_psd_20010109_v20151111.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 23.7500% of the 38 timesteps. 

CIS-CODIF 3D Proton distributions on C4, Low-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_H1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_3ddist_lowsens_diffenergyflux/2001/c4_cp_cis-codif_ls_h1_pef_20010109_v20151111.cdf. The most common cadence, 12026 [ms] = PT12.026S, occurred for 18.0071% of the 356 timesteps. 

CIS-CODIF 3D Proton distributions on C4, Low-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_3ddist_lowsens_diffparticleflux/2001/c4_cp_cis-codif_ls_h1_pf_20010109_v20151117.cdf. The most common cadence, 12026 [ms] = PT12.026S, occurred for 18.0071% of the 356 timesteps. 

CIS-CODIF 3D Proton distributions on C4, Low-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_H1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_3ddist_lowsens_phasespacedens/2001/c4_cp_cis-codif_ls_h1_psd_20010109_v20151117.cdf. The most common cadence, 12026 [ms] = PT12.026S, occurred for 18.0071% of the 356 timesteps. 

CIS-CODIF 3D Helium+ distributions on C4, Low-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_He1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_3ddist_lowsens_diffenergyflux/2001/c4_cp_cis-codif_ls_he1_pef_20010109_v20151111.cdf. The most common cadence, 64112 [ms] = PT1M4.112S, occurred for 21.7158% of the 81 timesteps. 

CIS-CODIF 3D Helium+ distributions on C4, Low-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_3ddist_lowsens_diffparticleflux/2001/c4_cp_cis-codif_ls_he1_pf_20010109_v20151118.cdf. The most common cadence, 64112 [ms] = PT1M4.112S, occurred for 21.7158% of the 81 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C4, Low-Sensitivity, in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_O1_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_3ddist_lowsens_diffenergyflux/2001/c4_cp_cis-codif_ls_o1_pef_20010109_v20151120.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 19.0866% of the 280 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C4, Low-Sensitivity, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_3ddist_lowsens_diffparticleflux/2001/c4_cp_cis-codif_ls_o1_pf_20010109_v20151119.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 19.0866% of the 280 timesteps. 

CIS-CODIF 3D Oxygen+ distributions on C4, Low-Sensitivity, in Phase_Space_Density

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_LS_O1_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_3ddist_lowsens_phasespacedens/2001/c4_cp_cis-codif_ls_o1_psd_20010109_v20151120.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 19.0866% of the 280 timesteps. 

CIS-CODIF 1D Oxygen+ distributions on C4 in Particle_Energy_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_O1_1D_PEF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_omni/2004/c4_cp_cis-codif_o1_1d_pef_20040507_v20151110.cdf. The most common cadence, 7934 [ms] = PT7.934S, occurred for 16.1000% of the 393 timesteps. 

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_PAD_HS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_pitchangle_highsens_diffparticleflux/2001/c4_cp_cis-codif_pad_hs_h1_pf_20010131_v20220812.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 24.3655% of the 48 timesteps. 

CIS-CODIF Helium+ Pitch-Angle Distribution, High-sensitivity side, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_PAD_HS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_pitchangle_highsens_diffparticleflux/2001/c4_cp_cis-codif_pad_hs_he1_pf_20010131_v20220812.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 30.1508% of the 60 timesteps. 

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_PAD_HS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_pitchangle_highsens_diffparticleflux/2001/c4_cp_cis-codif_pad_hs_o1_pf_20010131_v20220812.cdf. The most common cadence, 16036 [ms] = PT16.036S, occurred for 28.7736% of the 61 timesteps. 

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_PAD_LS_H1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/proton_pitchangle_lowsens_diffparticleflux/2001/c4_cp_cis-codif_pad_ls_h1_pf_20010131_v20220812.cdf. The most common cadence, 4009 [ms] = PT4.009S, occurred for 18.3311% of the 1474 timesteps. 

CIS-CODIF Helium+ Pitch-Angle Distribution, Low-sensitivity side, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_PAD_LS_He1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/heplus_pitchangle_lowsens_diffparticleflux/2001/c4_cp_cis-codif_pad_ls_he1_pf_20010131_v20130308.cdf. The most common cadence, 4009 [ms] = PT4.009S, occurred for 28.0252% of the 1510 timesteps. 

CIS-CODIF Oxygen+ Pitch-Angle Distribution, Low-sensitivity side, in Differential_Particle_Flux

Counts based on variable 'time_tags__C4_CP_CIS_CODIF_PAD_LS_O1_PF' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cis-codif/oplus_pitchangle_lowsens_diffparticleflux/2001/c4_cp_cis-codif_pad_ls_o1_pf_20010131_v20130308.cdf. The most common cadence, 4009 [ms] = PT4.009S, occurred for 23.8284% of the 1500 timesteps. 

Counts based on variable 'time_tags__C4_CP_EFW_L3_E3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/efw/efield_3dvect_spinreso_l3_inertialframe/2001/c4_cp_efw_l3_e3d_inert_20010107_v20230714.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 99.9942% of the 17188 timesteps. 

Counts based on variable 'time_tags__C4_CP_EFW_L3_P' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/efw/scpotential_spinreso_l3/2000/c4_cp_efw_l3_p_20001201_v20221111.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 99.9559% of the 6804 timesteps. 

Counts based on variable 'time_tags__C4_CP_EFW_L3_V3D_INERT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/efw/driftvelo_3dvect_spinreso_l3_inertialframe/2001/c4_cp_efw_l3_v3d_inert_20010107_v20230714.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 99.9942% of the 17188 timesteps. 

Counts based on variable 'time_tags__C4_CP_FGM_5VPS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/fgm/mfield_3dvect_5vectpersec/2001/c4_cp_fgm_5vps_20010107_v20140305.cdf. The most common cadence, 200 [ms] = PT0.2S, occurred for 99.9991% of the 347538 timesteps. 

Cluster Spacecraft 4 FluxGate Magnetometer (FGM) Spin-Resolution Parameters

Counts based on variable 'time_tags__C4_CP_FGM_SPIN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/cp/2001/c4_cp_fgm_spin_20010131_v01.cdf. The most common cadence, 4008 [ms] = PT4.008S, occurred for 58.9082% of the 12518 timesteps. 

Cluster spacecraft 4 (from all.xml/observatory/description/@short)

Cluster spacecraft 4 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Time_tags__C4_CP_RAP_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-ies/electron_3ddist_bestreso/2000/c4_cp_rap_e3dd_20001211_v20230309.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 62.2378% of the 1068 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_ESPCT6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-ies/electron_omni_spinreso/2000/c4_cp_rap_espct6_20001205_v20230309.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 86.0963% of the 161 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_HSPCT' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/proton_omni_spinreso/2000/c4_cp_rap_hspct_20001207_v20230309.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 73.4739% of the 11049 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_I3DM_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/cno_3ddist_stdreso/2000/c4_cp_rap_i3dm_cno_20001207_v20230309.cdf. The most common cadence, 128197 [ms] = PT2M8.197S, occurred for 46.3519% of the 216 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_I3DM_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/proton_3ddist_stdreso/2000/c4_cp_rap_i3dm_h_20001207_v20230309.cdf. The most common cadence, 128197 [ms] = PT2M8.197S, occurred for 46.3519% of the 216 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_I3DM_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/he_3ddist_stdreso/2000/c4_cp_rap_i3dm_he_20001207_v20230309.cdf. The most common cadence, 128197 [ms] = PT2M8.197S, occurred for 46.3519% of the 216 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_ISPCT_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/cno_omni_spinreso/2000/c4_cp_rap_ispct_cno_20001207_v20230309.cdf. The most common cadence, 32049 [ms] = PT32.049S, occurred for 69.8711% of the 1301 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_ISPCT_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/he_omni_spinreso/2000/c4_cp_rap_ispct_he_20001207_v20230309.cdf. The most common cadence, 32049 [ms] = PT32.049S, occurred for 69.8711% of the 1301 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-ies/electron_3ddist_2echannels_stdreso/2004/c4_cp_rap_l3dd_20040503_v20210208.cdf. The most common cadence, 3960 [ms] = PT3.96S, occurred for 76.7113% of the 975 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_PAD_CNO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/cno_pitchangle_stdreso/2001/c4_cp_rap_pad_cno_20010109_v20230309.cdf. The most common cadence, 128226 [ms] = PT2M8.226S, occurred for 47.0339% of the 111 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_PAD_E3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-ies/electron_pitchangle_bestreso/2001/c4_cp_rap_pad_e3dd_20010112_v20230309.cdf. The most common cadence, 4007 [ms] = PT4.007S, occurred for 79.4996% of the 2129 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_PAD_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/proton_pitchangle_stdreso/2001/c4_cp_rap_pad_h_20010109_v20230309.cdf. The most common cadence, 128226 [ms] = PT2M8.226S, occurred for 47.0339% of the 111 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_PAD_He' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-iims/he_pitchangle_stdreso/2001/c4_cp_rap_pad_he_20010109_v20230309.cdf. The most common cadence, 128226 [ms] = PT2M8.226S, occurred for 47.0339% of the 111 timesteps. 

Counts based on variable 'Time_tags__C4_CP_RAP_PAD_L3DD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/rap-ies/electron_pitchangle_2echannels_stdreso/2004/c4_cp_rap_pad_l3dd_20040503_v20210208.cdf. The most common cadence, 3960 [ms] = PT3.96S, occurred for 76.6929% of the 974 timesteps. 

Counts based on variable 'Time__C4_CP_STA_CWF_GSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/sta/mfield_calibwaveform_gse/2000/c4_cp_sta_cwf_gse_20001023_v20220610.cdf. The most common cadence, 40000000000 [ps] = PT0.04S, occurred for 68.9755% of the 15007 timesteps. 

Counts based on variable 'Time__C4_CP_STA_PPP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/sta/polarization_propagation/2001/c4_cp_sta_ppp_20010107_v20160411.cdf. The most common cadence, 4000000000000 [ps] = PT4S, occurred for 92.5472% of the 15932 timesteps. 

Counts based on variable 'Time__C4_CP_STA_PSD' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/sta/powerspectraldensity/2000/c4_cp_sta_psd_20001023_v20220608.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for all 3 timesteps. 

Counts based on variable 'time_tags__C4_CP_WHI_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/whi/efield_spectralpowerdensity_soundingmode/2000/c4_cp_whi_active_20001025_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 40.6557% of the 124 timesteps. 

Counts based on variable 'time_tags__C4_CP_WHI_ELECTRON_DENSITY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/whi/electron_density/2001/c4_cp_whi_electron_density_20010207_v20160311.cdf. The most common cadence, 2560 [ms] = PT2.56S, occurred for 21.2145% of the 2690 timesteps. 

Counts based on variable 'time_tags__C4_CP_WHI_NATURAL' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/whi/efield_spectralpowerdensity_naturalmode/2000/c4_cp_whi_natural_20001025_v20150715.cdf. The most common cadence, 856 [ms] = PT0.856S, occurred for 48.6486% of the 54 timesteps. 

Counts based on variable 'time_tags__C4_CP_WHI_PASSIVE_ACTIVE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/whi/efield_passivespectralpowerdensity_soundingmode/2000/c4_cp_whi_passive_active_20001025_v20150715.cdf. The most common cadence, 1440 [ms] = PT1.44S, occurred for 48.6275% of the 124 timesteps. 

Counts based on variable 'time_tags__C4_CP_WHI_WAVE_FORM_ENERGY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/whi/efield_integratedpowerdensity_naturalmode/2000/c4_cp_whi_wave_form_energy_20001025_v20150715.cdf. The most common cadence, 856 [ms] = PT0.856S, occurred for 56.8421% of the 54 timesteps. 

Counts based on variable 'Epoch__C4_JP_PMP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/jp/pmp/2000/c4_jp_pmp_20000814_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 4936 timesteps. 

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)AP _ ApogeeCY 1 Start of visibility window at Canberra (5 deg elevation)CY 2 Start of visibility window at Canberra (5 deg elevation)CY 3 Start of visibility window at Canberra (5 deg elevation)CZ 1 End of visibility window at Canberra (5 deg elevation)CZ 2 End of visibility window at Canberra (5 deg elevation)CZ 3 End of visibility window at Canberra (5 deg elevation)CZ 4 End of visibility window at Canberra (5 deg elevation)DY 1 Start of visibility window at Vilspa (5 deg elevation)DY 2 Start of visibility window at Vilspa (5 deg elevation)DY 3 Start of visibility window at Vilspa (5 deg elevation)DY 4 Start of visibility window at Vilspa (5 deg elevation)DZ 1 End of visibility window at Vilspa (5 deg elevation)DZ 2 End of visibility window at Vilspa (5 deg elevation)DZ 3 End of visibility window at Vilspa (5 deg elevation)GY 1 Start of visibility window at Goldstone (5 deg elevation)GY 2 Start of visibility window at Goldstone (5 deg elevation)GY 3 Start of visibility window at Goldstone (5 deg elevation)GY 4 Start of visibility window at Goldstone (5 deg elevation)GZ 1 End of visibility window at Goldstone (5 deg elevation)GZ 2 End of visibility window at Goldstone (5 deg elevation)GZ 3 End of visibility window at Goldstone (5 deg elevation)JY 1 Start of visibility window at Maspalomas (5 deg elevation)JY 2 Start of visibility window at Maspalomas (5 deg elevation)JY 3 Start of visibility window at Maspalomas (5 deg elevation)JY 4 Start of visibility window at Maspalomas (5 deg elevation)JZ 1 End of visibility window at Maspalomas (5 deg elevation)JZ 2 End of visibility window at Maspalomas (5 deg elevation)JZ 3 End of visibility window at Maspalomas (5 deg elevation)KA 1 Start of visibility window at Kourou (5 deg elevation)KA 2 Start of visibility window at Kourou (5 deg elevation)KA 3 Start of visibility window at Kourou (5 deg elevation)KA 4 Start of visibility window at Kourou (5 deg elevation)KL 1 End of visibility window at Kourou (5 deg elevation)KL 2 End of visibility window at Kourou (5 deg elevation)KL 3 End of visibility window at Kourou (5 deg elevation)KL 4 End of visibility window at Kourou (5 deg elevation)MY 1 Start of visibility window at Madrid (5 deg elevation)MY 2 Start of visibility window at Madrid (5 deg elevation)MY 3 Start of visibility window at Madrid (5 deg elevation)MY 4 Start of visibility window at Madrid (5 deg elevation)MZ 1 End of visibility window at Madrid (5 deg elevation)MZ 2 End of visibility window at Madrid (5 deg elevation)MZ 3 End of visibility window at Madrid (5 deg elevation)NS S Southbound neutral sheetNT I Enter north tail lobe from inner magnetospherePA 1 Start of visibility window at Perth (5 deg elevation)PA 2 Start of visibility window at Perth (5 deg elevation)PA 3 Start of visibility window at Perth (5 deg elevation)PA 4 Start of visibility window at Perth (5 deg elevation)PE _ PerigeePL 1 End of visibility window at Perth (5 deg elevation)PL 2 End of visibility window at Perth (5 deg elevation)PL 3 End of visibility window at Perth (5 deg elevation)PL 4 End of visibility window at Perth (5 deg elevation)PL 5 End of visibility window at Perth (5 deg elevation)QL I Inbound critical L value for auroral zoneQL O Outbound critical L value for auroral zoneRA 1 Start of visibility window at Redu (5 deg elevation)RA 2 Start of visibility window at Redu (5 deg elevation)RA 3 Start of visibility window at Redu (5 deg elevation)RL 1 End of visibility window at Redu (5 deg elevation)RL 2 End of visibility window at Redu (5 deg elevation)RL 3 End of visibility window at Redu (5 deg elevation)ST O Leave south tail lobe for inner magnetosphereTL I Inbound radiation belt entry for WECTL O Outbound radiation belt exit for WECVL I Inbound critical L value for EDIVL O Outbound critical L value for EDIWL B Outbound critical L value 2 for ASPOCWL I Inbound critical L value for ASPOCWL O Outbound critical L value for ASPOCXL I Inbound critical L value for PEACEXL O Outbound critical L value for PEACEYL I Inbound critical L value for RAPIDYL O Outbound critical L value for RAPIDZL I Inbound critical L value for CISZL O Outbound critical L value for CIS

Counts based on variable 'Epoch__C4_JP_PSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/jp/pse/2000/c4_jp_pse_20000801_v06.cdf. The most common cadence, 1 [ms] = PT0.001S, occurred for 10.9489% of the 30 timesteps. 

Introduction to the Active Spacecraft Potential Control (ASPOC) on Cluster II Tango

Counts based on variable 'Epoch__C4_PP_ASP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/asp/2000/c4_pp_asp_20001209_v01.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 99.9674% of the 21474 timesteps. 

NSSDC Master Catalog listing for Cluster II Tango Cluster Ion Spectrometry (CIS)

This site provides information concerning the Cluster II Tango Cluster Ion Spectrometry Instrument.

Counts based on variable 'Epoch__C4_PP_CIS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/cis/2000/c4_pp_cis_20001209_v01.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 28.4906% of the 2569 timesteps. 

Information about the Digital Wave Processor (DWP) experiment on the Cluster 2/FM5 (Tango) mission.

Counts based on variable 'Epoch__C4_PP_DWP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/dwp/2000/c4_pp_dwp_20001101_v01.cdf. The most common cadence, 4445 [ms] = PT4.445S, occurred for 73.1769% of the 14189 timesteps. 

NSSDC Master Catalog listing for the Cluster II Tango Electron Drift Instrument (EDI)

This site provides information concerning the Cluster II Tango Electron Drift Instrument.

NSSDC Master Catalog listing for Cluster II Tango Electric Field and Waves (EFW)

This site provides information concerning the Cluster II Tango Electric Field and Waves Instrument.

Counts based on variable 'Epoch__C4_PP_EFW' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/efw/2024/c4_pp_efw_20240531_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9768% of the 21578 timesteps. 

NSSDC Master Catalog listing for Cluster II Tango Plasma Electron and Current Experiment (PEACE)

This site provides information concerning the Cluster II Tango Plasma Electron and Current Experiment Instrument.

NSSDC Master Catalog listing for Cluster II Tango Research with Adaptive Particle Imaging Detectors (RAPID)

This site provides information concerning the Cluster II Tango Research with Adaptive Particle Imaging Detectors Instrument.

Counts based on variable 'Epoch__C4_PP_RAP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/rap/2000/c4_pp_rap_20001209_v01.cdf. The most common cadence, 4006 [ms] = PT4.006S, occurred for 74.6933% of the 7367 timesteps. 

NSSDC Master Catalog listing for Cluster II Tango Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF)

This site provides information concerning the Cluster II Tango Spatio-Temporal Analysis of Magnetic Field Fluctuations Instrument.

Counts based on variable 'Epoch__C4_PP_STA' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/sta/2000/c4_pp_sta_20001209_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 79.2464% of the 7740 timesteps. 

NSSDC Master Catalog listing for Cluster II Tango Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER)

This site provides information concerning the Cluster II Tango Waves of HF and Sounder for Probing Electron Density by Relaxation Instrument.

Counts based on variable 'Epoch__C4_PP_WHI' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/pp/whi/2000/c4_pp_whi_20001210_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 99.9920% of the 12476 timesteps. 

Cluster Spacecraft 4, FluxGate Magnetometer (FGM) Unvalidated Prime Parameters

NSSDC Master Catalog listing for Cluster II Tango Fluxgate Magnetometer (FGM)

This site provides information concerning the Cluster II Tango Fluxgate Magnetometer Instrument.

Counts based on variable 'Epoch__C4_UP_FGM' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/up/fgm/2019/c4_up_fgm_20190201_v01.cdf. The most common cadence, 4155 [ms] = PT4.155S, occurred for 57.6418% of the 11933 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/wbd/2001/01/c4_waveform_wbd_200101041450_v01.cdf. The most common cadence, 36439103 [ps] = PT0.000036439S, occurred for 74.9194% of the 4120226 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/c4/wbd_bm2/2000/10/c4_waveform_wbd_bm2_200010252320_v01.cdf. The most common cadence, 4554888 [ps] = PT0.000004555S, occurred for 52.6975% of the 2857653 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cassini/helio1day/cassini_helio1day_position_19971016_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 7273 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cassini/helio1hr/cassini_helio1hr_position_19971016_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 174575 timesteps. 

Cassini magnetic-field 1 minute averages for the year 2020 in RTN  coordinates. RTN coordinates consist of R (radial component, Sun tothe spacecraft), T (tangential component, parallel to the Solar    Equatorial plane and perpendicular to R), and N (normal component, completes right handed set).This file contains a subset of all of the Cassini MAG data for 2001consisting of only the data after the day of the last Jupiter      bowshock crossing (2001-01-15).This file was produced from raw (L1A) data at the PDS/PPI node usingsoftware provided by the Cassini MAG team, and employing the latest calibration available. The MAG team reports that while range-0 data are well calibrated, higher range data needs improvement (see the   RANGE_CHANGES.ASC document for a time history of range changes). Thesedata will be replaced as the calibration is improved." The data are mostly from the fluxgate magnetometer (FGM). The tableat vhm.txt identifies the 52 days in 2000-2004 for which the data are solely from the vector helium magnetometer (VHM).  Days not in the table contain only FGM data.VHM_mode variable indicates (value 1) whether data are from VHMThe data were produced from raw (L1A) data at the PDS/PPI node using software provided by the Cassini MAG team, and employing the latest calibration available.  PDS/PPI produced both 1-sec vectors and 1-min averages.  The MAG team reports that while range-0 data are well calibrated for both FGM and VHM, higher range data need improvement.  FGM_mode variable indicates (value 0) if data is range-0.Seehttp://www.igpp.ucla.edu/cgi-bin/ditdos?volume=COMAG_0XXX&folder=DOCUMENT/DATA_QUALITY&file=RANGE_CHANGESfor details.  In particular, this documentation reports that FGM wasin range=0 for the following extended intervals (plus other brief intervals):1999/230/05 - 1999/245/07 (YYYY/DDD/HH, inclusive)1999/245/09 - 2000/037/122000/039/00 - 2000/053/182000/053/20 - 2000/056/012000/057/23 - 2002/334/132002/334/17 - 2003/292/182003/292/22 - 2004/046/112004/046/15 - 2004/088/082004/088/12 - 2004/136/062004/136/11 - 2004/174/012004/174/06 - 2004/182/17

SPDF/CDAWeb. Please also acknowledge the data producer: Michele Dougherty at Imperial College, London

SPDF/SSCWeb. Please also acknowledge the data producer: Michele Dougherty at Imperial College, London

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Michele Dougherty at Imperial College, London

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cassini/mag_1min/cdf/cassini_mag_1min_magnetic_field_20000101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.6737% of the 240091 timesteps. 

MAG - Dual Technique Magnetometer (from all.xml/instrument/description/@short)

Cassini 1-min Magnetic Field (from Master/CDFglobalAttributes/Data_type)

Colorado Inner Radiation Belt Experiment, Relativistic Electron Proton Telescope integrated little experiment-2, Level 1A Data Product, Detectors

CIRBE is a 3U-CubeSat designed and developed by students and engineers at the Laboratory for Atmospheric and Space Physics.The primary objective of the science mission is to understand the formation of the inner belt (L<2) electrons (100s of keV to multiple MeV), and to determine the source, the intensity and dynamic variations of these electrons.The goal is to make accurate measurements with fine energy resolution (>40 channels) for electrons of 0.3-3 MeV throughout the slot region and inner belt, with secondary measurements of 6.7-35 MeV protons.Such measurements are required to address the following science questions:1) Where is the break point in terms of energy of electrons for a given event, below which electrons can be transported into the inner belt from the outer belt but above which electrons cannot, and what is the injection mechanism?2) What is the CRAND contribution to inner belt electrons, and what is the low energy neutron density near Earth?3) What is the role of wave-particle interactions in shaping inner-belt electron energy spectra?A detailed description of the instrument can be found at https://doi.org/10.1029/2021JA030249.We acknowledge the use of the IRBEM library (4.4.0) to process the data, the latest version of which can be found at https://doi.org/10.5281/zenodo.6867552.

The CIRBE/REPTile-2 data are available for science research. Users should contact the PI, professor Xinlin Li, to discuss the possible issues and appropriate applications of these data. Users publishing results should provide appropriate acknowledgement and should provide the version number of the data being used.

SPDF/CDAWeb. Please also acknowledge the data producer: Xinlin Li at University of Colorado at Boulder

SPDF/SSCWeb. Please also acknowledge the data producer: Xinlin Li at University of Colorado at Boulder

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Xinlin Li at University of Colorado at Boulder

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_2.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_2.)

Colorado Inner Radiation Belt Experiment (from all.xml/observatory/description/@short)

Relativistic Electron Proton Telescope integrated little experiment-2 (from all.xml/instrument/description/@short)

Colorado Inner Radiation Belt Experiment (from Master/CDFglobalAttributes/Source_name)

Level 1A Data Product (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cirbe/reptile-2/l1a_detector_counts/2023/cirbe_reptile-2_l1a_detectors_20230419_v01_01.cdf. The most common cadence, 999 [ms] = PT0.999S, occurred for 22.1254% of the 254 timesteps.

Countrate of Events that Trigger the First Detector but Not the Second

Count of Events that Trigger the First Detector but Not the Second

Countrate of Events that Trigger the First Two Detectors but Not the Third

Count of Events that Trigger the First Two Detectors but Not the Third

Countrate of Events that Trigger the First Three Detectors but Not the Fourth

Count of Events that Trigger the First Three Detectors but Not the Fourth

Counts based on variable 'Epoch_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cirbe/reptile-2/l1a_detector_counts/2023/cirbe_reptile-2_l1a_detectors_20230419_v01_01.cdf. The most common cadence, 16001 [ms] = PT16.001S, occurred for 24.4898% of the 48 timesteps.

Colorado Inner Radiation Belt Experiment, Relativistic Electron Proton Telescope integrated little experiment-2, Level 1B Data Product, Range Electrons

Level 1B Data Product (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cirbe/reptile-2/l1b_counts_range_electrons/2023/cirbe_reptile-2_l1b_rng_elecs_20230419_v01_01.cdf. The most common cadence, 999 [ms] = PT0.999S, occurred for 22.1254% of the 254 timesteps.

Counts based on variable 'Epoch_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cirbe/reptile-2/l1b_counts_range_electrons/2023/cirbe_reptile-2_l1b_rng_elecs_20230419_v01_01.cdf. The most common cadence, 16001 [ms] = PT16.001S, occurred for 24.4898% of the 48 timesteps.

Colorado Inner Radiation Belt Experiment, Relativistic Electron-Proton Telescope integrated little experiment-2, Level 2 Data Product, Range Electrons

Level 2 Data Product (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cirbe/reptile-2/l2_flux_range_electrons/2023/cirbe_reptile-2_l2_rng_elecs_20230419_v01_01.cdf. The most common cadence, 999 [ms] = PT0.999S, occurred for 22.1254% of the 254 timesteps.

FEDU: Directional Differential Electron Flux 0.3-5.83 MeV, in 50 energy bands

Counts based on variable 'Epoch_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cirbe/reptile-2/l2_flux_range_electrons/2023/cirbe_reptile-2_l2_rng_elecs_20230419_v01_01.cdf. The most common cadence, 16001 [ms] = PT16.001S, occurred for 24.4898% of the 48 timesteps.

Lunar Environment Heliophysics X-ray Imager (LEXI) Level 1c photon event data

The lunar environment heliophysics X-ray imager (LEXI) mission.BM Walsh, et al., Space Sci. Rev., 2024https://doi.org/10.1007/s11214-024-01063-4

SPDF/CDAWeb. Please also acknowledge the data producer: B. Walsh at Boston U.

SPDF/SSCWeb. Please also acknowledge the data producer: B. Walsh at Boston U.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: B. Walsh at Boston U.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lexi/photons/2025/clps-bgm1_lexi_l1c-photons_2025031619_v01.cdf. The most common cadence, 25000 [ns] = PT0.000025000S, occurred for 17.6190% of the 273923 timesteps.

Blue Ghost Mission 1 (from all.xml/observatory/description/@short)

Lunar Environment Heliospheric X-ray Imager (from all.xml/instrument/description/@short)

Blue Ghost Mission 1 (from Master/CDFglobalAttributes/Source_name)

Right Ascension angle of measured photon in J2000 frame centered on LEXI, scalar.

Declination angle of measured photon in J2000 frame centered on LEXI, scalar.

Azimuth angle of the measured photon in the local topocentric frame, scalar.

Elevation angle of the measured photon in the local topocentric frame, scalar.

Counts per second as observed by LEXI in its field of view, scalar

Lunar Environment Heliophysics X-ray Imager (LEXI) Level 2 image data

LEXI counts per (RA, Dec) pixel per second, background subtracted.

Cluster and Double Star Science Archive, Access to High Resolution Cluster Data

Counts based on variable 'Epoch__CL_JP_PCY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/cl/jp/pcy/1999/cl_jp_pcy_19990101_v96.cdf. The most common cadence, 2678400000 [ms] = P31D, occurred for 58.1994% of the 181 timesteps. 

Predicted Solar Cycle Trends (from all.xml/instrument/description/@short)

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 1997For geometrical configuration parameters, p328 of Tetrahedron Geometric Factorsby P.Robert et al, in Analysis Methods for Multi-Spacecraft Data,ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency andthe International Space Institute, Bern.

Counts based on variable 'Epoch__CL_JP_PGP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/cl/jp/pgp/2000/cl_jp_pgp_20000814_v05.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 4936 timesteps. 

Predicted Geometric Positions (from all.xml/instrument/description/@short)

Position, Velocity and Attitude of Four Spacecraft in GSE Reference

SPDF/CDAWeb. Please also acknowledge the data producer: Hungarian Data Centre/M. Tatrallyay at KFKI

SPDF/SSCWeb. Please also acknowledge the data producer: Hungarian Data Centre/M. Tatrallyay at KFKI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Hungarian Data Centre/M. Tatrallyay at KFKI

Counts based on variable 'Epoch__CL_SP_AUX' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/cl/sp/aux/2024/cl_sp_aux_20240930_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

CNOFS CINDI IVM ion density, composition, temperature, and drift (0.5-sec)

 The Communications/Navigation Outage Forecasting System (C/NOFS) is a prototype operational system designed to monitor and forecast ionospheric scintillation in real-time and on a global scale. In the space-borne segment, C/NOFS will fly a system of proven sensors on-board a three-axis stabilized satellite to detect ionospheric scintillation. This will provide data for global, real-time specification, and 4 hour forecast capability.  C/NOFS is a joint effort between the DOD Space Test Program and AFRL (Air Force Research Laboratory). The space test program provides the spacecraft, launch vehicle, launch and first year on-orbit operations.  AFRL is responsible for the multi-instrument payload, payload integration  and test, model development, data center operations, and product generation and distribution. The C/NOFS payload consists of six instruments: the Planar Langmuir Probe (PLP) for measurements of plasma density, the Vector Electric Field Instrument (VEFI) for measurements of vector electric and magnetic fields, the Ion Velocity Meter (IVM) for measurements of plasma drift velocities and ion temperatures, the Neutral Wind Meter (NWM) for measurements of neutral winds, the C/NOFS Occultation Receiver for Ionospheric Sensing and Specification (CORISS) for remote sensing of the electron density vertical profile, the Coherent Electromagnetic Radio Tomography (CERTO) for measurements of ionospheric scintillation parameters. Both the Neutral Wind Meter (NWM) and the Ion Velocity Meter (IVM) are provided by NASA as the CINDI (Coupled Ion-Neutral Dynamics Investigation) payload, which was selected as an Explorer Mission of Opportunity. The goal of C/NOFS is to forecast scintillation three to six hours before its onset such that system operators will be able to plan in ways that will optimize mission command and control.The spacecraft will be launched into an orbit with perigee/apogee of 400/700 km, and an inclination of 13 degrees. Launch is currently planned for early 2006.Information about C/NOFS can be found at Air Force Research Laboratory page: http://www.kirtland.af.mil/shared/media/document/AFD-070404-094.pdf.The Coupled Ion-Neutral Dynamics Investigation (CINDI) payload is funded by NASA as an Explorer Mission of Opportunity. CINDI consists of two instruments: the Ion Velocity Meter (IVM) and the Neutral Wind Meter (NWM). The IVM instrument includes a ion drift meter and a retarding potential analyzer. IVM measure the ion drift vector, the ion temperature, and the major ion composition with a spatial resolution of about 4 km along the satellite track; the ion drift meter also provides vertical and horizontal ion drift components at 500 m resolution. The NWM consists of a cross track wind sensor and a ram wind sensor providing a direct measure of the neutral wind vector with a spatial resolution of about 8 km along the satellite track.

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Roderick A. Heelis at University of Texas, Dallas

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Roderick A. Heelis at University of Texas, Dallas

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Roderick A. Heelis at University of Texas, Dallas

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cnofs/cindi/ivm_500ms_cdf/2008/cnofs_cindi_ivm_500ms_20080802_v01.cdf. The most common cadence, 500 [ms] = PT0.5S, occurred for 71.3471% of the 122784 timesteps. 

Communications Navigation Outage Forecast System (from all.xml/observatory/description/@short)

Coupled Ion-Neutral Dynamics (from all.xml/instrument/description/@short)

Communications Navigation Outage Forecast System (from Master/CDFglobalAttributes/Source_name)

RPA data quality flag: 0=high 9=low (https://spdf.gsfc.nasa.gov/pub/data/cnofs/cindi/)

Drift Meter data quality flag for v_horz and v_vert (https://spdf.gsfc.nasa.gov/pub/data/cnofs/cindi/)

Ion velocity in s/c coordinates in m/s (offset and photoemissission corrected if possible) -------> v_ram

Variance (VAR) of ion velocity in s/c coordinates -------> VAR of v_ram in m/s

Offset flag (0 if offset corrected, 1 if non-offset data are used)

-------> n*10+q  q=quality flag (https://spdf.gsfc.nasa.gov/pub/data/cnofs/cindi/), n=number of points for averaging

Spacecraft position in Earth-centered inertial (ECI) coordinates in km -------> X

IGRF geomagnetic field in nT in spacecraft coordinates (SCC) -------> x

Spacecraft absolute velocity in spacecraft coordinates SSC (in inertial space) -------> x

Spacecraft relative velocity in spacecraft coordinates (to co-rotating atmosphere) -------> x

Unit vectors for magnetic coordinate system in s/c coordinates (SC) -------> U_zonal_SC_x

Planar Langmuir Probe 1-sec average Key Parameters (Ni, Ne, Te). The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY

The Planar Langmuir Probe on C/NOFS is a suite of 2 current measuring sensors mounted on the ram facing surface of the spacecraft.  The primary sensor is an Ion Trap (conceptually similar to RPAs flown on many other spacecraft) capable of measuring ion densities as low as 1 cm-3 with a 12 bit log electrometer.  The secondary senor is a swept bias planar Langmuir probe (Surface Probe) capable of measuring Ne, Te, and spacecraft potential.The ion number density is the one second average of the ion density sampled at either 32, 256, 512, or 1024 Hz (depending on the mode).The ion density standard deviation is the standard deviation of the samples used to produce the one second average number density.DeltaN/N is the detrened ion number density 1 second standard deviation divided by the mean 1 sec density.The electron density, electron temperature, and spacecraft potential are all derived from a least squares fit to the current-bias curve from the Surface Probe.The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY.Regestering your email will allow notification of updates.

The C/NOFS mission is supported by the Air Force Research Laboratory, the Department of Defense Space Test Program, the National Aeronautics and Space Administration (NASA), the Naval Research Laboratory, and the Aerospace Corporation.

We request that all presentation and publications using PLP data:1) be submitted to the PI for review prior to publication or presentation,  2) Include PI authorhip or acknowledgement, 3) Acknowledge AFRLs C/NOFS program, and 4) Acknowledge the SMC Space Development and Test Wing.  donald.hunton@us.af.mil, patrick.roddy@us.af.mil

SPDF/CDAWeb. Please also acknowledge the data producer: D. E. Hunton at Air Force Research Laboratory, Space Vehicles Directorate

SPDF/SSCWeb. Please also acknowledge the data producer: D. E. Hunton at Air Force Research Laboratory, Space Vehicles Directorate

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. E. Hunton at Air Force Research Laboratory, Space Vehicles Directorate

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cnofs/plp/plasma_1sec/2008/cnofs_plp_plasma_1sec_20081101_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 58.3699% of the 50431 timesteps. 

Communications/Navigation Outage Forecast System (from all.xml/observatory/description/@short)

Planar Langmuir Probe (from all.xml/instrument/description/@short)

Communications/Navigation Outage Forecast System (from Master/CDFglobalAttributes/Source_name)

Key Parameter, The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY. (from Master/CDFglobalAttributes/Data_type)

Ion density from Ion Trap [PRELIMINARY, for BROWSE PURPOSES ONLY]

Standard deviation (STD) of 1-sec ion density [PRELIMINARY, for BROWSE PURPOSES ONLY.

(STD of detrended Ni)/(mean of Ni) for 1-sec interval [PRELIMINARY, for BROWSE PURPOSES ONLY]

Electron density from Langmuir Probe [PRELIMINARY, for BROWSE PURPOSES ONLY.

Electron temperature from Langmuir Probe [PRELIMINARY, for BROWSE PURPOSES ONLY.

Spacecraft potential in Volts [PRELIMINARY, for BROWSE PURPOSES ONLY.

Magnetic field solution (at 1 sample per sec) produced by VEFI on the Communication Navigation Outage Forecast System satellite. 

The DC vector magnetometer on the CNOFS spacecraft is a three axis, fluxgate sensor with active thermal control situated on a 0.6m boom.  This magnetometer measures the Earth's magnetic field, B, using 16 bit A/D converters at 1 sample per sec with a range of +/- 45,000 nT per sensor axis.  Its primary objective on the CNOFS spacecraft is to enable the most accurate V x B and E x B measurements along the spacecraft trajectory, where V is the spacecraft velocity in the fixed frame of the earth and E is the ambient, measured electric field.  The magnetic field data also provide indications of ionospheric currents as well as other geophysical phenomena.  In-flight calibration of the raw magnetic field data is carried out to determine gains, offsets, and the non-orthogonality matrix in the sensor axes frame.   The IGRF-11 model is used as a reference to help determine the calibration.  The calibrated magnetic field measurements are provided in the data file.  A full description of the instrument can be found in the published paper:  The Vector Electric Field Instrument (VEFI) on the C/NOFS Satellite, Pfaff et al., 2021, doi.org/10.1007/s11214-021-00859-y.         

VEFI was designed and built by NASA Goddard Space Flight Center. CNOFS is a joint effort between the Air Force Research Laboratory Space Vehicles Directorate and the USAF Space Test Program.

Users are requested to contact the P.I., Dr. Robert Pfaff at NASA GSFC, prior to publication of any VEFI data.

SPDF/CDAWeb. Please also acknowledge the data producer: Robert F. Pfaff at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Robert F. Pfaff at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Robert F. Pfaff at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cnofs/vefi/bfield_1sec/2008/cnofs_vefi_bfield_1sec_20080509_v06.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1454% of the 82251 timesteps. 

Electric Field solution (at 1 sample/sec) produced by VEFI on the Communication Navigation Outage Forecast System satellite.  The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY.

This data file contains information on the electric field solution as processed by the VEFI team at NASA/Goddard Space Flight Center.  The data is PRELIMINARY, and as such, is intended for BROWSE PURPOSES ONLY.  Registering your email will allow notification of updates.

While the VEFI data are still preliminary, users are requested to contact the P.I., Dr. Robert Pfaff at NASA GSFC, prior to publication of any VEFI data.

SPDF/CDAWeb. Please also acknowledge the data producer: Robert F. Pfaff at GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Robert F. Pfaff at GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Robert F. Pfaff at GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cnofs/vefi/efield_1sec/2008/cnofs_vefi_efield_1sec_20080509_v04.cdf. The most common cadence, 1007 [ms] = PT1.007S, occurred for 99.9598% of the 84553 timesteps. 

Key Parameter.  The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY. (from Master/CDFglobalAttributes/Data_type)

CNOFS VEFI Lightning Detector, low rate data (eclipse portion of CNOFS orbit)

This data file contains the low rate data from the VEFI lightning detector. Two photodiodes measure white light irradiance in 2 look directions and for 7 threshold values. Reference: Jacobson et al, J Atm Ocean Tech, 2011, doi:10.1175/JTECH-D-11-00047.1

SPDF/CDAWeb. Please also acknowledge the data producer: Robert H. Holzworth at University of Washington

SPDF/SSCWeb. Please also acknowledge the data producer: Robert H. Holzworth at University of Washington

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Robert H. Holzworth at University of Washington

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cnofs/vefi/ld_500msec/2008/cnofs_vefi_ld_500ms_200804232151_v02.cdf. The most common cadence, 503 [ms] = PT0.503S, occurred for 99.4557% of the 3837 timesteps. 

Vector Electric Field Instrument (from all.xml/instrument/description/@short)

Number of samples with white-light irradiance in 7 bins defined by the irradiance boundary values 0.23, 3.7, 11, 23, 39, 60, 84, > 84 mW/m^2 (north-viewing diode)

Number of samples with white-light irradiance in 7 bins defined by the irradiance boundary values 0.23, 3.7, 11, 23, 39, 60, 84, > 84 mW/m^2 (south-viewing diode)

Images and intensities. 557.7nm Images binned to geodetic gridReferences: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.

Canadian Auroral Network for the OPEN Program Unified Study, CANOPUS, Rules of the Road, Rules governing the Use and Distribution of CANOPUS Data

SPDF/CDAWeb. Please also acknowledge the data producer: J. Samson at U. Alberta

SPDF/SSCWeb. Please also acknowledge the data producer: J. Samson at U. Alberta

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Samson at U. Alberta

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/canopus/asi/1993/cn_k0_asi_19930213_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for 97.2973% of the 36 timesteps. 

Canadian Auroral Network Open Program Unified Study (from all.xml/observatory/description/@short)

Canadian Auroral Network Open Program Unified Study (from Master/CDFglobalAttributes/Source_name)

North & East Velocity components at 336.5 EDFL long. from 64.2 to 67.0 EDFL lat.References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.

SPDF/CDAWeb. Please also acknowledge the data producer: John Samson at University of Alberta

SPDF/SSCWeb. Please also acknowledge the data producer: John Samson at University of Alberta

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: John Samson at University of Alberta

Bistatic Auroral Radar System (from all.xml/instrument/description/@short)

Magnetic Field Extrema and LocationReferences: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/canopus/mari_mag/1992/cn_k0_mari_19920901_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Magnetometer and Riometer Array (from all.xml/instrument/description/@short)

Station Status, Merged Scaled 5577A Scans and Peak IntensityMerged Scans>from 3 stations along constant Geodetic Long. of 265, from Lat. 46 to 67References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.2.Samson, J.C., Lyons, L.R., Newell, P.T., Creutzberg, F. and Xu, B., Proton aurora substorm intensifications, Geophys. Res. Letters,19, 2167, 1992. 3.Samson, J.C., Hughes, T.J., Creutzberg, F., Wallis, D.D., Greenwald, R.A. and Ruohoniemi, J.M.,Observations of a detached discrete arc in association with field line resonances, J. Geophys. Res., 96, 15, 683, 1991.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/canopus/mpa/1992/cn_k0_mpa_19920901_v02.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 565 timesteps. 

Meridian Photometer Array (from all.xml/instrument/description/@short)

42 Values of 5577A Intensities from Geodetic Lat 46-67, Long=265

Riometer measurements and LocationReferences: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/canopus/mari_rio/1992/cn_k1_mari_19920901_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/cometgs_helio1day_position_19840101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 13514 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/cometgs_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/comethmp_helio1day_position_19960101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 9131 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/comethmp_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

CRRES MEA Data ArchiveThis is the re-processed version of the MEA data archive from the CRRES spacecraft. The raw data provided by Principal Investigator A. Vampola have been processed to derive 1 min average data. The data consists of counting rates from 17 energy channels in the range of 0.1-2 MeV and 19 pitch angle bins at 1 minute time intervals. The average flux, 90 degree flux and N value are included. Also included are the spacecraft geographic coordinates and altitude, L shell, and the local and equatorial magnetic field magnitudes from the 1977 Olson-Pfitzer model of the earth's geomagnetic field.The raw high resolution (0.512 sec) data and documentation of raw data can be found at: https://spdf.gsfc.nasa.gov/pub/data/crres/particle_mea/

This is an information file provided by the PI for the raw high resolution data.

SPDF/CDAWeb. Please also acknowledge the data producer: A. L. Vampola at Space Environment Effects, Vista, CA

SPDF/SSCWeb. Please also acknowledge the data producer: A. L. Vampola at Space Environment Effects, Vista, CA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. L. Vampola at Space Environment Effects, Vista, CA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/crres/particle_mea/mea_h0_cdaweb/1990/crres_h0_mea_19900728_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.6513% of the 12859 timesteps. 

Magnetic ElectronSpectrometer (MEA) data (from all.xml/observatory/description/@short)

Medium Electron A data (from all.xml/instrument/description/@short)

Trapped Radiation Modeling (from Master/CDFglobalAttributes/Discipline)

Magnetic ElectronSpectrometer (MEA) data (from Master/CDFglobalAttributes/Source_name)

High Resolution Data (from Master/CDFglobalAttributes/Data_type)

CSSWE is a 3U-CubeSat designed and developed by students at the University of Colorado at Boulder (CU-Boulder). The objective of the science mission is to address fundamental questions pertaining to the relationship between solar flares and energetic particles. These questions include the acceleration and loss mechanisms of outer radiation belt electrons. The goal is to measure differential fluxes of relativistic electrons in the energy range of 0.58-3.8 MeV and protons in 9-40 MeV. This project is a collaborative effort between the Laboratory for Atmospheric and Space Physics (LASP) and the Department of Aerospace Engineering Sciences (AES) at the University of Colorado, which includes the participation of students, faculty, and professional engineers. The science goals of the CSSWE mission are to study:    How flare location, magnitude, and frequency relate to the timing, duration, and energy spectrum of SEPs reaching Earth.   How the energy spectrum of radiation belt electrons evolve and how this evolution relates to the acceleration mechanism.To accomplish these goals CSSWE has a requirement for a minimum of 3 months of science operations based on expected flare and geomagnetic storm frequency. The first month of operations will be utilized for systems stabilization and check out.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/csswe/l1/reptile/counts/2012/csswe_reptile_6sec-counts-l1_20120914_v01.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for 97.3721% of the 11227 timesteps. 

Colorado Student Space Weather Experiment (from all.xml/observatory/description/@short)

Colorado Student Space Weather Experiment (from Master/CDFglobalAttributes/Source_name)

Relativistic Electron and Proton Telescope Integrated Little Experiment (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/csswe/l2/reptile/flux/2012/csswe_reptile_6sec-flux-l2_20120914_v01.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for 97.3721% of the 11227 timesteps. 

M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)NS S Southbound neutral sheetNT I Enter north tail lobe from inner magnetosphereST O Leave south tail lobe for inner magnetosphere

Counts based on variable 'Epoch__CT_JP_PSE' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/cluster/ct/jp/pse/2000/ct_jp_pse_20000801_v06.cdf. The most common cadence, 59100005 [ms] = PT16H25M0.005S, occurred for 9.0909% of the 2 timesteps. 

Cluster spacecraft Centroid (from all.xml/observatory/description/@short)

Cluster spacecraft Centroid (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dawn/helio1day/dawn_helio1day_position_20070928_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 4050 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dawn/helio1hr/dawn_helio1hr_position_20070928_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 316343 timesteps. 

DE-1 Retarding Ion Mass Spectrometer 1-min temperature and density data (low channel used for H+, He++, high channel for He+, O+, O++)

The data were provided by Dennis Gallagher (MSFC). The Retarding Ion Mass Spectrometer (RIMS) consisted of a retarding potential analyzer for energy analysis in series with a magnetic ion-mass spectrometer for mass analysis. Multiple sensor heads permitted the determination of the thermal plasma flow characteristics. This instrument was designed to operate in two basic commandable modes: a high-altitude mode in which the density, temperature, and bulk-flow characteristics of principally H+, He+, and O+ ions were measured; and a low-altitude mode that concentrated on the composition in the 1- to 32-u range. This investigation provided information on (1) the densities of H+, He+, and O+ ions in the ionosphere, plasmasphere, plasma trough, and polar cap (including the density distribution along the magnetic vector in the vicinity of the satellite apogee); (2) the temperature of H+, He+, and O+ ions in the ionosphere, plasmasphere, plasma trough, and polar cap (energy range 0-45 eV); (3) the bulk flow velocities of H+, He+, and O+ in the plasmapause, plasma trough and polar cap; (4) the changing character of the cold plasma density, temperature, and bulk flow in regions of interaction with hot plasma such as at the boundary between the plasmasphere and the ring current; and (5) the detailed composition of ionospheric plasma in the 1-to 32-u range. He++ and O++ were also measured. The instrument consisted of three detector heads. One looked out in the radial direction, and the other two were along the plus and minus spin-axis directions. Each detector had a 55-deg half-cone acceptance angle. The detector heads had a gridded, weakly collimating aperture where the retarding analysis was performed, followed by a parallel plate ceramic magnetic mass analyzer with two separate exit slits corresponding to ion masses in the ratio 1:4. Ions exiting from these slits were detected with electron multipliers. In the apogee mode, the thermal particle fluxes were measured while the potential on a set of retarding grids was stepped through a sequence of settings. In the perigee mode, the retarding grids were grounded and the detector utilized a continuous acceleration potential sweep that focused the mass ranges from 1 to 8, and 4 to 32 u. Time resolution was 16 msec. Additional details can be found in C. R. Chappell et al., Space Sci. Instrum., v. 5, n. 4, p. 477, 1981.Criterian for selecting data points to be fitted aperature bias = 0 must have at least 10 or more non-zero points in rpa curve.  if less that 1.3 Re high voltage monitor must be turned on maximum countr rate value must at least 5.0 must have at least 4 points starting from end of rpa curve find 3 consecutive point of increasing value, reset end of rpa curve to here make certain last point is 1 sigma above noise level (the points excluded in previous step), if not drop point and check new last point, continue until criteria is met, must have at least 3 points left starting at new end of selected rpa curve stop first point greater that 80% of maximum of spin curve, if non found stop at last point less that maximum, must have at least 3 points left change curve from count rate curve to l**2 curve if number of points are 5 or less: do a linear least squares fit (linfit) to the data, if the linear correlation coefficient (lcc) greater than 0.800 then points will be used, if not, data set is discarded if number of points are greater then 5: do a linfit to the bottom 5 and a linfit to the top 5 points, in 6 or more points do linfit to the middle 5, saving the lcc and slope for each case. if all three lccs are less than 0.800 discard data set through a series of tests find the set of 5 with the best lcc slope combination once set of 5 has been selected add rest of points one at a time and redo linfit, if lcc gets worse discard point otherwise keep it, do this until all points are checked we now have the points to be used

More information on DE-1 Retarding Ion Mass Spectrometer is available at

DE-1 Retarding Ion Mass Spectrometer, RIMS, Overview Web Page, MSFC

Information on the Dynamics Explorer 1, DE-1, Retarding Ion Mass Spectrometer, RIMS, at Marshall Space Flight Center

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Charles R. Chappell at NASA/MSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Charles R. Chappell at NASA/MSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Charles R. Chappell at NASA/MSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/plasma_rims/plasma_1min_cdf/1981/de1_1min_rims_19811007_v01.cdf. The most common cadence, 56000 [ms] = PT56S, occurred for 37.2588% of the 4132 timesteps. 

Dynamics Explorer 1 (from all.xml/observatory/description/@short)

Dynamics Explorer 1 (from Master/CDFglobalAttributes/Source_name)

Retarding Ion Mass Spectrometer (from Master/CDFglobalAttributes/Data_type)

H+ Temperature in eV, detector head in positive z-direction (spin axis)

H+ Temperature in eV, detector head in negative z-direction (spin axis)

H+ density in cm-3, fit to radial head data with temp-z held constant

H+ density in cm-3, radial head data with potential (avg_pot) held constant

H+ Temperature values minus standard deviation (StD) in K, +z head

n (H+) from fit to radial head data with temp held constant (temp_z-STD)

H+ density from fit to radial head data with potential (avg_pot) held constant, T-STD

+++ Temperature values plus standard deviation (STD): H+ temperature in K plus STD, +z head

n (H+) from fit to radial head data with temp held constant (temp_z+STD)

H+ density from fit to radial head data with potential (avg_pot) held constant, T+STD

SPDF/CDAWeb. Please also acknowledge the data producer: David Winningham at Southwest Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: David Winningham at Southwest Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David Winningham at Southwest Research Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/orbit/2sec_oa_cdaweb/1981/de1_2sec_oa_1981081500_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.9724% of the 3627 timesteps. 

Magnetospheric Ionospheric Interactions (from Master/CDFglobalAttributes/Discipline)

orbit and additude data (from Master/CDFglobalAttributes/Data_type)

Dynamics Explorer 1 spacecraft was one of two satellites in the Dynamics Explorer program.  The DE-1 and DE-2 satellites were launched by the same vehicle so that their orbits would be coplanar, allowing two-point measurements along magnetic field lines, for the purpose of studying coupling between the magnetosphere, ionosphere, and upper atmosphere.  The DE-1 orbit was highly elliptical with an apogee of 4.35 Re and a perigee of 500 km whereas the DE-2 spacecraft was placed in a much lower 300 x 1000 km altitude orbit. DE-1 was spin stabilized with its spin axis normal to the plane of the orbit. DE-2 was three axis stabilized with one face being nadir oriented. The study of field-aligned currents and MHD waves were the primary objectives of the DE-1/2 magnetometer investigation. Comparison of the magnetometer data with measurements of precipitating charged particles yielded new information on the field-aligned current carriers.  In combination with the electric field measurements, it was possible to determine the vertical Poynting Flux of electromagnetic energy flowing between the magnetosphere and ionosphere and to separate small-scale field-aligned currents from MHD waves through the evaluation of the local ratio of the electric to magnetic field amplitudes in these perturbations. The field-aligned current measurements and neutral atmosphere observations also provided an opportunity for investigating atmosphere-magnetosphere coupling and assessing the total rate of energy transfer into the upper atmosphere.  Finally, the DE-1/2 magnetometer investigation provided a vital service in so far as a knowledge of magnetic field direction and intensity is essential to any number of space plasma science investigations utilizing the various DE-1/2 particles and fields data sets.  The DE-1 magnetic field (MAG-A) high time resolution data set consists of triaxial fluxgate measurements taken every 62.5 msec (i.e., 16 vectors/second).  As described in Farthing et al. (1981), the DE-1 magnetometer had a digital resolution of +1.5 nT in its low altitude, least sensitive mode. Two higher sensitivity modes were used at higher altitudes with digital resolutions of +0.25 nT and +0.02 nT, respectively. The MAG-A data set consists of the three components of the magnetic field, B-Radial (Br), B-Theta (Bth), and B-Phi (Bph), in Geomagnetic Spherical (GMS) Coordinates. This is a local Cartesian coordinate system. The R, Theta and Phi axes are oriented relative to a MAGSAT magnetic field model (Langel et al., 1980) positive in the directions of increasing radial distance from the center of the Earth (i.e., outward), increasing magnetic colatitude (i.e., southward) and increasing azimuth angle (i.e., magnetic east). The following Orbit Attitude (OA) parameters are also included in the archive data set: model magnetic field in GMS coordinates; altitude of the satellite; magnetic latitude and longitude; magnetic local time, and invariant latitude. The data set consists of daily files from 81258 to 91049. Each file contains all of the data available for a given day. If there were no magnetometer data for a given time, the time record was left out. If there were magnetometer data, but no orbit or model field data, a fill value of 9999999.0 was used for the missing values.  The dominant source of error in the DE-1 magnetic field measurements is the uncertainty in the attitude of the spacecraft. The DE-1 spacecraft was designed to an attitude uncertainty specification of about 0.3 degree which appears to have been met much of the time. As a rule of thumb each 0.1 degree in attitude uncertainty near perigee corresponds to an error of approximately 100 nT in each component of the field when the magnetic field measured at the sensors is transferred to an inertial frame of reference or a model field is transferred into the 0spacecraft frame and subtracted from the measured field.  For this reason it is common for the residual, or delta-B field obtained by subtracting the model field at low altitudes (i.e., high fields) to show a gradual shift of several 100 nT from the start of a passage across the polar cap to the other side.  (These slow shifts in the baselines of the vector field components do not affect most scientific analyses, e.g., field-aligned current measurements, but they can be effectively dealt with through modeling if need be.  At higher altitudes the ambient field intensity is less and the uncertainty due to attitude errors is correspondingly smaller.The absolute accuracy of the DE-1 total magnetic field measurement has also been evaluated through comparison with the precision vector/scalar magnetic field observatories located on the ground which are used to monitor the geomagnetic field. On the basis of such cross-comparisons utilizing DE-1 perigee data over the life of the mission, R. Langel (private communication, 1994) found excellent agreement between the MAG-A and ground-based observatory scalar data sets at the 20 to 40 nT level. On time scales comparable to or less than the DE-1 spin period, 6 sec, other artifacts are present in the data set which must be considered for somescientific investigations. Like most telemetered geophysical data, the vector.components archived here suffer from occasional bad data points. These spurious data entries were caused, for the most part, by noise introduced in the satellite-receiving station telemetry link. Such bad data can usually be recognized by workers familiar with such data sets. These are for the most part single point data excursions which show no geophysical correlation between the magnetic field components and the observations of plasma phenomena by the other DE instruments. Similarly, there sometimes exist spurious data points in the ancillary orbit/attitude database.  Some are obvious such as model magnetic field values for which the sign values have been corrupted. Others, such as occasional millisecond jumps in the time, produce small, unphysical discontinuities in the processed field components. Small discontinuities are also sometimes present at the point where the magnetometer changes mode due to slight imperfections in calibration parameters which are independently determined for each mode. (N.B., mode changes can be readily detected by the change in the digital resolution of the data in an expanded vertical scale plot of B versus time.) In using any unfamiliar data set, caution is advised and tests to screen out instrumental artifacts should be devised before reaching important conclusions.De-spinning high sensitivity, boom mounted vector magnetometer data in high fields (i.e., >1000 nT) frequently results in a readily observable residual signal at the spin period and its harmonics. In the case of the DE-1 magnetometer measurements, the dominant causes of residual spin tone were found to be small (0.1 to 0.01%) changes in the instrument scale factors and boom bending of up to several tenths of a degree in response to varying thermal inputs due to orbit/attitude driven changes in solar illumination (e.g., seasonal variations, eclipses, etc.). These effects were minimized through an orbit by orbit calibration procedure which analyzed the residual spin tone around apogee and perigee and adjusted the scale factors and sensor attitude accordingly. Even after these in-flight calibration activities, residual spin tone signals in the MAG-A data with amplitudes of tens of nanotesla are common in high fields around perigee. The most probable cause of these residuals is the transverse field dependence of fluxgate magnetometers in high fields which was not well-appreciated at the time that DE-1/2 magnetometers were designed.and calibrated in the late 1970's. As discussed by Luhr et al. (1995) in regards to the magnetometer on the low altitude, spin stabilized Freja spacecraft, this non-linear effect can easily produce the residual spin frequency signals present in the MAG-A data set.

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Masahisa Sugiura at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Masahisa Sugiura at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Masahisa Sugiura at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/magnetic_fields_maga/62ms_magagms_cdaweb/1981/de1_62ms_maga-gms_19810915_v01.cdf. The most common cadence, 62 [ms] = PT0.062S, occurred for 49.9934% of the 121729 timesteps. 

Dynamics Explorer-1 (from all.xml/observatory/description/@short)

Magnetic Field Observations Triaxial Fluxgate Magnetometer (MAG-A) (from all.xml/instrument/description/@short)

Magnetospheric  Ionospheric Interactions (from Master/CDFglobalAttributes/Discipline)

Dynamics Explorer-1 (from Master/CDFglobalAttributes/Source_name)

NSSDC's Master Catalog on the Magnetic Field Observations Triaxial Fluxgate Magnetometer

Introduction to the Magnetic Field Observations Triaxial Fluxgate Magnetometer on DE 1

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/magnetic_fields_maga/6sec_magagms_cdaweb/1981/de1_6sec_magagms_19810915_v01.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for 99.7475% of the 1975 timesteps. 

Magnetic Field Observations Triaxial Fluxgate Magnetometer (MAG-A) (from Master/CDFglobalAttributes/Data_type)

Radial Component of reference magnetic field (MAGSAT model) in GEO coord.

Theta Component of reference magnetic field (MAGSAT model) in GEO coord. 

Phi Component of reference magnetic field (MAGSAT model) in GEO coord.

Parallel Component of Difference Magnetic Field in Local Magnetic (LMG) Coord.

Perpendicular Component (1) of Difference Magnetic Field in Local Magnetic (LMG) Coord.

Perpendicular (2) Component of Difference Magnetic Field in Local Magnetic (LMG) Coord.

DE-1 Plasma Wave Instrument (PWI) Low Frequency Correlator (LFC) Electric and Magnetic Field Spectral Density

S. D. Shawhan, D. A. Gurnett, D. L. Odem, R. A. Helliwell, and C. G. Park, The plasma wave and quasi-static electric field instrument (PWI) for Dynamics Explorer-A, Space Sci. Instrumen., 5, 535, 1981.

Users of the DE-1 PWI LFC data are encuraged to acknowledge NASA CDAWeb and The University of Iow as the source of the data in any publication.

More information on DE-1 Plama Wave Investigation is available at

DE-1 PWI LFC data are open to everyone. However, users of these data are encouraged to contact the PI institute and the DE-1 PWI website should questions arise.

SPDF/CDAWeb. Please also acknowledge the data producer: Donald Gurnett at University Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: Donald Gurnett at University Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Donald Gurnett at University Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/waves_pwi/lfc-spectra_cdaweb/1981/de1_pwi_lfc-spectra_19810916_v01.cdf. The most common cadence, 32000000000 [ns] = PT32S, occurred for 95.4545% of the 1008 timesteps. 

Plasma Wave Instrument (from all.xml/instrument/description/@short)

Low Frequency Correlator Electric and Magnetic Field Spectral Density (from Master/CDFglobalAttributes/Data_type)

Spin Plane E-Field (LFC Ex) Spectra, 200 meter antenna, 104 Hz to 409 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Plane E-Field (LFC Ex) Spectra, 200 meter antenna, 104 Hz to 409 kHz

Spin Axis E-Field (LFC Ez) Spectra, 8 meter antenna, 104 Hz to 409 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Axis E-Field (LFC Ez) Spectra, 8 meter antenna, 104 Hz to 409 kHz

Spin Plane E-Field (LFC Es) Spectra, 0.6 meter antenna, 104 Hz to 100 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Plane E-Field (LFC Es) Spectra, 0.6 meter antenna, 104 Hz to 100 kHz

Spin Axis B-Field Spectra (LFC H), search coil, 1.8 to 100 Hz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Axis B-Field Spectra (LFC H), search coil, 1.8 to 100 Hz

The Filter Receiver used to measure the Ex Antenna output (1=A,2=B,3=both)

Integer combining all data quality flags (0 = no issues detected)

Users of the DE-1 PWI data are encouraged to acknowledge NASA CDAWeb and The University of Iow as the source of the data in any publication.

More information on the DE-1 Plama Wave Investigation is available at the University of Iowa DE-1 PWI Page

DE-1 PWI ephemeris and attitude data are open to everyone.  However, users of these data are encouraged to contact the PI institute and the DE-1 PWI website should questions arise.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/orbit/or-at_cdaweb/1981/de1_pwi_or-at_19810916_v01.cdf. The most common cadence, 8000000000 [ns] = PT8S, occurred for 98.7261% of the 4185 timesteps. 

DE-1 Plasma Wave Instrument (PWI) Step Frequency Correlator (SFC) Electric and Magnetic Field Spectral Density

DE-1 PWI SFC data are open to everyone. However, users of these data are encouraged to contact the PI institute and the DE-1 PWI website should questions arise.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/waves_pwi/sfc-spectra_cdaweb/1981/de1_pwi_sfc-spectra_19810916_v01.cdf. The most common cadence, 32000000000 [ns] = PT32S, occurred for 95.4545% of the 1008 timesteps. 

Step Frequency Correlator Electric and Magnetic Field Spectral Density (from Master/CDFglobalAttributes/Data_type)

Spin Plane E-Field (SFC Ex) Spectra, 200 meter antenna, 104 Hz to 409 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Plane E-Field (SFC Ex) Spectra, 200 meter antenna, 104 Hz to 409 kHz

Spin Axis E-Field (SFC Ez) Spectra, 8 meter antenna, 104 Hz to 409 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Axis E-Field (SFC Ez) Spectra, 8 meter antenna, 104 Hz to 409 kHz

Spin Plane E-Field (SFC Es) Spectra, 0.6 meter antenna, 104 Hz to 100 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Plane E-Field (SFC Es) Spectra, 0.6 meter antenna, 104 Hz to 100 kHz

Spin Plane B-Field (SFC B) Spectra, 1.0 m**2 loop antenna, 104 to 409 kHz [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] Spin Plane B-Field (SFC B) Spectra, 1.0 m**2 loop antenna, 104 to 409 kHz

The SFR Receivers used to measure the Ex Antenna output (1=A,2=B,3=both)

Dynamics Explorer 2, DE 2, Merged Magnetometer Instrument, MAGB, and Vector Electric Field Instrument, VEFI, data readme text file, NASA GSFC

Dynamics Explorer 2, DE 2, Merged Magnetometer Instrument, MAGB, and Vector Electric Field Instrument, VEFI, data readme text file, hosted by NASA GSFC

Dynamics Explorer 2, DE 2, Magnetometer Instrument, MAGB, instrument and data description, NASA GSFC

Dynamics Explorer 2, DE 2, Magnetometer Instrument, MAGB, instrument and data description, hosted by NASA GSFC

Dynamics Explorer 2, DE 2, Vector Electric Field Instrument, VEFI, instrument and data description, NASA GSFC

Dynamics Explorer 2, DE 2, Vector Electric Field Instrument, VEFI, instrument and data description, hosted by NASA GSFC

OMNIWeb FTP Browser access to Dynamics Explorer 2 Magnetic and Electric Field ASCII data, NASA GSFC

OMNIWeb FTP Browser access to Dynamics Explorer 2 Magnetic and Electric Field ASCII data including plot, listing, and output file services, hosted by NASA GSFC

General information concerning the Dynamics Explorer 2, Magnetic Field Observations, MAG-B, instrument

General information concerning the Dynamics Explorer 2, Vector Electric Field Instrument, VEFI, instrument

SPDF/CDAWeb. Please also acknowledge the data producer: Jim Slavin at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Jim Slavin at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Jim Slavin at NASA/GSFC

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => vtimeEpoch, @1 => mtimeEpoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => vtimeEpoch, @1 => mtimeEpoch.)

merged Vector Electric field instrument and Magnetometer (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'vtimeEpoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/magnetic_electric_fields_vefi_magb/62ms_vefimagb_cdaweb/1981/de2_62ms_vefimagb_19810815_v01.cdf. The most common cadence, 62 [ms] = PT0.062S, occurred for 50.0372% of the 39001 timesteps. 

Counts based on variable 'mtimeEpoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/magnetic_electric_fields_vefi_magb/62ms_vefimagb_cdaweb/1981/de2_62ms_vefimagb_19810815_v01.cdf. The most common cadence, 62 [ms] = PT0.062S, occurred for 50.0385% of the 39002 timesteps. 

500-msec AC data from each channel for each of the 3 spectrometers of the vector electric field instrument

Dynamics Explorer 2, DE 2, Vector Electric Field Instrument, VEFI, data readme text file, NASA GSFC

Dynamics Explorer 2, DE 2, Vector Electric Field Instrument, VEFI, data readme text file, hosted by NASA GSFC

SPDF/CDAWeb. Please also acknowledge the data producer: N.C. Maynard/R. Pfaff at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: N.C. Maynard/R. Pfaff at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: N.C. Maynard/R. Pfaff at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/electric_fields_vefi/ac500ms_vefi_cdaweb/1981/de2_ac500ms_vefi_19810810_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 99.9268% of the 9560 timesteps. 

vector electric field instrument (from Master/CDFglobalAttributes/Data_type)

500-msec DC electric field x- and y-components from the vector electric field instrument

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Nelson C. Maynard at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Nelson C. Maynard at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Nelson C. Maynard at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/electric_fields_vefi/dca500ms_vefi_cdaweb/1981/de2_dca500ms_vefi_19810810_v01.cdf. The most common cadence, 500 [ms] = PT0.5S, occurred for 99.9702% of the 16762 timesteps. 

Electric field in Millivolts/meter in spacecraft coord. ---> x component

Electric field in Millivolts/meter in spacecraft coord. (non-adjusted)---> x component 

Integrated potential along the x-axis in spacecraft coordinates (non-adjusted)

NSSDC's Master Catalog on the Retarding Potential Analyzer (RPA)

The Retarding Potential Analyzer (RPA) measured the bulk ion velocity in the direction of the spacecraft motion, the constituent ion concentrations, and the ion temperature along the satellite path. These parameters were derived from a least squares fit to the ion number flux vs energy curve obtained by sweeping or stepping the voltage applied to the internal retarding grids of the RPA. In addition, a separate wide aperture sensor, a duct sensor, was flown to measure the spectral characteristics of iregularities in the total ion concentration. The measured parameters obtained from this investigation were important to the understanding of mechanisms that influence the plasma; i.e., to understand the coupling between the solar wind and the earth's atmosphere. The measurements were made with a multigridded planar retarding potential analyzer very similar in concept and geometry to the instruments carried on the AE satellites. The retarding potential was variable in the range from approximately +32 to 0 volts. The details of this voltage trace, and whether it was continuous or stepped, depended on the operating mode of the instrument. Specific parameters deduced from these measurements were ion temperature; vehicle potential; ram component of the ion drift velocity; the ion and electron concentration irregularity spectrum; and the concentration of H+, He+, O+, and Fe+, and of molecular ions near perigee. Additional details are in W. B. Hanson et al., Space Sci. Instrum., v. 5, n. 4, p. 503, 1981.

SPDF/CDAWeb. Please also acknowledge the data producer: Rod Heelis at University of Texas, Dallas

SPDF/SSCWeb. Please also acknowledge the data producer: Rod Heelis at University of Texas, Dallas

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Rod Heelis at University of Texas, Dallas

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_den, @1 => Epoch_wb1, @2 => Epoch_wb2, @3 => Epoch_wb3, @4 => Epoch_wb4, @5 => Epoch_wb5, @6 => Epoch_wb6, @7 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_den, @1 => Epoch_wb1, @2 => Epoch_wb2, @3 => Epoch_wb3, @4 => Epoch_wb4, @5 => Epoch_wb5, @6 => Epoch_wb6, @7 => Epoch.)

Retarding PotentialAnalyzer (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch_den' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 15 [ms] = PT0.015S, occurred for 99.8071% of the 40880 timesteps. 

Counts based on variable 'Epoch_wb1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3730% of the 317 timesteps. 

Counts based on variable 'Epoch_wb2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3730% of the 317 timesteps. 

Counts based on variable 'Epoch_wb3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3730% of the 317 timesteps. 

Counts based on variable 'Epoch_wb4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3730% of the 317 timesteps. 

Counts based on variable 'Epoch_wb5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3730% of the 317 timesteps. 

Counts based on variable 'Epoch_wb6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3730% of the 317 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/rpa16ms_cdaweb/1981/de2_duct16ms_rpa_19810803_v01.cdf. The most common cadence, 8000 [ms] = PT8S, occurred for 97.4684% of the 77 timesteps. 

2-sec ion temperature, velocity, and densities (O+, H+, He+, molecular)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_rpa/ion2s_cdaweb/1981/de2_ion2s_rpa_19810806_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 96.5753% of the 141 timesteps. 

x component of ion velocity in s/c coordinates (vx) - vx is app. parallel to s/c direction of motion

Y component of ion velocity in s/c coordinates (vy) - vy is app. vertical to s/c dir. of motion (>0 up)

z component of ion velocity in s/c coordinates (vz) - vz is app. vertical to s/c dir. of motion (>0 right)

Data quality flag (<0 untrustworthy, see https://spdf.gsfc.nasa.gov/pub/data/de/de2/plasma_rpa/

Sweep type (1: 0->10Volt, 2: 0-10V, 3: 0-8V Integral, 4: 0-8V Electronic

DE-2, LAPI_Corrected Electron Counts and Flux from Power Supply 1 IDFS format

The DE-2 spacecraft (low-altitude mission) complemented the high-altitude mission DE-1and was placed into an orbit with a perigee sufficiently low to permit measurements of neutral composition, temperature, and wind. The apogee was high enough to permit measurements above the interaction regions of suprathermal ions, and also plasma flow measurements at the feet of the magnetospheric field lines. The general form of the spacecraft was a short polygon 137 cm in diameter and 115 cm high. The triaxial antennas were 23 m tip-to-tip. One 6-m boom was provided for remote measurements. The spacecraft weight was 403 kg. Power was supplied by a solar cell array, which charged two 6-ampere-hour nickel-cadmium batteries. The spacecraft was three-axis stabilized with the yaw axis aligned toward the center of the earth to within 1 deg. The spin axis was normal to the orbit plane within 1 deg with a spin rate of one revolution per orbit. A single-axis scan platform was included in order to mount the low-altitude plasma instrument (81-070B-08). The platform rotated about the spin axis. A pulse code modulation telemetry data system was used that operated in real time or in a tape-recorder mode. Data were acquired on a science-problem-oriented basis, with closely coordinated operations of the various instruments, both satellites, and supportive experiments. Measurements were temporarily stored on tape recorders before transmission at an 8:1 playback-to-record ratio. Since commands were also stored in a command memory unit, spacecraft operations were not real time. Additional details can be found in R. A. Hoffman et al., Space Sci. Instrum., v. 5, n. 4, p. 349, 1981. DE-2 reentered the atmosphere on February 19, 1983. The Low-Altitude Plasma Instrument (LAPI) provided high-resolution velocity space measurements of positive ions and electrons from 5 eV to 32 keV. The two Geiger-Mueller counter tubes (0 and 90 deg) measured trapped electrons and precipitating electrons above 35 keV as integral number flux. Pitch angle measurements covered the full 180 deg range. Data from this investigation and supporting measurements were used to study (1) the identification and intensities of Birkeland currents, (2) auroral particle source regions and acceleration mechanisms, (3) the existence and role of E parallel to B, (4) sources and effects of polar cap particle fluxes, (5) the transport of plasma within and through the magnetospheric cusp, (6) dynamic configurations of high-latitude flux tubes, (7) loss-cone effects of wave-particle interactions, (8) hot-cold plasma interactions, (9) ionospheric effects of particle precipitation, and (10) plasma convection at high altitudes. The instrument contained an array of 15 parabolic electrostatic analyzers of the ISIS 2 type, each with an electron channel and an ion channel, in order to obtain detailed pitch-angle distributions as a function of energy. Two Geiger-Mueller counters were mounted on the scan platform. The basic mode of operation provided a 32-point energy spectrum in the range 5 eV to 32 kev every second. The voltages on the electrostatic analyzers were programmable to allow for greater space/time resolution over limited portions of the energy and angular distributions. The instrument was mounted on a one-axis scan platform controlled by a magnetometer, whose purpose was to maintain the detector array, which spanned 180 deg, at a nearly constant angle to the magnetic field. Additional details are found in J. D. Winningham et al., Space Sci. Instrum., v. 5, n. 4, p. 465, 1981. From March 16, 1982 to April 4, 1982 the instrument was turned off for corrective action. The Instrument Data File Set. URL http://www.idfs.org 

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. J. David  Winningham at Southwest Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. J. David  Winningham at Southwest Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. J. David  Winningham at Southwest Research Institute

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Mode_Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Mode_Epoch.)

LAPI_Corrected Electron Counts and Flux from Power Supply 1 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_electron-flux-counts-pps1-cdf/1981/de2_lapi_electron-flux-counts-pps1_19810815130902_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.3478% of the 546 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_electron-flux-counts-pps1-cdf/1981/de2_lapi_electron-flux-counts-pps1_19810815130902_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.3478% of the 546 timesteps. 

DE-2, LAPI_Corrected Electron Counts and Flux from Power Supply 2 IDFS format

Dynamics Explorer 2 (from all.xml/observatory/description/@short)

LAPI_Corrected Electron Counts and Flux from Power Supply 2 (from all.xml/instrument/description/@short)

Dynamics Explorer 2 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_electron-flux-counts-pps2-cdf/1981/de2_lapi_electron-flux-counts-pps2_19810815130901_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.2834% of the 546 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_electron-flux-counts-pps2-cdf/1981/de2_lapi_electron-flux-counts-pps2_19810815130901_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.2834% of the 546 timesteps. 

DE-2, The Low Altitude Plasma Instrument (LAPI) Corrected IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_geiger-mueller-cdf/1981/de2_lapi_geiger-mueller_19810815130902_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9327% of the 1485 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_geiger-mueller-cdf/1981/de2_lapi_geiger-mueller_19810815130902_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9327% of the 1485 timesteps. 

The Low Altitude Plasma Instrument /LAPI/ The Low Altitude Plasma Instrument on the Dynamics Explorer-B spacecraft provides high resolution velocity space measurements of positive ions and electrons from 5 eV to 32 keV and a monitor of electrons with energies above 35 keV. It consists of an array of 15 parabolic electrostatic analyzers spanning 180 deg in angle and two Geiger-Mueller counters mounted on a one-degree of freedom-scan platform. The platform is controlled by a magnetometer that allows placement of the array to selected angles with respect to the magnetic field. Each parabolic analyzer simultaneously measures electrons and positive ions. The temporal resolution and energy range of the measurements and the detector complement to be sampled are programmable by ground command. 1. The Instrument Data File Set. URL http://www.idfs.org 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_geiger-mueller-ratio-cdf/1981/de2_lapi_geiger-mueller-ratio_19810815130902_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9327% of the 1485 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_geiger-mueller-ratio-cdf/1981/de2_lapi_geiger-mueller-ratio_19810815130902_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9327% of the 1485 timesteps. 

DE-2, LAPI_Corrected Ion Counts and Flux from Power Supply 1 IDFS format

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. J. David Winningham at Southwest Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. J. David Winningham at Southwest Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. J. David Winningham at Southwest Research Institute

LAPI_Corrected Ion Counts and Flux from Power Supply 1 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_ion-flux-counts-pps1-cdf/1981/de2_lapi_ion-flux-counts-pps1_19810815130902_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.3478% of the 546 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_ion-flux-counts-pps1-cdf/1981/de2_lapi_ion-flux-counts-pps1_19810815130902_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.3478% of the 546 timesteps. 

DE-2, LAPI_Corrected Ion Counts and Flux from Power Supply 2 IDFS format

The Low Altitude Plasma Instrument /LAPI/ The Low Altitude Plasma Instrument on the Dynamics Explorer-B spacecraft provides high resolution velocity space measurements of positive ions and electrons from 5 eV to 32 keV and a monitor of electrons with energies above 35 keV. It consists of an array of 15 parabolic electrostatic analyzers spanning 180 deg in angle and two Geiger-Mueller counters mounted on a one-degree of freedom-scan platform. The platform is controlled by a magnetometer that allows placement of the array to selected angles with respect to the magnetic field. Each parabolic analyzer simultaneously measures electrons and positive ions. The temporal resolution and energy range of the measurements and the detector complement to be sampled are programmable by ground command. 1. The Instrument Data File Set. URL http://www.idfs.org

LAPI_Corrected Ion Counts and Flux from Power Supply 2 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_ion-flux-counts-pps2-cdf/1981/de2_lapi_ion-flux-counts-pps2_19810815130901_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.2834% of the 546 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_ion-flux-counts-pps2-cdf/1981/de2_lapi_ion-flux-counts-pps2_19810815130901_v01.cdf. The most common cadence, 2062000000 [ns] = PT2.062S, occurred for 59.2834% of the 546 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_lapi-mag-cdf/1981/de2_lapi_lapi-mag_19810815130902_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9327% of the 1485 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_lapi-mag-cdf/1981/de2_lapi_lapi-mag_19810815130902_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9327% of the 1485 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_orbit-attitude-cdf/1981/de2_lapi_orbit-attitude_19810815130902_v01.cdf. The most common cadence, 8000000000 [ns] = PT8S, occurred for 99.4565% of the 183 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_orbit-attitude-cdf/1981/de2_lapi_orbit-attitude_19810815130902_v01.cdf. The most common cadence, 8000000000 [ns] = PT8S, occurred for 99.4565% of the 183 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_orbit-attitude-magb-cdf/1981/de2_lapi_orbit-attitude-magb_19810815034446_v01.cdf. The most common cadence, 62000000 [ns] = PT0.062S, occurred for 50.0412% of the 11527 timesteps. 

LAPI_Corrected Precopitation and Pitch Angles (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_pitch-angles-cdf/1981/de2_lapi_pitch-angles_19810815130852_v01.cdf. The most common cadence, 500000000 [ns] = PT0.5S, occurred for all 2990 timesteps. 

Data Quality Indicator for LAPI+ 97.5 deg Pitch Angle, sensor 22

Data Quality Indicator for LAPI+ 112.5 deg Pitch Angle sensor 23

Data Quality Indicator for LAPI+ 172.5 deg Pitch Angle sensor 27

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_pitch-angles-cdf/1981/de2_lapi_pitch-angles_19810815130852_v01.cdf. The most common cadence, 500000000 [ns] = PT0.5S, occurred for all 2990 timesteps. 

The DE-2 spacecraft (low-altitude mission) complemented the high-altitude mission DE-1and was placed into an orbit with a perigee sufficiently low to permit measurements of neutral composition, temperature, and wind. The apogee was high enough to permit measurements above the interaction regions of suprathermal ions, and also plasma flow measurements at the feet of the magnetospheric field lines. The general form of the spacecraft was a short polygon 137 cm in diameter and 115 cm high. The triaxial antennas were 23 m tip-to-tip. One 6-m boom was provided for remote measurements. The spacecraft weight was 403 kg. Power was supplied by a solar cell array, which charged two 6-ampere-hour nickel-cadmium batteries. The spacecraft was three-axis stabilized with the yaw axis aligned toward the center of the earth to within 1 deg. The spin axis was normal to the orbit plane within 1 deg with a spin rate of one revolution per orbit. A single-axis scan platform was included in order to mount the low-altitude plasma instrument (81-070B-08). The platform rotated about the spin axis. A pulse code modulation telemetry data system was used that operated in real time or in a tape-recorder mode. Data were acquired on a science-problem-oriented basis, with closely coordinated operations of the various instruments, both satellites, and supportive experiments. Measurements were temporarily stored on tape recorders before transmission at an 8:1 playback-to-record ratio. Since commands were also stored in a command memory unit, spacecraft operations were not real time. Additional details can be found in R. A. Hoffman et al., Space Sci. Instrum., v. 5, n. 4, p. 349, 1981. DE-2 reentered the atmosphere on February 19, 1983. The Low-Altitude Plasma Instrument (LAPI) provided high-resolution velocity space measurements of positive ions and electrons from 5 eV to 32 keV. The two Geiger-Mueller counter tubes (0 and 90 deg) measured trapped electrons and precipitating electrons above 35 keV as integral number flux. Pitch angle measurements covered the full 180 deg range. Data from this investigation and supporting measurements were used to study (1) the identification and intensities of Birkeland currents, (2) auroral particle source regions and acceleration mechanisms, (3) the existence and role of E parallel to B, (4) sources and effects of polar cap particle fluxes, (5) the transport of plasma within and through the magnetospheric cusp, (6) dynamic configurations of high-latitude flux tubes, (7) loss-cone effects of wave-particle interactions, (8) hot-cold plasma interactions, (9) ionospheric effects of particle precipitation, and (10) plasma convection at high altitudes. The instrument contained an array of 15 parabolic electrostatic analyzers of the ISIS 2 type, each with an electron channel and an ion channel, in order to obtain detailed pitch-angle distributions as a function of energy. Two Geiger-Mueller counters were mounted on the scan platform. The basic mode of operation provided a 32-point energy spectrum in the range 5 eV to 32 kev every second. The voltages on the electrostatic analyzers were programmable to allow for greater space/time resolution over limited portions of the energy and angular distributions. The instrument was mounted on a one-axis scan platform controlled by a magnetometer, whose purpose was to maintain the detector array, which spanned 180 deg, at a nearly constant angle to the magnetic field. Additional details are found in J. D. Winningham et al., Space Sci. Instrum., v. 5, n. 4, p. 465, 1981. From March 16, 1982 to April 4, 1982 the instrument was turned off for corrective action. Instruments abbreviations: FPI: Fabry-Perot InterferometerIDM: Ion Drift MeterLANG: Langmuir ProbeLAPI: Low Altitude Plasma InstrumentMAG-B: Magnetic Field Observations Triaxial Fluxgate MagnetometerNACS: Neutral Atmosphere Composition SpectrometerVEFI: Vector Electric Field InstrumentWATS: Wind and Temperature SpectrometerThe Instrument Data File Set. URL http://www.idfs.org 

Dynamics Explorer 2>MAGB> Magnetic Field Observations Triaxial Fluxgate Magnetometer 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_projected-magb-cdf/1981/de2_lapi_projected-magb_19810815130852_v01.cdf. The most common cadence, 500000000 [ns] = PT0.5S, occurred for all 2990 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri_spacecraft-magb-cdf/1981/de2_lapi_sc-magb_19810815034446_v01.cdf. The most common cadence, 62500000 [ns] = PT0.0625S, occurred for 99.9522% of the 23024 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri-shaft-encoder-angle-cdf/1981/de2_lapi_shaft-encoder-angle_19810815130902_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.8652% of the 741 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/particles_lapi/swri-shaft-encoder-angle-cdf/1981/de2_lapi_shaft-encoder-angle_19810815130902_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.8652% of the 741 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Nelson W. Spencer at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Nelson W. Spencer at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Nelson W. Spencer at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/neutral_gas_nacs/neutral1s_nacs_cdaweb/1981/de2_neutral1s_nacs_19810808_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 73.5756% of the 2531 timesteps. 

neutral gas 1 second (from all.xml/instrument/description/@short)

Neutral Atmosphere Composition Spectrometer (from Master/CDFglobalAttributes/Data_type)

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. R. Niciejewski at University of Michigan

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. R. Niciejewski at University of Michigan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. R. Niciejewski at University of Michigan

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/neutral_gas_fpi/de2_neutral8s_fpi/1981/de2_neutral8s_fpi_19810809_v01.cdf. The most common cadence, 8000 [ms] = PT8S, occurred for all 14 timesteps. 

neutral gas 8 second (from all.xml/instrument/description/@short)

Fabry-Perot Interferometer (from Master/CDFglobalAttributes/Data_type)

.5 sec electron temperature, plasma density, and satellite potential

DE-2 LANG 0.5-sec electron temperature, plasma density, and satellite potential

SPDF/CDAWeb. Please also acknowledge the data producer: Larry H. Brace at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Larry H. Brace at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Larry H. Brace at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_lang/plasma500ms_lang_cdaweb/1981/de2_plasma500ms_lang_19810805_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 75.1579% of the 357 timesteps. 

Langmuir Probe Instrument (from Master/CDFglobalAttributes/Data_type)

DE-2 UA 16-sec combined neutral and plasma unified abstract data

SPDF/CDAWeb. Please also acknowledge the data producer: Mr. Larry H. Brace at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Mr. Larry H. Brace at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Mr. Larry H. Brace at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/combined_plasma_neutrals_ua/ua16s_all_cdaweb/1981/de2_ua16s_all_19810806_v01.cdf. The most common cadence, 16000 [ms] = PT16S, occurred for 89.7959% of the 44 timesteps. 

Unified abstract 16 second (from all.xml/instrument/description/@short)

all instruments combined (from Master/CDFglobalAttributes/Data_type)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_velZ, @2 => Epoch_velY.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_velZ, @2 => Epoch_velY.)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_idm/vion250ms_cdaweb/1981/de2_vion250ms_idm_19810815_v01.cdf. The most common cadence, 8000 [ms] = PT8S, occurred for 93.9227% of the 170 timesteps. 

NSSDC standard-reference time value (ion velocity) Z direction. 

Counts based on variable 'Epoch_velZ' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_idm/vion250ms_cdaweb/1981/de2_vion250ms_idm_19810815_v01.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 49.9306% of the 1439 timesteps. 

Data quality flag for vi_z (0-1: good; 2-3: averaging recom.; 4-5: unreliable

NSSDC standard-reference time value (ion velocity) Y direction. 

Ion velocity in s/c y direction - vi_y - app. vertical (>0 upward)

Counts based on variable 'Epoch_velY' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/plasma_idm/vion250ms_cdaweb/1981/de2_vion250ms_idm_19810815_v01.cdf. The most common cadence, 16000 [ms] = PT16S, occurred for 87.7778% of the 79 timesteps. 

Data quality flag for vi_y (0-1: good; 2-3: averaging recom.; 4-5: unreliable

2-sec neutral densities, temperature, and horizontal (zonal) wind velocity

DE-2 WATS 2-sec Neutral Densities, Temperatures, and horizontal (zonal) wind velocities

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de2/neutral_gas_wats/wind2s_wats_cdaweb/1981/de2_wind2s_wats_19810808_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 43.2182% of the 513 timesteps. 

Wind and Temperature Spectrometer (from Master/CDFglobalAttributes/Data_type)

Mode = 3,4 measuring the horizontal velocity, =5,6 measuring the vertical velocity

Horizontal velocity in s/c coordinates (positive in the Z-axis direction)

-------------------> Vertical velocity (positive in the Y-axis direction)

Horizontal velocity in corotatingEarth frame (positive eastward)

Horizontal velocity in corotating Earth frame after WATSCOR correction

   Instrument functional description:        The spin-scan auroral imagers (SAI) comprise three photometers which   provide images of Earth at various wavelengths via interference filters   mounted on a wheel and selected by ground command.  Two of the photometers   provide visible wavelength images, and the third provides images at   vacuum-ultraviolet wavelengths.       The three photometers are mounted on the spacecraft such that their   fields of view are separated by about 120 degrees in a plane oriented   perpendicular to the spin axis.  Each photometer in operation collects   one scan line during each spacecraft rotation, with an internal mirror   stepping once per rotation to start a new scan line.       An auroral image is a nadir-centered two-dimensional pixel array   provided by the spacecraft rotation and the photometer's stepping mirror   which advances the field of view 0.25 degrees once per rotation in a   direction perpendicular to the plane of rotation.  A change in mirror-   stepping direction signals the start of a new image.  One, two, or   three photometers may be in operation at one time.  The images from all   operating photometers are telemetered simultaneously with image repetition   rates that typically vary from about 3 to 12 minutes.       One of the three imaging photometers is equipped with filters and a   photocathode for observations at vacuum-ultraviolet wavelengths, in   particular emissions of the Lyman-Birge-Hopfield band of molecular   nitrogen at about 140 to 170 nm.  Imaging at these wavelengths allows   coverage of the auroral oval in both the dark and sunlit ionospheres.   The filter array for the vacuum-ultraviolet imaging photometer also   includes filters for atomic hydrogen Lyman alpha at 121.6 nm and oxygen   lines at 130.4 and 135.6 nm.       The full width of the fields of view of the photometers   corresponding to a single pixel is 0.29 degrees.  An image frame   consists of all scan lines obtained by mirror steps in one direction   which deflect the field of view by 0.25 degrees per rotation.  The   angular separation of two consecutive pixels in the direction of   spacecraft rotation is about 0.23 degrees.  A full frame has 120   scan lines or 30 degrees of width.  For routine processing the   angular width along a scan line is 150 pixels, or about 34.5 degrees   of length.  The frame width is occasionally adjusted to less than   120 scan lines.     Reference:    Frank, L. A., J. D. Craven, K. L. Ackerson, M. R. English, R. H. Eather,       and R. L. Carovillano, Global auroral imaging instrumentation for       the Dynamics Explorer mission, Space Sci. Inst., 5, 369-393, 1981.     Data set description:        Each DE SAI UV image CDF contains all of images collected by the   UV photometer during one day of operations.  The displayable image   counts are in variable 3.       Coordinates are calculated for each position of the image count array.   These coordinates are in variables 14, 15, and 16.       To facilitate viewing of the images, a mapping of pixel value to a   recommended color table based on the characteristics of the selected   filter will be included with each image.  See the description of variables   17, 18, and 19 below.       A relative intensity scale is provided by the uncompressed count   table of variable 20.  Approximate intensity levels in kiloRayleighs are   given in the intensity table of variable 21.       Other variables provide orbit and attitude data and information about   the selected filter and the mirror stepping direction.   Variable descriptions:   1,2. Start time        The time assigned to an image is the start time of the initial scan        line within a resolution of one second.     3. Image counts        Image pixel counts range from 0 to 255.  They are stored in a two-        dimensional byte array of 121 columns by 150 rows.  Each column        contains one scan line.  Images will generally not fill all of the        121 columns.  When an image is displayed with row 1 at the top and        column 1 on the left, the spacecraft spin axis is oriented to the        left in the display, and the orbit normal vector is oriented to the        right.     4. Filter        Twelve filters are available for ultra-violet imaging; the filter        number, 1-12, is given here.  In addition, the peak wavelength in        Angstroms is given for the selected filter.     5. Presumed altitude of emissions        The presumed altitude of the emissions seen in the image varies        with the characteristics of the filter used.   6,7. First and last mirror location counters (MLCs)        The MLC range is from 28 in column 1 (leftmost) to 148 in column 121        (rightmost).  The direction of mirror stepping motion is shown by        comparing first and last MLCs.     8. Orbit/attitude time        Whenever possible, the approximate center time of the image is used        for determining the orbit and attitude parameters.  If O/A data is        not available for the center time, the closest available O/A time        is used.     9. Spacecraft position vector, GCI    10. Spacecraft velocity vector, GCI    11. Spacecraft spin axis unit vector, GCI    12. Sun position unit vector, GCI    13. Orbit normal unit vector, GCI    14. Geographic longitude or right ascension        East longitude is given for each image pixel on the Earth at the        altitude given in variable 5.  When the pixel altitude is greater        than the value of variable 5, the right ascension is given.    15. Geographic latitude or declination        North latitude is given for each image pixel on the Earth at the        altitude given in variable 5.  When the pixel altitude is greater        than the value of variable 5, the declination is given.    16. Pixel altitude        For each image pixel on the Earth, the presumed altitude of the        emissions is used.  This is equal to the value of variable 5.  For each        pixel off the Earth, the altitude of the line of sight is used.    17. Pixel UT        This array gives the start time for the collection of each image pixel.    18. RGB color table        This is the recommended color table to be used with the        limits given in variables 19 and 20. 19,20. Low and high color mapping limits        The low and high color limits are recommended for remapping        the color table entries, as follows:            For pixel values less than the low limit, use the color                at table position 1.            For pixel values greater than or equal to the low limit                and less than or equal to the high limit, use the color                at table position (pix-low)/(high-low) x 255 + 1.            For pixel values greater than the high limit, use the color                at table position 256.    21. Expanded count table        The image pixel counts are quasi-logarithmically compressed to the        range 0-255.  This table gives the average of the uncompressed range        for each compressed count value.  Table entries 1-128 correspond to        compressed counts 0-127 respectively.  Count levels greater than        127 are considered overflow.    22. Intensity table        For each of the twelve filters, approximate intensity levels in        kiloRayleighs are given for each compressed count value.  Table        entries 1-128 correspond to compressed counts 0-127 respectively.        No count conversion data is available for count levels greater than        127.     Supporting software:          Directions for obtaining supporting software is available on the SAI   website at the URL http://www-pi.physics.uiowa.edu/www/desai/software/.   Included is an IDL program that displays the images with the recommended   color bar and provides approximate intensities and coordinate data for   each pixel.

Dynamics Explorer Spin-Scan Auroral Imager ultraviolet camera images

SPDF/CDAWeb. Please also acknowledge the data producer: Louis A. Frank at The Univ. of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: Louis A. Frank at The Univ. of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Louis A. Frank at The Univ. of Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/images_sai/uv_sai_cdaweb/1981/de_uv_sai_19810923_v01.cdf. The most common cadence, 727224 [ms] = PT12M7.224S, occurred for 19.0476% of the 4 timesteps. 

Spin-Scan Auroral Imager (from all.xml/instrument/description/@short)

DE-1 Energetic Ion Composition Spectrometer (EICS), Validated Summary Data

SPDF/CDAWeb. Please also acknowledge the data producer: E. G. Shelley at Lockheed Martin

SPDF/SSCWeb. Please also acknowledge the data producer: E. G. Shelley at Lockheed Martin

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: E. G. Shelley at Lockheed Martin

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/de/de1/particles_eics/vs_eics_cdaweb/1981/81259_eics_de_96s_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 89.4737% of the 34 timesteps. 

Energetic Ion Composition Spectrometer (from all.xml/instrument/description/@short)

Validated Summary Data (from Master/CDFglobalAttributes/Data_type)

H+ number flux, at 15 energies (~0.01 to ~20keV) and 14 pitch angles (6 shown)

---> ONE Standard deviation of H+ number flux at 15 energy and 14 pitch angle bins.

O+ number flux, at 15 energies (~0.01 to ~20keV) and 14 pitch angles (6 shown)

---> ONE Standard deviation of O+ number flux at 15 energy and 14 pitch angle bins.

He+ number flux, at 15 energies (~0.01 to ~20keV) and 14 pitch angles (6 shown)

ONE Standard deviation of He+ number fluxat 15 energy and 14 pitch angle bins.

[PLOTTING NOT SUPPORTED] Combined Flags indicating mode and data quality

Bitwise combination of  He_data,N_flag, C_flag, A_flag, Noisy_flag, Short_flag, and PA_coverage_flag. scalar

---> Data valid flag 0=good; 1=Not available or use with caution

---> Sun Pulse Flag0=good; 1=use data from the lowest energy channel with caution. 

---> Attitude Available Flag 0: Source data CAN provide sensor orientation relative to the spacecraft velocity. 1: CAN NOT

---> Supplemental Data Valid Flag #1 0=good; 1= Telemetry interval contains unphysically high signal levels 

---> Supplemental Data Valid Flag #2 0=good; 1=Too short to evaluate data quality. 

---> Pitch Angle Coverage Flag 0=good; 1=Incomplete PA coverage.

Geographic Position Altitude above the geoid, latitude and longitude. 

Geomagnetic Position Magnetic local time, Invariant latitude and geomagnetic latitude. 

Precipitating electrons and ions observed at nominally 850km altitude and over a range of energies from 30 eV to 30 keV using the Special Sensor J (SSJ) instrument.  Please contact Rob.Redmon@noaa.gov with questions and comments. Many individuals made important contributions including: D. Hardy, E. Holeman, F. Rich, D. Ober, G. Wilson, J. Machuzak, K. Kadinsky-Cade, J. McGarity, W.F. Denig, K. Martin, R. Redmon, D. Knipp, L. Kilcommons.

Data access provided by NCEI in coordination with AFRL and CU Boulder.

Please acknowledge providers.  If you find problems, please report them.

SPDF/CDAWeb. Please also acknowledge the data producer: Staff at AFRL, NCEI, CU

SPDF/SSCWeb. Please also acknowledge the data producer: Staff at AFRL, NCEI, CU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Staff at AFRL, NCEI, CU

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf06/ssj/precipitating-electrons-ions/1987/dmsp-f06_ssj_precipitating-electrons-ions_19870101_v1.1.0.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

precipitating-electrons-ions (from Master/CDFglobalAttributes/Data_type)

Earth Centered Inertial (ECI) spacecraft location (x,y,z) in km.

Estimated uncertainty in electron differential energy flux (ev/cm2/delta-eV/ster/s).

Electron total energy flux integrated over energy (eV/cm2/ster/s).

Estimated uncertainty in electron total energy flux integrated over energy (eV/cm2/ster/s).

Estimated uncertainty in ion differential energy flux (ev/cm2/delta-eV/ster/s).

Estimated uncertainty in ion total energy flux integrated over energy (eV/cm2/ster/s).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf07/ssj/precipitating-electrons-ions/1987/dmsp-f07_ssj_precipitating-electrons-ions_19870101_v1.1.0.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf08/ssj/precipitating-electrons-ions/1987/dmsp-f08_ssj_precipitating-electrons-ions_19870625_v1.1.0.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf09/ssj/precipitating-electrons-ions/1988/dmsp-f09_ssj_precipitating-electrons-ions_19880324_v1.1.0.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf12/ssj/precipitating-electrons-ions/2000/dmsp-f12_ssj_precipitating-electrons-ions_20001228_v1.1.2.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Estimated relative uncertainty in electron differential energy flux (fractional).

Estimated relative uncertainty in electron total energy flux integrated over energy (fractional).

Estimated relative uncertainty in average electron energy (fractional).

Estimated relative uncertainty in ion differential energy flux (fractional).

Estimated relative uncertainty in ion total energy flux integrated over energy (fractional).

Estimated relative uncertainty in ion average energy (fractional).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf13/ssj/precipitating-electrons-ions/2000/dmsp-f13_ssj_precipitating-electrons-ions_20000101_v1.1.5.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf14/ssj/precipitating-electrons-ions/2000/dmsp-f14_ssj_precipitating-electrons-ions_20001228_v1.1.2.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf15/ssj/precipitating-electrons-ions/2000/dmsp-f15_ssj_precipitating-electrons-ions_20001228_v1.1.2.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

The Special Sensors-Ions, Electrons, and Scintillation (SSIES) thermal plasma analysis package is a suite of instruments built by the Center for Space Sciences at the University of Texas at Dallas and flown on a number of the DMSP satellites. SSIESS includes a Retarding Potential Analyzer (RPA), Ion Drift meter (IDM), scintillation meter, and Langmuir probe.

We gratefully acknowledge the University of Texas Dallas, Center for Space Sciences and the US Air Force for providing the DMSP thermal plasma data

SPDF/CDAWeb. Please also acknowledge the data producer: William Hanson, Rod Heelis, Marc Hairston at University of Texas Dallas, Center for Space Sciences

SPDF/SSCWeb. Please also acknowledge the data producer: William Hanson, Rod Heelis, Marc Hairston at University of Texas Dallas, Center for Space Sciences

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: William Hanson, Rod Heelis, Marc Hairston at University of Texas Dallas, Center for Space Sciences

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf16/ssies/ssies-3rl/thermal-plasma-cdf/2006/dmsp-f16_ssies-3_thermal-plasma_200601010048_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 99.9672% of the 6099 timesteps. 

Defense Meteorological Satellite Program (from all.xml/observatory/description/@short)

Special Sensors-Ions, Electrons, and Scintillation thermal plasma analysis package (from all.xml/instrument/description/@short)

Defense Meteorological Satellite Program (from Master/CDFglobalAttributes/Source_name)

electron background monitor - high energy particle currents detected by the RPA 

potential difference between SSIES instruments and spacecraft ground

potential of the SSIES instruments relative to the plasma ground

corotation velocity of ionosphere in the horizontal crosstrack direction 

NGDC Solar and Terrestrial Physics, STP, Satellite Data Services

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf16/ssj/precipitating-electrons-ions/2003/dmsp-f16_ssj_precipitating-electrons-ions_20031029_v1.1.2.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Electrons 30eV-30keV:  Electron counts as observed; no corrections.

-----> Estimated uncertainty in electron differential energy flux (fractional).

--> Electron total energy flux integrated over energy (eV/cm2/ster/s).

-----> Estimated uncertainty in electron total energy flux integrated over energy (fractional).

-----> Estimated uncertainty in electron average energy (fractional).

-----> Estimated uncertainty in ion differential energy flux (fractional).

--> Ion total energy flux integrated over energy (eV/cm2/ster/s).

-----> Estimated uncertainty in ion total energy flux integrated over energy (fractional).

-----> Estimated uncertainty in ion average energy (fractional).

Defense Meteorolgy Satellite Program F16 Vector Magnetometer Measurements (850km Altitude)

Data access provided by NGDC in coordination with AFRL and CU Boulder.

SPDF/CDAWeb. Please also acknowledge the data producer: Staff at AFRL, NGDC, CU

SPDF/SSCWeb. Please also acknowledge the data producer: Staff at AFRL, NGDC, CU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Staff at AFRL, NGDC, CU

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf16/ssm/magnetometer/2009/dmsp-f16_ssm_magnetometer_20090101_v1.0.5.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

delta-B (Original measured B - Modeled IGRF field) (x,y,z) in nT in spacecraft frame. 

Baseline Corrected delta-B in nT rotated into geocentric spherical (east-north-up) coordinates.

Baseline Corrected delta-B in nT rotated into Modified Apex Coordinates with Reference Height 110 km.

Numerical code for auroral region of spacecraft location (1=Equatorial,2=Auroral,3=Polar)

Integer representing the orbit of the day, signed by hemisphere (>0 Northern, <0 Southern).

Unit vector in the direction of spacecraft velocity (ram) in geocentric coordintes

Unit vector across the spacecraft track to the left ( orthogonal to the direction of spacecraft velocity (ram) ) in geocentric coordintes.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf17/ssies/ssies-3rl/thermal-plasma-cdf/2006/dmsp-f17_ssies-3_thermal-plasma_200611081733_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 99.9832% of the 5958 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf17/ssj/precipitating-electrons-ions/2009/dmsp-f17_ssj_precipitating-electrons-ions_20090101_v1.1.3.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Defense Meteorolgy Satellite Program F17 Vector Magnetometer Measurements (850km Altitude)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf17/ssm/magnetometer/2009/dmsp-f17_ssm_magnetometer_20090101_v1.0.5.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf18/ssies/ssies-3rl/thermal-plasma-cdf/2009/dmsp-f18_ssies-3_thermal-plasma_200910221631_v02.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 6118 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf18/ssj/precipitating-electrons-ions/2009/dmsp-f18_ssj_precipitating-electrons-ions_20091024_v1.1.2.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

Defense Meteorolgy Satellite Program F18 Vector Magnetometer Measurements (850km Altitude)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dmsp/dmspf18/ssm/magnetometer/2010/dmsp-f18_ssm_magnetometer_20100101_v1.0.4.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 93.4768% of the 80763 timesteps. 

The Johns Hopkins University Applied Physics Laboratory, Super Dual Auroral Radar Network, SuperDARN, Informational Web Site. The SuperDARN now consists of 32 Radars operating on Frequencies between 8 MHz and 20 MHz and looking into the Polar Regions of the Earth. These Radars can measure the Position and Velocity of Plasma Irregularities in the Earth's Ionosphere, the highest Layer of the Earth's Atmosphere. The Movements of these Irregularities respond to Energy coupled into the Auroral Regions from the Solar Wind and the Magnetosphere. Therefore, SuperDARN Data provides Scientists with Information regarding the Earth's Interaction with the Space Environment.

Canadian Super Dual Auroral Radar Network, SuperDARN, Informational Web Site

British Antarctic Survey, BAS, Super Dual Auroral Radar Network, SuperDARN, Informational Web Site

University of Leicester, Pykkvibaer Super Dual Auroral Radar Network, SuperDARN, Informational Web Site

Finnish Meteorological Institute, FMI, Scandinavian Twin Auroral Radar Experiment, STARE, Informational Web Site

Super Dual Auroral Radar Network, SuperDARN, Worldwide List of SuperDARN Observatories

SPDF/CDAWeb. Please also acknowledge the data producer: R. Greenwald at JHU/APL

SPDF/SSCWeb. Please also acknowledge the data producer: R. Greenwald at JHU/APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Greenwald at JHU/APL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/gbay/1999/dn_k0_gbay_19991104_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 96.8954% of the 593 timesteps. 

Dual Auroral Radar Network (from all.xml/observatory/description/@short)

Dual Auroral Radar Network (from Master/CDFglobalAttributes/Source_name)

Ionospheric Convection Velocity (east, north) at 30 geographic positions along scan

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/hank/1996/dn_k0_hank_19960701_v05.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 60.2257% of the 427 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/icew/1994/dn_k0_icew_19940828_v01.cdf. The most common cadence, 100000 [ms] = PT1M40S, occurred for 61.3072% of the 469 timesteps. 

Iceland West (Stokkseyri) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/kapu/1994/dn_k0_kapu_19940828_v01.cdf. The most common cadence, 100000 [ms] = PT1M40S, occurred for 84.0951% of the 460 timesteps. 

vlptm version 2.42Ref1: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME) to be submitted to Reviews of Geophysics (copy held by GGS group at NASA)Ref2:Baker et al.,EOS 70,p785 1989. Ref3: Greenwald et al.,Radio Sci.20,p63 1985Info:Keith Morrison,GGS Scientist,British AntarcticSurvey,Cambridge,CB3 0ET,UKE-mail: 19989::MORRISON

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/pace/1992/dn_k0_pace_19921204_v01.cdf. The most common cadence, 100000 [ms] = PT1M40S, occurred for 77.4629% of the 574 timesteps. 

Halley Station,Polar Anglo-American Conjugate Experiment (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/pykk/1996/dn_k0_pykk_19960701_v05.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 77.5264% of the 514 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/darn/sask/1994/dn_k0_sask_19940702_v01.cdf. The most common cadence, 100000 [ms] = PT1M40S, occurred for 64.3177% of the 575 timesteps. 

Magnetometer high-resolution data for the GOES-8 through GOES-17, (GOES I-M, GOES-NOP and GOES-R series of 10 spacecraft). The GOES MAG subsystem consists of fluxgate magnetometer instruments monitoring three orthogonal components of the geomagnetic field at geosynchronous orbit (L = 6.6) with high resolution sampling rate (G8-15: 2 Hz and G16-17: 10 Hz). The NetCDF product files include the magnetometer observations from the instrument(s) in several coordinate systems, and the satellite location calculated using a standard SGP/SDP orbit propagator. The field measurements are provided as B field vectors in the ECI (Earth-centered inertial), EPN (earthward, poleward, normal/eastward), GSE (geocentric solar ecliptic), GSM(geocentric solar magnetospheric) and VDH (dipole aligned) coordinate systems. For comprehensive documentation including caveats and usage recommendations, please consult the GOES magnetometer User's Guide at NCEI. 

GOES I-S (G08-G17) L2 Magnetometer (MAG) Geomagnetic Field 2 Hz Product with Complete Coordinate Frames

SPDF/CDAWeb. Please also acknowledge the data producer: Rob Redmon, Paul Loto'aniu, Howard Singer at DOC/NOAA/NCEI and DOC/NOAA/NWS/SWPC respectively

SPDF/SSCWeb. Please also acknowledge the data producer: Rob Redmon, Paul Loto'aniu, Howard Singer at DOC/NOAA/NCEI and DOC/NOAA/NWS/SWPC respectively

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Rob Redmon, Paul Loto'aniu, Howard Singer at DOC/NOAA/NCEI and DOC/NOAA/NWS/SWPC respectively

Magnetic field in EPN coordinates - E: earthward, P: perpendicular to the satellite orbital plane, N: ExP (eastward) 

Magnetic field in Earth Centered Inertial (ECI) coordinates (x, y, z)

Magnetic field in Geocentric Solar Ecliptic (GSE) coordinates (x, y, z)

Magnetic field in Geocentric Solar Magnetospheric (GSM) coordinates (x, y, z)

Magnetic field in VDH coordinates - V: anti-earthward, D: eastward, H: northward along dipole.

Magnetic field in Body Reference Frame (BRF) coordinates (spacecraft x=Roll, y=Pitch, z=Yaw). This is also the frame of the SEISS instrument.

Data quality flag (0 = good quality data). Note: CDF_UINT4 data was converted to HAPI double.

The GOES-R spacecraft includes a pair of boom-mounted fluxgate magnetometer instruments which operate simultaneously to obtain measurements of the geomagnetic field. The Magnetometer Subsystem supports the following mission objectives: 1) Map the space environment that controls charged particle dynamics in the outer region of the magnetosphere, 2) Measure the magnitude and direction of the Earth's ambient magnetic field in three orthogonal directions in the geosynchronous equatorial orbit, 3) Determine general level of geomagnetic activity, and 4) Detect magnetopause crossings, storm sudden commencements, and substorms. The product described in this file includes the magnetometer observations in several coordinate systems.

L2 Magnetometer (MAG) Geomagnetic Field 10 Hz Product with Complete Coordinate Frames

SPDF/CDAWeb. Please also acknowledge the data producer: Rob Redmon, Paul Loto'aniu at DOC/NOAA/NESDIS/NCEI/OGSSD/STP

SPDF/SSCWeb. Please also acknowledge the data producer: Rob Redmon, Paul Loto'aniu at DOC/NOAA/NESDIS/NCEI/OGSSD/STP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Rob Redmon, Paul Loto'aniu at DOC/NOAA/NESDIS/NCEI/OGSSD/STP

Total estimated ambient magnetic field computed from the ACRF frame.

Estimated ambient magnetic field in EPN coordinates (x, y, z). E: earthward, P: perpendicular to orbital plane, N: ExP.

Estimated ambient magnetic field in Earth Centered Inertial coordinates (x, y, z)

Estimated ambient magnetometer data in Geocentric Solar Ecliptic coordinates (x, y, z)

Estimated ambient magnetometer data in Geocentric Solar Magnetospheric coordinates (x, y, z)

Estimated ambient magnetometer data in VDH coordinates (x, y, z). V: anti-earthward, D: eastward, H: northward along dipole.

Estimated ambient magnetic field in Body Reference Frame coordinates (x, y, z). This frame orients the magnetometer to the SEISS.

Magnetometer L1b processing and data quality flags (0 = good quality data). Note: CDF_UINT4 data was converted to HAPI double.

GOES-19 Magnetometer L2 Geomagnetic Field 10 Hz Product with Complete Coordinate Frames

DSCOVR 3-axis stabilized definitive Attitude data file.5 second time resolutionConvention: intrinsic rotations applied in Yaw, Pitch, Roll orderExtended Kalman Filter applied to ground based solution during normal operations. OBC solution used during calibration maneuvers.

Deep Space Climate Observatory, DSCOVR, Web Page hosted by the National Environmental Satellite, Data, and Information Service, NESDIS, National Oceanic and Atmospheric Administration, NOAA

SPDF/CDAWeb. Please also acknowledge the data producer: A. Szabo at NASA Goddard Space Flight Center

SPDF/SSCWeb. Please also acknowledge the data producer: A. Szabo at NASA Goddard Space Flight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Szabo at NASA Goddard Space Flight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dscovr/orbit/def_at/2015/dscovr_at_def_20150211_v01.cdf. The most common cadence, 5000 [ms] = PT5S, occurred for all 505 timesteps. 

Deep Space Climate Observatory (from all.xml/observatory/description/@short)

Heliospheric Science (from Master/CDFglobalAttributes/Discipline)

Deep Space Climate Observatory (from Master/CDFglobalAttributes/Source_name)

DSCOVR 3-axis stabilized preliminary Attitude data file.Time resolution varies.Convention: intrinsic rotations applied in Yaw, Pitch, Roll order 5 point Median Filter applied to DCM matrix

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dscovr/orbit/pre_at/2015/dscovr_at_pre_20150211_v01.cdf. The most common cadence, 9998 [ms] = PT9.998S, occurred for 35.7564% of the 182 timesteps. 

DSCOVR Fluxgate Magnetometer 1-sec Definitive Data                              

SPDF/CDAWeb. Please also acknowledge the data producer: A. Koval at UMBC, NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: A. Koval at UMBC, NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Koval at UMBC, NASA/GSFC

Counts based on variable 'Epoch1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dscovr/h0/mag/2015/dscovr_h0_mag_20150608_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for all 86399 timesteps. 

1-sec Definitive Data (from Master/CDFglobalAttributes/Data_type)

Best fit parameters from nonlinear fitting of a single, isotropic Maxwellian velocity distribution function to sets of DSCOVR Faraday Cup measurements of the solar wind thermal proton peak. 1-minute resolution data are obtained by fitting to the 1-minute integrated distributions, comprising ~15 as-measured charged current spectra each. Reported uncertainties are fitting uncertainties, which do not account for so-called prior uncertainties associated with non-Maxwellian distributions in nature or with conditions that vary on timescales faster than 1 minute. The uncertainties associated with measurement of charged flux as a function of energy are propagated. Certain empirical corrections have been applied.

This research has made use of Deep Space Climate Observatory (DSCOVR) Faraday Cup experiment science data. These data are provided by the space plasma group at the Smithsonian Astrophysical Observatory under NASA Grant NNX17AC98G. The DSCOVR mission is a project of the U.S. National Oceanic and Atmospheric Administration.

Acknowledgement is kindly requested in publications and public presentations that make use of these data. Consulation with the instrument team is encouraged but not required.

SPDF/CDAWeb. Please also acknowledge the data producer: Justin C. Kasper at Smithonian Astrophysical Observatory

SPDF/SSCWeb. Please also acknowledge the data producer: Justin C. Kasper at Smithonian Astrophysical Observatory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Justin C. Kasper at Smithonian Astrophysical Observatory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dscovr/h1/faraday_cup/2016/dscovr_h1_fc_20160603_v02.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for 55.5942% of the 800 timesteps. 

Data Quality Flag: 0=good; 1=bad. Note: CDF_UINT4 data was converted to HAPI double.

Proton solar winds' most probable thermal speed. (w/o error bars)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/dscovr/orbit/pre_or/2015/dscovr_orbit_pre_20150211_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 20 timesteps. 

The DYNAMO-2 Dual Electrostatic Analyzer (DESA) instrument consisted of a single boom-mounted prototype sensor (DESA-NX-02A), and a main electronics box (MEB). The instrument was flown primarily as an engineering test flight of the DESA sensor and was only flown aboard the second of the two DYNAMO-2 rockets (35.357). The instrument had a single fixed field-of-view looking up towards space along the spin-axis of the rocket. For full details of the instrument, see Collinson et al., (2022). The instrument was configured as a low-energy photoelectron spectrometer.

Collinson, G. A., Glocer, A., Chornay, D., Michell, R., Pfaff, R., Cameron, T., et al. (2022). Rocket measurements of electron energy spectra from Earth's photoelectron production layer. Geophysical Research Letters, 49, e2022GL098209

SPDF/CDAWeb. Please also acknowledge the data producer: G. Collinson at NASA GSFC / Catholic University of America

SPDF/SSCWeb. Please also acknowledge the data producer: G. Collinson at NASA GSFC / Catholic University of America

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Collinson at NASA GSFC / Catholic University of America

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/dynamo2/cdf/dynamo-2_desa_nx02a-esa-flux_20210711_v01.cdf. The most common cadence, 9000 [ms] = PT9S, occurred for 71.4286% of the 15 timesteps. 

Dual Electrostatic Analyzer NX-02A (from Master/CDFglobalAttributes/Data_type)

Time/energy spectrogram of raw counts of electrons from the single detector of the DESA-NX-02A sensor

Time/energy spectrogram of Differential Energy Flux of electrons

Time/energy spectrogram of Differential Energy Flux of electrons,corrected for the potential of the spacecraft from active pulses of the DYNAMO-2 Langmuir Probe.

Altitude above sea level during operation of the DYNAMO-2 DESA-NX-02A instrument

Latitude during operation of the DYNAMO-2 DESA-NX-02A Instrument

Geographic Longitude during operation of the DYNAMO-2 DESA-NX-02A Instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/earth_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/earth_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

Energetic Particle Detector, Counts, Electrons>keV [UNCALIBRATED RAW DATA] 

The Electron Losses and Fields Investigation (ELFIN) mission is a space weather mission using three scientific instruments in a 3U+ CubeSat. The instruments measure wave and particle data.

Electron Losses and Fields INvestigation-A twin satellite mission

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos at UCLA, IGPP/EPSS

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos at UCLA, IGPP/EPSS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos at UCLA, IGPP/EPSS

Counts based on variable 'ela_pef_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfina/l1/fast/electron/2018/ela_l1_epdef_20181214_v01.cdf. The most common cadence, 203125000 [ns] = PT0.203125S, occurred for all 15 timesteps. 

Electron Losses and Fields INvestigation-A (from all.xml/observatory/description/@short)

Electron Losses and Fields INvestigation-A (from Master/CDFglobalAttributes/Source_name)

Energetic Particle Detector, Counts, Ions>keV [UNCALIBRATED RAW DATA] 

Counts based on variable 'ela_pif_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfina/l1/fast/ion/2018/ela_l1_epdif_20181214_v01.cdf. The most common cadence, 203906000 [ns] = PT0.203906S, occurred for 31.5789% of the 30 timesteps. 

ELFIN-A state file, contains definitive position, attitude and orbit events

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => ela_state_time, @1 => ela_att_time.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => ela_state_time, @1 => ela_att_time.)

Counts based on variable 'ela_state_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfina/ephemeris/defn/2018/ela_l1_state_defn_20180916_v02.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

ELFIN-A state file, contains predictive position, velocity, and attitude

Counts based on variable 'ela_state_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfina/ephemeris/pred/2018/ela_l1_state_pred_20180917_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86400 timesteps. 

Counts based on variable 'elb_pef_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfinb/l1/fast/electron/2019/elb_l1_epdef_20190522_v01.cdf. The most common cadence, 375781000 [ns] = PT0.375781S, occurred for 48.4359% of the 480 timesteps. 

Electron Losses and Fields INvestigation-B (from all.xml/observatory/description/@short)

Electron Losses and Fields INvestigation-B (from Master/CDFglobalAttributes/Source_name)

[ADC UNITS ONLY] L1 EPD Electron counts, Fast Mode - all 16 energies

[UNCALIBRATED RAW DATA ONLY] Energetic Partical Detector Energy Particles, Ions>keV 

Counts based on variable 'elb_pif_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfinb/l1/fast/ion/2019/elb_l1_epdif_20190522_v01.cdf. The most common cadence, 375781000 [ns] = PT0.375781S, occurred for 47.5059% of the 600 timesteps. 

ELFIN-B state file, contains definitive position, attitude and orbit events

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => elb_state_time, @1 => elb_att_time.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => elb_state_time, @1 => elb_att_time.)

Counts based on variable 'elb_state_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfinb/ephemeris/defn/2018/elb_l1_state_defn_20180916_v02.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

ELFIN-B state file, contains predictive position, velocity, and attitude

Counts based on variable 'elb_state_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/elfin/elfinb/ephemeris/pred/2018/elb_l1_state_pred_20180917_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86400 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_ephemeris_def_20220511_v01.cdf. The most common cadence, 19989000 [ns] = PT0.019989S, occurred for 22.0244% of the 9722 timesteps. 

Endurance GPS Velocity, Position, Altitude, and Magnetic Latitude and Longitude

Data from the GPS receiver aboard Endurance plus a conversion of the coordinates into magnetic latitude and longitude

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_ephemeris_gps_20220511_v01.cdf. The most common cadence, 50 [ms] = PT0.05S, occurred for 99.7980% of the 17789 timesteps. 

TM1 electric field sphere potential (skins) voltages from Endurance FIELDS experiment during flight.

SPDF/CDAWeb. Please also acknowledge the data producer: R. Pfaff at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: R. Pfaff at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Pfaff at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_fields_skinpot-500us_20220511_v01.cdf. The most common cadence, 500000 [ns] = PT0.000500000S, occurred for 54.7595% of the 876863 timesteps. 

Calibrated electric field probe voltages (from Master/CDFglobalAttributes/Data_type)

TM1 electric field sphere differential voltages from Endurance FIELDS experiment during flight.

SPDF/CDAWeb. Please also acknowledge the data producer: G. Collinson at NASA GSFC / Catholic University

SPDF/SSCWeb. Please also acknowledge the data producer: G. Collinson at NASA GSFC / Catholic University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Collinson at NASA GSFC / Catholic University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/2022/endurance_fields_vlf-33us_20220511_v01.cdf. The most common cadence, 33334 [ns] = PT0.000033334S, occurred for 32.9945% of the 8886751 timesteps.

Level 1a PES Science and Housekeeping data at 40ms time resolution as downlinked in the Data Matrix

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l1a_pes_20220511_v01.cdf. The most common cadence, 4003200 [ns] = PT0.004003S, occurred for 60.1932% of the 138501 timesteps. 

Photoelectron Spectrometer (from all.xml/instrument/description/@short)

Uncalibrated L1b raw counts per energy step from the 8 DESA sensors during science portion of mission

The Endurance PES instrument was comprised of 8 boom-mounted Dual Electrostatic Analyzer (DESA) sensors, and a main electronics box (MEB). Each DESA sensor had two look directions; A-side (looking down to Earth from launch to pitch-over maneuver, and then up to space until loss of signal (LOS)); and B-side (looking up to space from launch to pitch-over, and then down to Earth until loss of signal (LOS)). The sensors were synchronized by the MEB and cross-calibrated to look at approximately the same energy at the same time. A PES sweep consisted of 81 different steps and took 10 seconds. At each step, a voltage could be applied to the Electrostatic Analyzer (ESA) and/or the Retarding Potential Analyzer (RPA). Of these 81 steps; 3 (0, 1, 44) were used to take background counts with the ESA grounded, and to fire the SLP; 34 (2:9, 33, 56:80) were used to collect the standard resolution data measurement (15% DE/E, 10eV to 1keV) using the ESA alone; and 44 (10:32, 34:43, 45:55) were used to collect the high-resolution measurement (0.5% DE/E, 20.3 eV to 25.85 eV) using the ESA and RPA combined.”

Collinson, G., Glocer, A., Pfaff, R. et al. The Endurance Rocket Mission. Space Sci Rev 218, 39 (2022). https://doi.org/10.1007/s11214-022-00908-0

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l1b_pes_20220511_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 94.8052% of the 73 timesteps. 

The Endurance PES instrument was comprised of 8 boom-mounted Dual Electrostatic Analyzer (DESA) sensors, and a main electronics box (MEB). Each DESA sensor had two look directions; A-side (looking down to Earth from launch to pitch-over maneuver, and then up to space until loss of signal (LOS)); and B-side (looking up to space from launch to pitch-over, and then down to Earth until loss of signal (LOS)). The sensors were synchronized by the MEB and cross-calibrated to look at approximately the same energy at the same time. These data present the standard resolution data measurement (15% DE/E, 10eV to 1keV) using the ESA alone, using counts from all the sensors combined together.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l2-esa_pes_20220511_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 94.8052% of the 73 timesteps. 

Level 2 Electrostatic Analyzer Mode (Standard Resolution) (from Master/CDFglobalAttributes/Data_type)

Time/energy spectrogram of Differential Energy Flux of electrons from the 8 combined A-sides of PES

Time/energy spectrogram of Differential Energy Flux of electrons from the 8 combined B-sides of PES

The Endurance PES instrument was comprised of 8 boom-mounted Dual Electrostatic Analyzer (DESA) sensors, and a main electronics box (MEB). Each DESA sensor had two look directions; A-side (looking down to Earth from launch to pitch-over maneuver, and then up to space until loss of signal (LOS)); and B-side (looking up to space from launch to pitch-over, and then down to Earth until loss of signal (LOS)). The sensors were synchronized by the MEB and cross-calibrated to look at approximately the same energy at the same time. A PES sweep consisted of 81 different steps and took 10 seconds. At each step, a voltage could be applied to the Electrostatic Analyzer (ESA) and/or the Retarding Potential Analyzer (RPA). Of these 81 steps; 3 (0, 1, 44) were used to take background counts with the ESA grounded, and to fire the SLP; 34 (2:9, 33, 56:80) were used to collect the standard resolution data measurement (15% DE/E, 10eV to 1keV) using the ESA alone; and 44 (10:32, 34:43, 45:55) were used to collect the high-resolution measurement (0.5% DE/E, 20.3 eV to 25.85 eV) using the ESA and RPA combined. These calibration data present the variation in Geometric Factor with PES operation during flight

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l2-gf_pes_20220511_v01.cdf. The most common cadence, 136 [ms] = PT0.136S, occurred for 88.0323% of the 5561 timesteps. 

Level 2 Geometric Factor Time Series (from Master/CDFglobalAttributes/Data_type)

Variation of geometric factor of PES all sensors, A-side during operation

Variation of geometric factor of PES all sensors, B-side during operation

The Endurance PES instrument was comprised of 8 boom-mounted Dual Electrostatic Analyzer (DESA) sensors, and a main electronics box (MEB). Each DESA sensor had two look directions; A-side (looking down to Earth from launch to pitch-over maneuver, and then up to space until loss of signal (LOS)); and B-side (looking up to space from launch to pitch-over, and then down to Earth until loss of signal (LOS)). The sensors were synchronized by the MEB and cross-calibrated to look at approximately the same energy at the same time. These data present the high-resolution measurement (0.5% DE/E, 20.3 eV to 25.85 eV) using the ESA and RPA counts from all the sensors combined together

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l2-rpa_pes_20220511_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 94.8052% of the 73 timesteps. 

Level 2 Retarding Potential Analyzer Mode (High Resolution (from Master/CDFglobalAttributes/Data_type)

High resolution Time/energy spectrogram of Differential Energy Flux of electrons from the 8 combined A-sides of PES. Uncorrected for Spacecraft Potential

High resolution Time/energy spectrogram of Differential Energy Flux of electrons from the 8 combined B-sides of PES. Uncorrected for Spacecraft Potential

High resolution Time/energy spectrogram of Differential Energy Flux of electrons from the 8 combined A-sides of PES. Corrected for Spacecraft Potential

High resolution Time/energy spectrogram of Differential Energy Flux of electrons from the 8 combined B-sides of PES. Corrected for Spacecraft Potential

Calibrated L2 thermal plasma measurements from the Sweeping Langmuir Probe (SLP)

The Endurance SLP was a needle probe mounted on the forward Fo’c’sle of the spacecraft. It measured thermal plasma density, electron temperature, the potential difference between the spacecraft and ambient plasma (plasma potential) and the relative potential of the spacecraft. SLP performed an active (20ms) sweep once every 5 seconds, wherein a sweeping +/- 5V voltage was applied to the needle. The data products here were derived from the I-V curves and intercalibrated with EISCAT Radar and the PES instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: A. Barjatya at Embry Riddle Aeronautical University

SPDF/SSCWeb. Please also acknowledge the data producer: A. Barjatya at Embry Riddle Aeronautical University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Barjatya at Embry Riddle Aeronautical University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l2_slp_20220511_v01.cdf. The most common cadence, 5116 [ms] = PT5.116S, occurred for 44.2953% of the 66 timesteps. 

Swept Langmuir Probe (SLP) Calibrated (L2) Data (from all.xml/instrument/description/@short)

Thermal Plasma (Electron & Ion) Density in particles per cubic centimeter

The Sweeping Langmuir Probe is a traditional Langmuir probe with a sweep voltage of +/-5V is applied to a gold plated cylinder.  Besides generating I-V curves to derive electron temperature, ion and electron density and spacecraft floating potential, spectra were obtained with a duty cycle of once per 5 seconds.

The Endurance Rocket Mission, Guaging Earth's Ambipolar Electric Potential

Collinson, G., Glocer, A., Pfaff, R., et al. 2022, Space Science Reviews, 218, 39.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/2022/endurance_l2_slp_psd_20220511_v01.cdf. The most common cadence, 4880000000 [ns] = PT4.88S, occurred for 43.9189% of the 65 timesteps.

Calibrated SLP spectra (from Master/CDFglobalAttributes/Data_type)

Electric Potential Drop parallel to Earth’s magnetic Field below Endurance

The Endurance mission was designed to make the first measurement of Earth’s electric potential. This Level 3 data product is the potential drop below Endurance as measured from the shift in the peak of the N2 A2 Πu  He-II photopeak, corrected for spacecraft potential by the Swept Langmuir Probe. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/endurance/endurance-2022/cdf/endurance_l3_pes_20220511_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 84.3750% of the 54 timesteps. 

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.8 AUX

SPDF/CDAWeb. Please also acknowledge the data producer:  EDC at MPE

SPDF/SSCWeb. Please also acknowledge the data producer:  EDC at MPE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer:  EDC at MPE

Counts based on variable 'Epoch%eq_pp_aux' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/equator-s/pp/aux/1997/eq_pp_aux_19971216_v01.cdf. The most common cadence, 1487 [ms] = PT1.487S, occurred for 89.7841% of the 17507 timesteps. 

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.2 EDI

Counts based on variable 'Epoch%eq_pp_edi' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/equator-s/pp/edi/1998/eq_pp_edi_19980325_v01.cdf. The most common cadence, 8000 [ms] = PT8S, occurred for 17.6955% of the 43 timesteps. 

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.5 EPI

SPDF/CDAWeb. Please also acknowledge the data producer: T. Sanderson at ESTEC

SPDF/SSCWeb. Please also acknowledge the data producer: T. Sanderson at ESTEC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. Sanderson at ESTEC

Energetic Particle Instrument (from all.xml/instrument/description/@short)

Equator-S Ion Composition Instrument Prime Parameters.(The raw moments calculated onboard should only be used qualitatively for identifying regions and temporal variations. Quantitative analysis should be done with the final moments generated from telemetered 3D distributions.)

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.3 ICI

Energy spectrograms, pitch angle distributions, moments and mass spectra

SPDF/CDAWeb. Please also acknowledge the data producer: L. Kistler at UNH

SPDF/SSCWeb. Please also acknowledge the data producer: L. Kistler at UNH

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: L. Kistler at UNH

Counts based on variable 'Epoch%eq_pp_ici' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/equator-s/pp/ici/1998/eq_pp_ici_19980121_v03.cdf. The most common cadence, 1490 [ms] = PT1.49S, occurred for 84.7007% of the 11986 timesteps. 

Equator-S Ion Spectrometry (from all.xml/instrument/description/@short)

ICI status flags for operational modes, data compression, scalar ([0]: 0=bad,1=caution,2=OK)

Final proton temperature tensor (3d), 1 parallel and 2 perpendicular GSE components

Final oxygen+ temperature tensor (3d), 1 parallel and 2 perpendicular GSE components

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.1 MAM

SPDF/CDAWeb. Please also acknowledge the data producer: W. Baumjohann at MPE

SPDF/SSCWeb. Please also acknowledge the data producer: W. Baumjohann at MPE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: W. Baumjohann at MPE

Counts based on variable 'Epoch%eq_pp_mam' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/equator-s/pp/mam/1997/eq_pp_mam_19971216_v02.cdf. The most common cadence, 1487 [ms] = PT1.487S, occurred for 89.6829% of the 17481 timesteps. 

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.6 PCD

SPDF/CDAWeb. Please also acknowledge the data producer: K. Torkar at IWF

SPDF/SSCWeb. Please also acknowledge the data producer: K. Torkar at IWF

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Torkar at IWF

Potential Control Device (from all.xml/instrument/description/@short)

see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.7 SFD

SPDF/CDAWeb. Please also acknowledge the data producer: L. Adams at ESTEC

SPDF/SSCWeb. Please also acknowledge the data producer: L. Adams at ESTEC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: L. Adams at ESTEC

Counts based on variable 'Epoch%eq_sp_sfd' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/equator-s/sp/sfd/1997/eq_sp_sfd_19971216_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 98.7097% of the 459 timesteps. 

Scintillating Fibre Detector (from all.xml/instrument/description/@short)

High-energy electron experiments (HEP) Level-2 omni flux data, ARASE/ERG)

Level-2 omni flux data obtained by the High-energy electron experiments (HEP) instrument onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Takefumi Mitani at ISAS, JAXA

SPDF/SSCWeb. Please also acknowledge the data producer: Takefumi Mitani at ISAS, JAXA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Takefumi Mitani at ISAS, JAXA

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_H, @1 => Epoch_L.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_H, @1 => Epoch_L.)

Inner Magnetosphere (from all.xml/observatory/description/@short)

High-energy electron experiments (from all.xml/instrument/description/@short)

Inner Magnetosphere (from Master/CDFglobalAttributes/Source_name)

HEP Level-2 omni flux data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/hep/l2/omniflux/2017/erg_hep_l2_omniflux_20170320_v02_00.cdf. The most common cadence, 7984460000 [ns] = PT7.98446S, occurred for 16.0363% of the 1734 timesteps. 

Counts based on variable 'Epoch_L' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/hep/l2/omniflux/2017/erg_hep_l2_omniflux_20170320_v02_00.cdf. The most common cadence, 7984460000 [ns] = PT7.98446S, occurred for 16.8794% of the 1825 timesteps. 

Low-Energy Particle experiments - electron analyzer (LEP-e) Level 2 omni electron flux data, ARASE/ERG

Level 2 electron omni flux data obtained by the Low-Energy Particle experiments - electron analyzer (LEP-e) onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Shiang-Yu Wang at Academia Sinica, Taiwan

SPDF/SSCWeb. Please also acknowledge the data producer: Shiang-Yu Wang at Academia Sinica, Taiwan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Shiang-Yu Wang at Academia Sinica, Taiwan

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/lepe/l2/omniflux/2018/erg_lepe_l2_omniflux_20180301_v04_01.cdf. The most common cadence, 8000118000 [ns] = PT8.000118S, occurred for 9.7165% of the 778 timesteps. 

Low-Energy Particle experiments - electron analyzer (from all.xml/instrument/description/@short)

LEPe level 2 electron omni flux (from Master/CDFglobalAttributes/Data_type)

Exploration of Low Energy Particle Ion (LEPi) Experiment 3D ion flux data, ARASE/ERG

Level 2 Omni ion flux data obtained by the Low Energy Particle Ion (LEPi) Experiment instrument onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Kazushi Asamura at ISAS, Jaxa

SPDF/SSCWeb. Please also acknowledge the data producer: Kazushi Asamura at ISAS, Jaxa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Kazushi Asamura at ISAS, Jaxa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/lepi/l2/omniflux/2017/erg_lepi_l2_omniflux_20170401_v03_00.cdf. The most common cadence, 31969000000 [ns] = PT31.969S, occurred for 22.8843% of the 795 timesteps. 

Low Energy Particle Ion experiment (from all.xml/instrument/description/@short)

LEPi level 2 3D ion omniflux data (from Master/CDFglobalAttributes/Data_type)

Exploration of Energization and Radiation in Geospace (ERG) Medium-Energy Particle experiments - electron analyzer (MEP-e) Level 2 3D electron flux data

Level 2 3D electron flux data obtained by the Medium-Energy Particle experiments - electron analyzer (MEP-e) onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Satoshi Kasahara at The University of Tokyo

SPDF/SSCWeb. Please also acknowledge the data producer: Satoshi Kasahara at The University of Tokyo

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Satoshi Kasahara at The University of Tokyo

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch, @1 => epoch_sp.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch, @1 => epoch_sp.)

Medium-Energy Particle experiments - electron analyzer (from all.xml/instrument/description/@short)

MEP-e level 2 3D electron flux data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mepe/l2/3dflux/2017/erg_mepe_l2_3dflux_20170323_v01_01.cdf. The most common cadence, 7984470000 [ns] = PT7.98447S, occurred for 28.5061% of the 2803 timesteps. 

[WILL NOT PLOT] Unidirectional Differential Electron Flux (before noise correction)

---> 73 keV Unidirectional differential electron flux (before noise correction)

---> 35 keV Unidirectional differential electron flux (before noise correction)

---> 17 keV Unidirectional differential electron flux (before noise correction)

---> 8.4 keV Unidirectional differential electron flux (before noise correction)

[WILL NOT PLOT] Unidirectional Differential Electron Energy Flux

Time for each spin sector, corresponding to middle of each spin sector

Counts based on variable 'epoch_sp' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mepe/l2/3dflux/2017/erg_mepe_l2_3dflux_20170323_v01_01.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 59.6364% of the 187668 timesteps. 

Medium Energy Particle experiments - electron analyzer (MEP-e) electron omni flux data, ARASE/ERG

Level 2 electron omni flux data obtained by the Medium Energy Particle experiments - electron analyzer (MEP-e) onboard the ERG satellite

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mepe/l2/omniflux/2017/erg_mepe_l2_omniflux_20170323_v01_02.cdf. The most common cadence, 7984470016 [ns] = PT7.98447S, occurred for 21.5601% of the 2120 timesteps. 

Medium Energy Particle experiments - electron analyzer (from all.xml/instrument/description/@short)

MEP-e level 2 electron omni flux (from Master/CDFglobalAttributes/Data_type)

Exploration of Energization and Radiation in Geospace (ERG) Medium Energy Particle experiments - ion mass analyzer (MEP-i) Level-2 3D flux data

Level 2 3D ion flux data obtained by the Medium Energy Particle experiments - ion mass analyzer (MEP-i) onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Shoichiro Yokota at Osaka University

SPDF/SSCWeb. Please also acknowledge the data producer: Shoichiro Yokota at Osaka University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Shoichiro Yokota at Osaka University

Medium Energy Particle experiments - ion mass analyzer (from all.xml/instrument/description/@short)

MEP-i level 2 3D ion flux data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mepi/l2/3dflux/2017/erg_mepi_l2_3dflux_20170324_v01_03.cdf. The most common cadence, 15984560000 [ns] = PT15.98456S, occurred for 40.6455% of the 869 timesteps. 

[CDAWeb plots not supported] Unidirectional differential proton flux

[CDAWeb plots not supported] Unidirectional differential proton energy flux

[CDAWeb plots not supported] Unidirectional differential He++ flux

[CDAWeb plots not supported] Unidirectional differential He++ energy flux

[CDAWeb plots not supported] Unidirectional differential He+ flux

[CDAWeb plots not supported] Unidirectional differential He+ energy flux

[CDAWeb plots not supported] Unidirectional differential O++ flux

[CDAWeb plots not supported] Unidirectional differential O++ energy flux

[CDAWeb plots not supported] Unidirectional differential O+ flux

[CDAWeb plots not supported] Unidirectional differential O+ energy flux

[CDAWeb plots not supported] Unidirectional differential O2+ flux

[CDAWeb plots not supported] Unidirectional differential O2+ energy flux

Counts based on variable 'epoch_sp' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mepi/l2/3dflux/2017/erg_mepi_l2_3dflux_20170324_v01_03.cdf. The most common cadence, 500010000 [ns] = PT0.50001S, occurred for 47.5178% of the 16262 timesteps. 

Medium Energy Particle experiments - ion mass analyzer (MEP-i) 3D ion omni flux data, ARASE/ERG

Level 2 3D ion omni flux data obtained by the Medium Energy Particle experiments - ion mass analyzer (MEP-i) instrument onboard the ERG satellite

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mepi/l2/omniflux/2017/erg_mepi_l2_omniflux_20170324_v02_01.cdf. The most common cadence, 15984560013 [ns] = PT15.98456S, occurred for 15.3414% of the 328 timesteps. 

MEPi level 2 3D ion omniflux data (from Master/CDFglobalAttributes/Data_type)

Magnetic Field Experiment (MGF) Level 2 spin-averaged magnetic field data, ARASE/ERG

Level 2 magnetic field data obtained by the Magnetic Field Experiment (MGF) instrument onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Ayako Matsuoka at Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan

SPDF/SSCWeb. Please also acknowledge the data producer: Ayako Matsuoka at Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Ayako Matsuoka at Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan

Counts based on variable 'epoch_8sec' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/mgf/l2/8sec/2017/erg_mgf_l2_8sec_20170313_v03.04.cdf. The most common cadence, 7995264000 [ns] = PT7.995264S, occurred for 3.8041% of the 202 timesteps. 

Magnetic Field Experiment (from all.xml/instrument/description/@short)

level 2 spin-averaged magnetic field data (from Master/CDFglobalAttributes/Data_type)

Exploration of Energization and Radiation in Geospace (ERG) Level-2 orbit data

SPDF/CDAWeb. Please also acknowledge the data producer:  at JAXA/ISAS

SPDF/SSCWeb. Please also acknowledge the data producer:  at JAXA/ISAS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer:  at JAXA/ISAS

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/orb/l2/2016/erg_orb_l2_20161022_v04.cdf. The most common cadence, 6000000000 [ns] = PT6S, occurred for all 13997 timesteps. 

R, magnetic latitude, and magnetic local time of spacecraft positions (using IGRF model)

Spacecraft positions mapped onto the magnetic equator (using IGRF model)

Geographic latidue and longitude of spacecraft footprints at 100 km in the northern hemisphere (using IGRF model)

Geographic latidue and longitude of spacecraft footprints at 100 km in the southern hemisphere (using IGRF model)

Magnetic field strength at spacecraft positions, using IGRF model

Magnetic field at spacecraft positions mapped onto the magnetic equator , using  IGRF model

Magnetic field strength at spacecraft positions mapped onto the magnetic equator , using  IGRF model

Exploration of Energization and Radiation in Geospace (ERG) Level-2 long-term predicted orbit data

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/orb/lpre/l2/2018/erg_orb_lpre_l2_20180101_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 1440 timesteps. 

Level-2 predicted orbit data (from Master/CDFglobalAttributes/Data_type)

Exploration of Energization and Radiation in Geospace (ERG) Level-2 medium-term predicted orbit data

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/orb/mpre/l2/2017/erg_orb_mpre_l2_20171205_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 1440 timesteps. 

Exploration of Energization and Radiation in Geospace (ERG) Level-2 predicted orbit data

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/orb/pre/l2/2016/erg_orb_pre_l2_20161220_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 1440 timesteps. 

Exploration of Energization and Radiation in Geospace (ERG) Level-2 short-term predicted orbit data

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/orb/spre/l2/2016/erg_orb_spre_l2_20161220_v02.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 1440 timesteps. 

Plasma Wave Experiment (PWE) Electric Field Detector (EFD) Level 2 spectrum data, ARASE/ERG

Level 2 plasma wave electromagnetic field data obtained by the Plasma Wave Experiment (PWE) instrument onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Yoshiya Kasahara at Kanazawa University

SPDF/SSCWeb. Please also acknowledge the data producer: Yoshiya Kasahara at Kanazawa University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Yoshiya Kasahara at Kanazawa University

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_spb.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_spb.)

Plasma Wave Experiment (from all.xml/instrument/description/@short)

level 2 plasma wave experiment data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/pwe/efd/l2/e_spin/2017/erg_pwe_efd_l2_e_spin_20170303_v04_01.cdf. The most common cadence, 7992187500 [ns] = PT7.992188S, occurred for 59.2239% of the 6395 timesteps. 

quality flag for EFD. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'Epoch_spb' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/pwe/efd/l2/e_spin/2017/erg_pwe_efd_l2_e_spin_20170303_v04_01.cdf. The most common cadence, 7984459877 [ns] = PT7.98446S, occurred for 5.8780% of the 635 timesteps. 

Plasma Wave Experiment (PWE) Electric Field Detector (EFD) Level 2 potential data, ARASE/ERG

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/pwe/efd/l2/pot/2017/erg_pwe_efd_l2_pot_20170323_v03_02.cdf. The most common cadence, 7984467030 [ns] = PT7.984467S, occurred for 13.0551% of the 1411 timesteps. 

No HAPI parameter information available to generate Parameter list.

Plasma Wave Experiment (PWE) Onboard Frequency Analyzer (OFA) Level 2 spectrum data, ARASE/ERG

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_e132, @1 => epoch_b132.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_e132, @1 => epoch_b132.)

Counts based on variable 'epoch_e132' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/pwe/ofa/l2/spec/2017/erg_pwe_ofa_l2_spec_20170323_v02_03.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 86.8064% of the 74999 timesteps. 

Counts based on variable 'epoch_b132' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/pwe/ofa/l2/spec/2017/erg_pwe_ofa_l2_spec_20170323_v02_03.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 85.6293% of the 73982 timesteps. 

Exploration of Energization and Radiation in Geospace (ERG) Extremely High-Energy Electron Experiment (XEP) Level 2 extremely high energy electron data

Level 2 extremely high energy electron data obtained by the Extremely High-Energy Electron Experiment (XEP) onboard the ERG satellite

SPDF/CDAWeb. Please also acknowledge the data producer: Nana Higashio at Space Environment Group, Aerospace Research and Development Directorate, Tsukuba Space Center, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan

SPDF/SSCWeb. Please also acknowledge the data producer: Nana Higashio at Space Environment Group, Aerospace Research and Development Directorate, Tsukuba Space Center, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Nana Higashio at Space Environment Group, Aerospace Research and Development Directorate, Tsukuba Space Center, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/erg/xep/l2/omniflux/2017/erg_xep_l2_omniflux_20170319_v00_00.cdf. The most common cadence, 7984462000 [ns] = PT7.984462S, occurred for 34.1229% of the 3688 timesteps. 

Extremely High-Energy Electron Experiment (from all.xml/instrument/description/@short)

level 2 extremely high energy electron data (from Master/CDFglobalAttributes/Data_type)

Calibrated fluxgate magnetometer data acquired by the Fast Auroral SnapshoT Small Explorer (FAST). Data have been calibrated, despun, and detrended against the International Geomagnetic Reference Field (IGRF), using IGRF coefficients for the date of acquisition. Data are provided in several coordinate systems. Non detrended data in spacecraft and Geocentric Equatorial Inertial coordinates are also provided. Ephemeris data are provided.

Elphic, R. C., J. D. Means, R. C. Snare, R. J. Strangeway, L. Kepko, and R. E. Ergun, Magnetic field instruments for the Fast Auroral Snapshot Explorer, Space Sci. Rev., 98, 151-168, 2001.

FAST Fluxgate Magnetometer Instrument Description Space Science Review Paper

SPDF/CDAWeb. Please also acknowledge the data producer: Robert Strangeway at UCLA

SPDF/SSCWeb. Please also acknowledge the data producer: Robert Strangeway at UCLA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Robert Strangeway at UCLA

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Spin_Epoch, @2 => Ephemeris_Epoch, @3 => Orbit_Fixed_Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Spin_Epoch, @2 => Ephemeris_Epoch, @3 => Orbit_Fixed_Epoch.)

Fast Auroral SnapshoT (from all.xml/observatory/description/@short)

Fast Auroral SnapshoT (from Master/CDFglobalAttributes/Source_name)

High Time Resolution (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/dcf/l2/dcb/1996/09/fast_hr_dcb_19960928004521_00407_v02.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 77.2140% of the 30559 timesteps. 

Full Magnetic Field in Geocentric Equatorial Inertial Coordinates

Removed Magnetic Field Spin-Tone Harmonic in Despun Spacecraft Coordinates

Counts based on variable 'Spin_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/dcf/l2/dcb/1996/09/fast_hr_dcb_19960928004521_00407_v02.cdf. The most common cadence, 14982345581 [ns] = PT14.982346S, occurred for 0.7968% of the 4 timesteps. 

Counts based on variable 'Ephemeris_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/dcf/l2/dcb/1996/09/fast_hr_dcb_19960928004521_00407_v02.cdf. The most common cadence, 1000000238 [ns] = PT1S, occurred for 45.7922% of the 3662 timesteps. 

Spacecraft Position in Geocentric Equatorial Inertial Coordinates

Spacecraft Velocity in Geocentric Equatorial Inertial Coordinates

Model Magnetic Field in Geocentric Equatorial Inertial Coordinates

Footprint Magnetic Field in Geocentric Equatorial Inertial Coordinates

Dipole Orientation in Geocentric Equatorial Inertial Coordinates

GROUP 1    Satellite   Resolution   Factor            fast           60         1                                                                                               Start Time           Stop Time            1996 235 00:00       2009 124 00:00   Coord/            Min/Max   Range Filter       FilterComponent   Output Markers  Minimum  Maximum   Mins/Maxes GEO X        YES      -         -           -             -         -             -   GEO Y        YES      -         -           -             -         -             -   GEO Z        YES      -         -           -             -         -             -   GEO Lat      YES      -         -           -             -         -             -   GEO Lon      YES      -         -           -             -         -             -   GEO LT       YES      -         -           -             -         -             -   GM X         YES      -         -           -             -         -             -   GM Y         YES      -         -           -             -         -             -   GM Z         YES      -         -           -             -         -             -   GM Lat       YES      -         -           -             -         -             -   GM Lon       YES      -         -           -             -         -             -   GM LT        YES      -         -           -             -         -             -   GSE X        YES      -         -           -             -         -             -   GSE Y        YES      -         -           -             -         -             -   GSE Z        YES      -         -           -             -         -             -   GSE Lat      YES      -         -           -             -         -             -   GSE Lon      YES      -         -           -             -         -             -   GSE LT       YES      -         -           -             -         -             -   GSM X        YES      -         -           -             -         -             -   GSM Y        YES      -         -           -             -         -             -   GSM Z        YES      -         -           -             -         -             -   GSM Lat      YES      -         -           -             -         -             -   GSM Lon      YES      -         -           -             -         -             -   SM X         YES      -         -           -             -         -             -   SM Y         YES      -         -           -             -         -             -   SM Z         YES      -         -           -             -         -             -   SM Lat       YES      -         -           -             -         -             -   SM Lon       YES      -         -           -             -         -             -   SM LT        YES      -         -           -             -         -             -                                                                                       Addtnl             Min/Max      Range Filter          FilterOptions     Output Markers    Minimum     Maximum    Mins/MaxesdEarth       YES      -         -           -             -   MagStrgth    YES      -         -           -             -   dNeutS       YES      -         -           -             -   dBowSck      YES      -         -           -             -   dMagPause    YES      -         -           -             -   L_Value      YES      -         -           -             -   InvarLat     YES      -         -           -             -   Perform the following magnetic field traces:       North trace for GEO footpoint; Output: lat, lon, arclen.    South trace for GEO footpoint; Output: lat, lon, arclen.    North trace for GM footpoint; Output: lat, lon, arclen.    South trace for GM footpoint; Output: lat, lon, arclen.Magnetic field model:                              Internal: IGRF    External: Tsyganenko 89C     External: Tsyganenko 89C     Kp:  3-,3,3+    Stop trace altitude (km):   100.00                                          Formats and units:                              Day/Time format: YYYY DDD HH:MM    Degrees/Hemisphere format: Decimal degrees with 2 place(s).        Longitude 0 to 360, latitude -90 to 90.    Distance format: Earth radii with 2 place(s).

SPDF/CDAWeb. Please also acknowledge the data producer: SSCWeb at SPDF/Goddard

SPDF/SSCWeb. Please also acknowledge the data producer: SSCWeb at SPDF/Goddard

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: SSCWeb at SPDF/Goddard

SPDF/SSCWeb and the HAPI project. Please also acknowledge the data producer: SSCWeb at SPDF/Goddard

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/ephemeris/1996/fast_or_ssc_19960801_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 6678720 timesteps. 

The arc length of the line from the spacecraft to the north geographic magnetic field footprint

The arc length of the line from the spacecraft to the south geographic magnetic field footprint

The arc length of the line from the spacecraft to the north geomagnetic footprint

The arc length of the line from the spacecraft to the south geomagnetic field footprint

SPDF/CDAWeb. Please also acknowledge the data producer: Lynn Kistler at University of New Hampshire

SPDF/SSCWeb. Please also acknowledge the data producer: Lynn Kistler at University of New Hampshire

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Lynn Kistler at University of New Hampshire

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_Helium.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_Helium.)

Time of Flight Energy Angle Mass Spectrometer (from all.xml/instrument/description/@short)

Level 2 Survey Resolution (from Master/CDFglobalAttributes/Data_type)

H+ Energy-Pitch Angle Distribution (spectrograms at 16 selected pitch angles)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/teams/l2/pa/1996/fast_teams_pa_l2_19960920_322_v02.cdf. The most common cadence, 5568359375 [ns] = PT5.568359S, occurred for 7.1038% of the 13 timesteps. 

O+ Energy-Pitch Angle Distribution (spectrograms at 16 selected pitch angles)

Proton Flag. Non-zero values indicate that incomplete data was used

Oxygen Flag. Non-zero values indicate that incomplete data was used

Spacecraft orbit number. Note: CDF_UINT4 data was converted to HAPI double.

He+ Energy-Pitch Angle Distribution (spectrograms at 16 selected pitch angles)

Counts based on variable 'Epoch_Helium' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/teams/l2/pa/1996/fast_teams_pa_l2_19960920_322_v02.cdf. The most common cadence, 5568359375 [ns] = PT5.568359S, occurred for 9.5890% of the 14 timesteps. 

Helium Flag. Non-zero values indicate that incomplete data was used

SPDF/CDAWeb. Please also acknowledge the data producer: J. P. McFadden at U.C. Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: J. P. McFadden at U.C. Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. P. McFadden at U.C. Berkeley Space Sciences Laboratory

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/esa/l2/eeb/1996/09/fa_esa_l2_eeb_19960916224356_00287_v02.cdf. The most common cadence, 169 [ms] = PT0.169S, occurred for 92.8571% of the 13 timesteps. 

Fast Auroral SnapshoT Explorer (from all.xml/observatory/description/@short)

Fast Auroral SnapshoT Explorer, Electrostatic Analyzer (from all.xml/instrument/description/@short)

Fast Auroral SnapshoT Explorer (from Master/CDFglobalAttributes/Source_name)

Level 2 data: Eesa Burst (from Master/CDFglobalAttributes/Data_type)

CDF EPOCH time, one element per ion distribution (NUM_DISTS elements)

Burst Electron Raw Counts data with dimensions (96, 64, NUM_DISTS)

Differential burst-mode electron energy flux array with dimensions (96, 64, NUM_DISTS) (as plasmagrams)

---> Pitch Angle values for each distribution (96, 64, NUM_DISTS)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/esa/l2/ees/1996/08/fa_esa_l2_ees_19960830220759_00103_v02.cdf. The most common cadence, 836 [ms] = PT0.836S, occurred for 98.3412% of the 415 timesteps. 

Level 2 data: Eesa Survey (from Master/CDFglobalAttributes/Data_type)

Survey Electron Raw Counts data with dimensions (96, 64, NUM_DISTS)

Differential survey-mode electron energy flux array with dimensions (96, 64, NUM_DISTS) (as plasmagrams)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/esa/l2/ieb/1996/09/fa_esa_l2_ieb_19960916224356_00287_v02.cdf. The most common cadence, 169 [ms] = PT0.169S, occurred for 92.8571% of the 13 timesteps. 

Level 2 data: Iesa Burst (from Master/CDFglobalAttributes/Data_type)

Differential burst-mode ion energy flux array with dimensions (96, 64, NUM_DISTS) (as plasmagrams)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/esa/l2/ies/1996/08/fa_esa_l2_ies_19960830220801_00103_v02.cdf. The most common cadence, 836 [ms] = PT0.836S, occurred for 94.2928% of the 380 timesteps. 

Level 2 data: Iesa Survey (from Master/CDFglobalAttributes/Data_type)

Differential survey-mode ion energy flux array with dimensions (96, 64, NUM_DISTS) (as plasmagrams)

The FAST home page maintained at the University of California Berkeley with links to publications, documentation, access to data and software.

SPDF/CDAWeb. Please also acknowledge the data producer: C. Carlson at U.C. Berkeley

SPDF/SSCWeb. Please also acknowledge the data producer: C. Carlson at U.C. Berkeley

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C. Carlson at U.C. Berkeley

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/acf/k0/1996/fa_k0_acf_19960830_v01.cdf. The most common cadence, 3344 [ms] = PT3.344S, occurred for 30.4281% of the 1379 timesteps. 

FAST AURORAL SNAPSHOT (from all.xml/observatory/description/@short)

MAGNETOSPHERIC SCIENCE (from Master/CDFglobalAttributes/Discipline)

FAST AURORAL SNAPSHOT (from Master/CDFglobalAttributes/Source_name)

Electric field power spectral density (0-2 MHz), in 59 fixed frequency bins of width 32 kHz

Electric field power spectral density (0-16 kHz), in 56 fixed frequency bins

Electric field power spectral density (0-2 kHz), in 62 fixed frequency bins

Magnetic field power spectral density (0-2 MHz), in 59 fixed frequency bins of width 32 kHz

Magnetic field power spectral density (0-16 kHz), in 56 fixed frequency bins

Magnetic field power spectral density (0-2 kHz), in 62 fixed frequency bins

array containing HF Electric Power and HF Magnetic Power (0-2 MHz)

array containing VLF Electric Power and VLF Magnetic Power (0-16 kHz)

array containing ELF Electric Power and ELF Magnetic Power (0-2 kHz)

Spacecraft altitude above an equatorial earth radius of 6378.14 km, km

Geodetic latitude of magnetic footprint at 100 km above the oblate earth, deg

Geodetic longitude of magnetic footprint at 100 km above the oblate earth, deg

The Time-of-Flight Energy, Angle, Mass Spectrograph (TEAMS) Experiment for FAST,  D. M. Klumpar, E. Moebius, L. M. Kistler, M. Popecki, E. G. Shelley, E. Hertzberg, K. Crocker, M. Granoff, Li Tang, C. W. Carlson, J. McFadden, B. Klecker, F. Eberl, E. Kuenneth, H. Kaestle, M. Ertl, W. K. Peterson, and D. Hovestadt, published, Space Science Reviews, 2001, volume 98, pages 197-291,  doi:10.1023/A:1013127607414. The 3-D Plasma Distribution Function Analyzers with Time-of-Flight Mass Discrimination for CLUSTER, FAST,and Equator-S, E. Moebius, L. M. Kistler, M. Popecki, K. Crocker, M. Granoff, Y. Jiang, E. Satori, V. Ye, H. Reme, J. A. Sauvaud, A. Cros, A. Aoustin, T. Camus, J. L. Medale, J. Rouzaud, C. W. Carlson, J. McFadden, D. Curtis, H. Heetdirks, J. Croyle, C. Ingraham, E. G. Shelley, D. M. Klumpar, E. Hertzberg, B. Klecker, M. Ertl, F. Eberl, H. Kaestle, E. Kuenneth, P. Laeverenz, E. Seidenschwang, G. Parks, M. McCarthy, A. Korth, B. Graeve, H. Balsiger, U. Schwab, and M. Steinacher, Measurement Techniques for Space Plasmas: Particles, 1998, Geophysical Monograph Series, volume 102, pages 243-248.Data are derived from a time-of-flight mass spectrograph that determines 3-dimensional distribution functions of individual ion species over the energy range 1 - 12000 eV, within 2.5 seconds (one-half spacecraft spin).  The instrument consists of a toroidal top-hat electrostatic analyzer with instantaneous acceptance of ions over 360 degrees in polar angle in 16 sectors.  Ions passing through the electrostatic analyzer are postaccelerated by up to 25 kV and then analyzed for mass per charge in a foil-based time-of-flight analyzer.  The data used to construct CDF data products are derived from the Survey data.  Survey data consists of 4 mass groups x 48 energies x 64 solid angle segments. The 4 mass groups are H+, O+, He+, and He++.  Only the 16 equatorial angle segments are used for the CDF data set. Each equatorial solid angle segment contains 2 (4) samples at each energy in the 32 (64) sweep/spin mode.  The full angular range is covered in half a spin but the actual time resolution of the survey data product depends upon the telemetry mode.  In the highest TM rate modes H+ and O+ survey data read out every half spin.  In lowest TM rate mode these data are accumulated for 4 spins.  The minimum accumulation time included in the CDF is 1 spin, so if the actual accumulation time is a half spin, two data points are averaged.  Otherwise, the full resolution is included. In every mode He+ and He++ are accumulated twice as long as H+ and O+.  To force the H+, O+, and He+ to have an equal number of data points when H+ and O+ have twice the time resolution, each He+ data point is written twice consecutively in the file. 

Caveats for the FAST Time-of-flight Energy Angle Mass Spectrograph, TEAMS, Survey Data

SPDF/CDAWeb. Please also acknowledge the data producer: E. Lund at UNH

SPDF/SSCWeb. Please also acknowledge the data producer: E. Lund at UNH

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: E. Lund at UNH

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/fast/teams/k0/1996/fa_k0_tms_19961001_v01.cdf. The most common cadence, 19988 [ms] = PT19.988S, occurred for 8.5389% of the 90 timesteps. 

FAST Auroral Snapshot Explorer (from all.xml/observatory/description/@short)

FAST Auroral Snapshot Explorer (from Master/CDFglobalAttributes/Source_name)

H+ diff energy flux, averaged over 0-360 pitchangle, at 48 energies, 1-12000 eV 

O+ diff energy flux, averaged over 0-360 pitchangle, at 48 energies, 1-12000 eV 

He+ diff energy flux, averaged over 0-360 pitchangle, at 48 energies, 1-12000 eV 

Keograms are quick-look data of an all-sky camera at Kilpisjarvi (69.02 N, 20.79 E)   maintained and operated by the Finnish Meteorological Institute.Keograms show the intensity along the middle meridian of the camera field-of-view as a function of time. The camera has a fish-eye lens of 180 degrees and narrow bandpass interference filters of wavelengths 557.7 nm (green) and 630.0 nm (red). In standard operating mode, the sampling interval is 20 s and 60 s for the red and green images, respectively.The exposure time is typically 1000 ms. The time resolution of keograms is 1 min and they are constructed using only the green images.The size of a digital image is 512x512 pixels and intensity values vary between 0 and 255. At the altitude of 110 km the field-of-view (with reasonable spatial resolution) is a spherical area with the diameter of 600 km.  The keograms shown here are intensity versus latitude plots while the original keograms (available in http://www.geo.fmi.fi/MIRACLEare intensity versus zenith angle plots.The conversion from zenith angle dependence to equidistant latitude grid causes occasionally artificial two-band structure to the keograms(light bands below and above the darker zenith).The artefact becomes visible especially during quiet periods, and the autoscaling color palette may even strengthen the effect.Note that some keograms show also the Moon as a sphere or ellipsoid with very high, even saturating intensities. 

Finnish Meteorological Institute, FMI, All-Sky Cameras, Imaging the Auroras

SPDF/CDAWeb. Please also acknowledge the data producer: K. Kauristie at Finnish Meteorological Institute

SPDF/SSCWeb. Please also acknowledge the data producer: K. Kauristie at Finnish Meteorological Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Kauristie at Finnish Meteorological Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/FinnishMeteorInst/kilp/1997/fm_k0_kilp_19970101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Finnish Meteorological Institute (from all.xml/observatory/description/@short)

Kilpisjarvi All-Sky Camera (from all.xml/instrument/description/@short)

Finnish Meteorological Institute (from Master/CDFglobalAttributes/Source_name)

Auroral luminosity, 557.7nm keogram, all-sky camera at Kilpisjarvi (N69.02,E20.79)

IDN>Ion Number Density. Advanced Ionospheric Probe (AIP) is provided by Graduate Institute of Space Science, National Central University (NCU) for the FORMOSAT-5 satellite as a scientific payload. The AIP is an all-in-one plasma sensor with sampling rate up to 8,192 Hz to measure ionospheric plasma concentrations, velocities, and temperatures over a wide range of spatial scales. Once a comprehensive dataset is available from the AIP, a systematic examination of longitudinal and seasonal variations of the ionospheric parameters in the topside F region can be conducted for all latitudinal coverage. The transient and long-term variations of ionospheric plasma can be monitored in the upcoming solar maximum period and are beneficial to predict the trend of the space weather as well as the seismic precursors associated with earthquakes.

Please write 'We are grateful to NSPO, Taiwan, for the formosat-5 data.' in acknowledgment. Please cite 'Lin, Z. W., C. K. Chao, J. Y. Liu, C. M. Huang, Y. H. Chu, C. L. Su, Y. C. Mao, and Y. S. Chang (2017), Advanced Ionospheric Probe scientific mission onboard FORMOSAT-5 satellite, Terr. Atmos. Ocean. Sci., doi: 10.3319/TAO.2016.09.14.01(EOF5).'.

SPDF/CDAWeb. Please also acknowledge the data producer: C.K. Chao at NCU

SPDF/SSCWeb. Please also acknowledge the data producer: C.K. Chao at NCU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C.K. Chao at NCU

Advanced Ionospheric Probe (from all.xml/instrument/description/@short)

The NOAA Geostationary Operational  Environmental Satellite (GOES) key parameters are obtained from the Energetic Particle Sensor (EPS) and the magnetometer (MAG).  The key parameters are a subset of the  data available from the GOES Space Environment Monitor (SEM) instruments.The energetic particle fluxes are  given as five-minute averaged values and the vector magnetic field is given as one-minute average values.Flux values for three integral electron channels (E >0.6 MeV, E >2.0 MeV, and E >4.0 MeV) and one differential proton channel(0.7 MeV < E <4 MeV) are provided. These data are used by NOAA Space Environment Center (SEC) for the real-time monitoring and prediction of the conditions in the Earth's space environment.  A new series of GOES spacecraft began with GOES-8 launched on 4/13/94, GOES-9 launched on 5/23/95, and GOES-10 launched on 4/25/97. Typically two satellites are maintained operational,one at about 135 degrees geographic west longitude and one at about 75 degrees geographic west longitude. The satellite inclination is typically within a few tenths of a degree of the geographic equator.However, the satellites can be moved, especially during the six months to one year following launch, and the inclination can increase after years of satellite operation.Instrument data quality flags are set from real-time telemetry, or, in the case of historically-processed data sets when telemetry is not available, fixed to a level-1 instrument status flag for all dataReference: Geostationary Operational Environmental Satellite GOES I-M System Description, compiled by John Savides, Space Systems/Loral, Palo Alto, California, December 1992. Dr. Terrance Onsager, NOAA/SEC, tonsager@sec.noaa.gov, 303-497-5713, Boulder CO 80303 USA, or Martin Black, NOAA/SEC, mblack@sec.noaa.gov, 303-497-7235, 325 Broadway, Boulder CO 80303 USANOTICE: GOES 12 energetic particle data are not availabledue to the failure of two proton channels in the detectors.  These channels were used for the correction and processing of the proton and electron data.  Beginning April 8, 2003, the GOES energetic particle data are obtained from GOES 10 only. 

SPDF/CDAWeb. Please also acknowledge the data producer: T. Onsager at NOAA SEC

SPDF/SSCWeb. Please also acknowledge the data producer: T. Onsager at NOAA SEC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. Onsager at NOAA SEC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes10/ep8_k0/1999/g0_k0_ep8_19990321_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Geostationary Operational Environmental Satellite 10 (from all.xml/observatory/description/@short)

Energetic Particle Sensor (from all.xml/instrument/description/@short)

The NOAA Geostationary Operational  Environmental Satellite (GOES) key parameters are obtained from the Energetic Particle Sensor (EPS) and and the magnetometer (MAG).  The key parameters are a subset of the  data available from the GOES Space Environment Monitor (SEM) instruments.The vector magnetic field is  given as one-minute averaged values in three coordinate systems: (1) Spacecraft (s/c) P,E,N, (2) GSM x,y,z, (3) GSE x,y,zs/c mag. field is defined as: Hp, perpendicular to the satellite orbital plane or parallel to the Earths spin axis in the case of a zero degree inclination orbit; He, perpendicular to Hp and directed earthwards; and Hn, perpendicular to both Hp and directed eastwards.These data are used by NOAA Space Environment Center (SEC) for the real-time monitoring and prediction of the conditions in the Earth's space environment.  A new series of GOES spacecraft began with GOES-8 launched on 4/13/94, GOES-9 launched on 5/23/95, and GOES-10 launched on 4/25/97.Typically two satellites are operational,one at about 135 degrees geographic west longitude and one at about 75 degrees geographic west longitude. The satellite inclination is typically within a few tenths of a degree of the geographic equator. However, the satellites can be moved, especially during the six months to one year following launch, and the inclination can increase after years of satellite operation.Instrument data quality flags are set from real-time telemetry, or, in the case of historically-processed data sets when telemetry is not available, fixed to a level-1 instrument status flag for all dataReference: Monitoring Space Weather with GOES Magnetometers, Singer, H.J, L. Matheson, R.Grubb A.Newman, and S.D.Bouwer, SPIE Proceedings, Volume 2812, 4-9 Aug 1996.  For more info, contact:Dr. Howard Singer, NOAA/SEC, hsinger@sec.noaa.gov, 303-497-6959, Boulder CO 80303 USA, or Martin Black, NOAA/SEC, mblack@sec.noaa.gov, 303-497-7235, 325 Broadway, Boulder CO 80303 USA

SPDF/CDAWeb. Please also acknowledge the data producer: H. Singer at NOAA SEC

SPDF/SSCWeb. Please also acknowledge the data producer: H. Singer at NOAA SEC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: H. Singer at NOAA SEC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes10/mag_k0/1999/g0_k0_mag_19990321_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

GOES-10 High Resolution Magnetometer data vectors (at 512 ms, ephem at 60 sec)

Satellite positions and velocities derived from SSCWEB GEI ephemeris, interpolated to one minute time resolution; perpendicular vectors for ENP coordinate system derived from pos X vel. B field vectors in LH-ENP and GEI systems, B field total magnitude, magnetotorquer counts, and data quality flags derived from 512 msec binary GOES data files. General Comments from Dr. Howard J. Singer (GOES Magnetometer PI)   1. Data Description: A full description of the GOES magnetometer data, including use of the quality flags and torquer current information, is contained in a GOES 8-12 Magnetometer Readme File prepared by Dr. Howard J. Singer. The GOES data have been prepared at NOAA Space Weather Prediction Center (SWPC) by Dr. Howard J. Singer with major data processing and data evaluation contributions by SWPC staff, Lorne Matheson and Ann Newman, as well as coordinate transformation development by Dr. Paul Loto aniu (University of Colorado/SWPC). 2. Coordinate description for PEN: .Hp:  magnetic field vector component, points northward, perpendicular to orbit plane which for a zero degree inclination orbit is parallel to Earth's spin axis. .He:  magnetic field vector component, perpendicular to Hp and Hn and points earthward. .Hn:  magnetic field vector component, perpendicular to Hp and He and points eastward. Ht:  total field.  3. Magnetometer offsets and noise: GOES 8-12 spacecraft are 3-axis stabilized. There is only one opportunity for a spin maneuver at the beginning of the mission to determine on-orbit magnetic field offsets. There are additional complications that result from needing to know the changing offsets introduced by torquer coils on the satellites. While comparisons of GOES data to model fields during quiet times and comparisons to nearby encounters with other spacecraft are used to demonstrate the observed data values are reasonable, caution should be used in assigning absolute accuracy. While there has been a significant effort to remove the effects of torquer coil interference in the 0.512 s data, there can be small, typically less than 1 nT spikes in the data at the time of torquer current changes. More information on this topic is included the more extensive readme file. This file is a living document that will be updated periodically.  4.  Orbital Inclination: During the primary operational lifetime of the GOES satellites, the satellite inclination is typically kept within a few tenths of a degree of 0 degrees inclination; however, as the satellite ages, the inclination can grow to several degrees.

SPDF/CDAWeb. Please also acknowledge the data producer: Howard J. Singer at NOAA Space Weather Prediction Center

SPDF/SSCWeb. Please also acknowledge the data producer: Howard J. Singer at NOAA Space Weather Prediction Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Howard J. Singer at NOAA Space Weather Prediction Center

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => g10_longitude_epoch, @1 => g10_ephem_epoch, @2 => g10_sample_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => g10_longitude_epoch, @1 => g10_ephem_epoch, @2 => g10_sample_epoch.)

Geostationary Operational Environmental Satellite (GOES-10) (from all.xml/observatory/description/@short)

Fluxgate magnetometer (from all.xml/instrument/description/@short)

Geostationary Operational Environmental Satellite (GOES-10) (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'g10_ephem_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes10/mag_l2/2007/g10_l2_mag_20070101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Unit vector in GEI perp to orbital plane (parallel to Earth's spin axis for 0 inclination orbit)

Magnetic field in LH-ENP (P=northward Perp to orbital plane, E=Earthward perp to P and Earth center, N=eastward/LH Normal to P and E)

Counts based on variable 'g10_sample_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes10/mag_l2/2007/g10_l2_mag_20070101_v01.cdf. The most common cadence, 511 [ms] = PT0.511S, occurred for 33.8924% of the 57191 timesteps. 

Data quality flag (7=good). Note: CDF_UINT4 data was converted to HAPI double.

GOES-11 High Resolution Magnetometer data vectors (at 512 ms, ephem at 60 sec)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => g11_longitude_epoch, @1 => g11_ephem_epoch, @2 => g11_sample_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => g11_longitude_epoch, @1 => g11_ephem_epoch, @2 => g11_sample_epoch.)

Geostationary Operational Environmental Satellite (GOES-11) (from all.xml/observatory/description/@short)

Geostationary Operational Environmental Satellite (GOES-11) (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'g11_ephem_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes11/mag_l2/2007/g11_l2_mag_20070101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'g11_sample_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes11/mag_l2/2007/g11_l2_mag_20070101_v01.cdf. The most common cadence, 511 [ms] = PT0.511S, occurred for 34.2236% of the 57752 timesteps. 

GOES-12 High Resolution Magnetometer data vectors (at 512 ms, ephem at 60 sec)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => g12_longitude_epoch, @1 => g12_ephem_epoch, @2 => g12_sample_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => g12_longitude_epoch, @1 => g12_ephem_epoch, @2 => g12_sample_epoch.)

Geostationary Operational Environmental Satellite (GOES-12) (from all.xml/observatory/description/@short)

Geostationary Operational Environmental Satellite (GOES-12) (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'g12_ephem_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes12/mag_l2/2007/g12_l2_mag_20070101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'g12_sample_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes12/mag_l2/2007/g12_l2_mag_20070101_v01.cdf. The most common cadence, 511 [ms] = PT0.511S, occurred for 33.3527% of the 56282 timesteps. 

The NOAA GOES satellites include 2 sensors: an Energetic Particle Sensor (EPS), and a Magnetometer (MAG).The satellites are geostationary. For older satellites, inclination may be up to 15 deg.Data sometimes contains errors. especially GOES-6 EPS & possibly both  GOES 6,7 magnetometers. The EPS data are 5-min. averages, the MAG data are 1-min. averages. The NOAA Space Environment Lab (SEL), Space Environ. Services Center (SESC) uses this data in real time for forecasting and monitoring. Reference: GOES Spacecraft OperationsManual, Volume I, May 1980, Hughes RefNo. D5150 SCG 00169RGOES-8, with 3 electron sensors should launch in early 93: the IE variables will be defined post-launch.For additional info., contact Dave Bouwer, NOAA/SEL, Mail Code R/E/SE, 325 Broadway, Boulder, CO 80303 USA (303)497-3899.SELVAX::DBOUWER or dbouwer@selvax.sel.bldrdoc.gov

SPDF/CDAWeb. Please also acknowledge the data producer: H. Sauer at NOAA

SPDF/SSCWeb. Please also acknowledge the data producer: H. Sauer at NOAA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: H. Sauer at NOAA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes06/eps_k0/1992/g6_k0_eps_19921212_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Geostationary Operational Environmental Satellite 6 (from all.xml/observatory/description/@short)

The NOAA GOES satellites include 2 sensors: an Energetic Particle Sensor (EPS), and a Magnetometer (MAG).The satellites are geostationary. For older satellites, inclination may be up to 15 deg.Data sometimes contains errors.The EPS data are 5-min. averages, the MAG data are 1-min. averages. B s/c has undeterm. errors in x,y B field for GSM and GSE is missing while corrections are developed.The NOAA Space Environment Lab (SEL), Space Environ. Services Center (SESC) uses this data in real time for forecasting and monitoring. Reference: GOES Spacecraft OperationsManual, Volume I, May 1980, Hughes RefNo. D5150 SCG 00169RGOES-8, with 3 electron sensors should launch in early 93: the IE variables will be defined post-launch.For additional info., contact Dave Bouwer, NOAA/SEL, Mail Code R/E/SE, 325 Broadway, Boulder, CO 80303 USA (303)497-3899.SELVAX::DBOUWER or dbouwer@selvax.sel.bldrdoc.gov

SPDF/CDAWeb. Please also acknowledge the data producer: R. Zwickl at NOAA SEL

SPDF/SSCWeb. Please also acknowledge the data producer: R. Zwickl at NOAA SEL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Zwickl at NOAA SEL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes06/mag_k0/1992/g6_k0_mag_19921212_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes07/eps_k0/1992/g7_k0_eps_19921212_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Geostationary Operational Environmental Satellite 7 (from all.xml/observatory/description/@short)

GOES 7 s/c position, Geographic, Polar Coordinates (data begin March 6, 1993)

GOES 7 s/c position, Geographic, Cartesian Coordinates (data begin March 6, 1993)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes07/mag_k0/1992/g7_k0_mag_19921212_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes07/mag_k1/g7_k1_mag_19950211_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1199 timesteps. 

Geostationary Operational Environmental Satellite 7 (from Master/CDFglobalAttributes/Source_name)

The NOAA Geostationary Operational Environmental Satellite (GOES) keyparameters are obtained from theEnergetic Particle Sensor (EPS)and the magnetometer (MAG).  Thekey parameters are a subset of the data available from the GOES SpaceEnvironment Monitor (SEM) instruments.The energetic particle fluxes are given as five-minute averaged valuesand the vector magnetic field is givenas one-minute average values.Flux values for three integral electronchannels (E >0.6 MeV, E >2.0 MeV,and E >4.0 MeV) and one differentialproton channel(0.7 MeV < E <4 MeV)are provided. These data are used byNOAA Space Environment Center (SEC)for the real-time monitoring andprediction of the conditions in theEarth's space environment.  A newseries of GOES spacecraft beganwith GOES-8 launched on 4/13/94 andGOES-9 launched on 5/23/95. Typicallytwo satellites are maintainedoperational,one at about 135 degreesgeographic west longitude and one atabout 75 degrees geographic westlongitude. The satellite inclinationis typically within a few tenths of adegree of the geographic equator.However, the satellites can be moved,especially during the six months toone year following launch, and theinclination can increase after yearsof satellite operation.Reference: Geostationary OperationalEnvironmental Satellite GOES I-MSystem Description, compiled by JohnSavides, Space Systems/Loral, PaloAlto, California, December 1992.Dr. Terrance Onsager, NOAA/SEC,tonsager@sec.noaa.gov, 303-497-5713,Boulder CO 80303 USA,or Dave Bouwer, NOAA/SEC,dbouwer@sel.noaa.gov, 303-497-3899,325 Broadway, Boulder CO 80303 USA

GOES 8 Energetic Particle Sensor Additional Data File Information

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes08/ep8_k0/1995/g8_k0_ep8_19951201_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Geostationary Operational Environmental Satellite 8 (from all.xml/observatory/description/@short)

The NOAA Geostationary Operational  Environmental Satellite (GOES) key parameters are obtained from the Energetic Particle Sensor (EPS) and and the magnetometer (MAG).  The key parameters are a subset of the  data available from the GOES Space Environment Monitor (SEM) instruments.The vector magnetic field is  given as one-minute averaged values in three coordinate systems: (1) Spacecraft (s/c) P,E,N, (2) GSM x,y,z, (3) GSE x,y,zs/c mag. field is defined as: Hp, perpendicular to the satellite orbital plane or parallel to the Earths spin axis in the case of a zero degree inclination orbit; He, perpendicular to Hp and directed earthwards; and Hn, perpendicular to both Hp and directed eastwards.These data are used by NOAA Space Environment Center (SEC) for the real-time monitoring and prediction of the conditions in the Earth's space environment.  A new series of GOES spacecraft began with GOES-8 launched on 4/13/94 and GOES-9 launched on 5/23/95.Typically two satellites are operational,one at about 135 degrees geographic west longitude and one at about 75 degrees geographic west longitude. The satellite inclination is typically within a few tenths of a degree of the geographic equator. However, the satellites can be moved, especially during the six months to one year following launch, and the inclination can increase after years of satellite operation.Reference: Monitoring Space Weather with GOES Magnetometers, Singer, H.J, L. Matheson, R.Grubb A.Newman, and S.D.Bouwer, SPIE Proceedings, Volume 2812, 4-9 Aug 1996.  For more info, contact:Dr. Howard Singer, NOAA/SEC, hsinger@sec.noaa.gov, 303-497-6959, Boulder CO 80303 USA, or Dave Bouwer, NOAA/SEC, dbouwer@sec.noaa.gov, 303-497-3899, 325 Broadway, Boulder CO 80303 USA

A web site hosted by NOAA with information and links to the GOES spacecraft and data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes08/mag_k0/1995/g8_k0_mag_19951201_v04.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

MGF Instrument Status:  0=OK, 1=minor problems, 2=major problems, 3=missing data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes09/ep8_k0/1995/g9_k0_ep8_19951201_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Geostationary Operational Environmental Satellite 9 (from all.xml/observatory/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes09/mag_k0/1995/g9_k0_mag_19951201_v04.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/galileo/helio1day/galileo_helio1day_position_19891020_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 5093 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/galileo/helio1hr/galileo_helio1hr_position_19891020_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 122231 timesteps. 

Fully processed Level 2 solar wind ion data at 2.5-min intervals including proton density (/cc), temperature (K), velocity vectors (km/s) in GSE and RTN systems, alpha/proton ratio, and flags for times of bi-directional electron streaming. 

Data are openly available for scientific study. Users are encouraged to consult with team members on data usage. Please send copies of publications making use of this data to the LANL team.

SPDF/CDAWeb. Please also acknowledge the data producer: Roger C. Wiens at LANL

SPDF/SSCWeb. Please also acknowledge the data producer: Roger C. Wiens at LANL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Roger C. Wiens at LANL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/genesis/gim/3dl2_gim/2001/genesis_3dl2_gim_20010824_v01.cdf. The most common cadence, 160036 [ms] = PT2M40.036S, occurred for 1.2223% of the 48 timesteps. 

Genesis Ion Monitor (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: J.H. King, N. Papatashvilli at Perot Sys, NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J.H. King, N. Papatashvilli at Perot Sys, NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.H. King, N. Papatashvilli at Perot Sys, NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/merged/magplasma_sw_1min_cdaweb/1995/ge_1min_mag_plasma_sw_only_19950101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

merged IMF, Plasma, Ephemerides data, solar wind only (from all.xml/instrument/description/@short)

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer:  at 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/orbit/def_at/2022/ge_at_def_20220925_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 99.2958% of the 141 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/orbit/pre_at/2022/ge_at_pre_20221211_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC),Japan, while the Editor-B data are 24-hours continuouslyrecorded in the onboard tape recorders and are dumpedover the NASA/JPL Deep Space Network (DSN) stations                                     Please use the Editor-A LEP dataset prior to the Editor-B LEP dataset sinceplasma moments in the Editor-A data are more reliable. (Plasma moments inthe Editor-B are calculated onboard.)                                     The ion energy analyzer (LEP-EAi) has two energy scan mode: RAM-A (60eV to 40 keV) and RAM-B (5 keV to 40 keV). The energy scan mode is automatically selected onboard depending on the incoming ion fluxes. At present, only the plasma moments in the RAM-A mode are plotted (listed) for the LEP-EAi data. (The LEP-EAi moments are presented by the solid lines in the plot.)                                     The plasma moment data of the solar wind analyzer (LEP-SW) should beused only qualitatively. The LEP-SW plasma moments are plotted (listed) when the energy scan mode of LEP-EAi is RAM-B. (The LEP-SW moments are presented by the dotted lines in the plot.) J.Geomag.Geoelectr.,46,669,1994

12-sec LEP plasma moments data supplied by and also available at

Reprint of Mukai, T., S. Machida, Y. Saito, M. Hirahara, T. Terasawa, N. Kaya, T. Obara, M. Ejiri, and A. Nishida, The low energy particle (LEP) experiment onboard the Geotail satellite, J. Geomag. Geoelectr., 46, 669-692, 1994.

SPDF/CDAWeb. Please also acknowledge the data producer: T. Mukai at ISAS

SPDF/SSCWeb. Please also acknowledge the data producer: T. Mukai at ISAS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. Mukai at ISAS

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/lep/eda12sec_lep/1993/ge_eda12sec_lep_19930914_v01.cdf. The most common cadence, 12074 [ms] = PT12.074S, occurred for 62.2458% of the 704 timesteps. 

Low-Energy Particles (from all.xml/instrument/description/@short)

Ion Density (qualitative use only if Energy Scan Code = 2 = RAM-B/SW)

Ion Temperature in Satellite coordinates (qualitative use only if Energy Scan Code = 2 = RAM-B/SW)

Ion Velocity (GSE) (qualitative use only if Energy Scan Code = 2 = RAM-B/SW) 

Ion Velocity (GSM) (qualitative use only if Energy Scan Code = 2 = RAM-B/SW) 

Ion Velocity (SM) (qualitative use only if Energy Scan Code = 2 = RAM-B/SW) 

The Bz offset is still contained in the magnetic field data. Themagnitude of the Bz offset is about 0.5 nT (+-0.3 nT). The correctedversion of the magnetic field data will be published soon.Kokubun et al., Geotail Prelaunch Report, ISAS, 58-70, 1992

3-sec MGF magnetic field data suppliled by and also available at

Reprint of Kokubun, S., T. Yamamoto, M. H. Acuna, K. Hayashi, K. Shiokawa, and H. Kawano, The Geotail Magnetic Field Experiment, J. Geomag. Geoelectr., 46, 7-21, 1994.

SPDF/CDAWeb. Please also acknowledge the data producer: S. Kokubun at STELAB Nagoya Univ., Japan

SPDF/SSCWeb. Please also acknowledge the data producer: S. Kokubun at STELAB Nagoya Univ., Japan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: S. Kokubun at STELAB Nagoya Univ., Japan

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/mgf/eda3sec_mgf/1993/ge_eda3sec_mgf_19930901_v01.cdf. The most common cadence, 3019 [ms] = PT3.019S, occurred for 81.1168% of the 1104 timesteps. 

Editor-A 3 second (no correction for Bz offset) (from Master/CDFglobalAttributes/Data_type)

Magnetic field vector in GSE cartesian coordinates (no Bz offset correction)

Magnetic field vector in GSM coordinates (no Bz offset correction)

Magnetic field vector in SM coordinates (no Bz offset correction)

Standard deviation of sin fitting for magnetic field in sensor coordinates 

Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC),Japan, while the Editor-B data are 24-hours continuously recorded in the onboard tape recorders and are dumped over the NASA/JPL Deep Space Network (DSN) stations.                                     Please use the Editor-A LEP dataset prior to the Editor-B LEP dataset since plasma moments in the Editor-A data are more reliable.(Plasma moments in the Editor-B are calculated onboard.)                                     The ion energy analyzer (LEP-EAi) has two energy scan modes: RAM-A (60eV to 40 keV) and RAM-B (5 keV to 40 keV). The energy scan mode is automatically selected onboard depending on the incoming ion fluxes. At present, only the plasma moments in the RAM-A mode are plotted (listed) for the LEP-EAi data. (The LEP-EAi moments are presented by the solid lines in the plot.)                                     The plasma moment data of the solar wind analyzer (LEP-SW) should be used only qualitatively. The LEP-SW plasma moments are plotted (listed) when the energy scan mode of LEP-EAi is RAM-B. (The LEP-SW moments are presented by the dotted lines in the plot.) J.Geomag.Geoelectr.,46,669, 1994

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/lep/edb12sec_lep/1993/ge_edb12sec_lep_19931005_v01.cdf. The most common cadence, 11990 [ms] = PT11.99S, occurred for 52.3837% of the 3670 timesteps. 

Editor-B 12 second (use Editor-A whenever available) (from Master/CDFglobalAttributes/Data_type)

Ion Density (Use only if no Editor-A data; qualitative use only if Energy Scan Code = 2 = RAM-B/SW)

Ion Temperature in Satellite coordinates (Use only if no Editor-A data; qualitative use only if Energy Scan Code = 2 = RAM-B/SW)

Ion Velocity (GSE) (Use only if no Editor-A data; qualitative use only if Energy Scan Code = 2 = RAM-B/SW)

Ion Velocity (GSM) (Use only if no Editor-A data; qualitative use only if Energy Scan Code =  2 = RAM-B/SW)

Ion Velocity (SM) (Use only if no Editor-A data; qualitative use only if Energy Scan Code = 2 = RAM-B/SW)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/mgf/edb3sec_mgf/1993/ge_edb3sec_mgf_19930901_v01.cdf. The most common cadence, 3019 [ms] = PT3.019S, occurred for 62.0344% of the 7245 timesteps. 

Editor-B 3 second (no correction for Bz offset)) (from Master/CDFglobalAttributes/Data_type)

Magnetic field vector in GSM coordinates (no Bz offset correction 

Plasma Moments, Definitive Geotail CPI/SWA (Comprehensive Plasma Instrument / Solar Wind Analyzer)

Version 6 data processing replaced version 5 processing for data after March 10, 2006, when the CPI team started using 64 energy steps per spectrum instead of the previously used 32 steps per spectrum.  The change was made to ensure that even for very cold flows, the spectrum would have a sufficient number of significant points to derive moments.  The change resulted in 96s spectra and 96s-resolution moments, vs. 48s previously.

SPDF/CDAWeb. Please also acknowledge the data producer: L. Frank, W. Patterson and K. Ackerson at U. Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: L. Frank, W. Patterson and K. Ackerson at U. Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: L. Frank, W. Patterson and K. Ackerson at U. Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/cpi/cpi_h0/1992/ge_h0_cpi_19920928_v06.cdf. The most common cadence, 47500 [ms] = PT47.5S, occurred for 23.7685% of the 386 timesteps. 

Comprehensive Plasma Instrumentation (from all.xml/instrument/description/@short)

SWA Definitive Moments (from Master/CDFglobalAttributes/Data_type)

Ion Bulk Flow Velocity (H only when in solar wind), GSE polar components

---> Ion Bulk Flow Velocity (H only when in solar wind), GSE cartesian components

Note: variables above are not fully filtered for telemetry errors

SPDF/CDAWeb. Please also acknowledge the data producer: L. Frank at U. Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: L. Frank at U. Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: L. Frank at U. Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/cpi/cpi_hpamom/1992/ge_HPAmom_cpi_19921006_v01.cdf. The most common cadence, 72000 [ms] = PT1M12S, occurred for 48.3957% of the 543 timesteps. 

Plasma Moments From Hot Plasma Analyzer (HPA) (from Master/CDFglobalAttributes/Data_type)

Plasma Moments, Key Parameters, Geotail CPI (Comprehensive Plasma Instrument)

GEOTAIL Prelaunch Report April 1992, SES-TD-92-007SY CPI-SW Solar Wind Analyzer   Key Parameters      Ion number density      Average proton energy      Bulk flow velocity CPI-HP Hot Plasma Analyzer   Key Parameters      Ion number density      Average proton energy      Average electron energy      Bulk flow velocity      Plasma pressure CPI-IC Ion Composition Analyzer   Key Parameters      Principal Species        H+        He++        He+        O+ CPI Survey Data will be made available via the World Wide Web as image files for the mission operation periods in a compressed time resolution for viewing and/or downloading with a WWW browser from the URL http://www-pi.physics.uiowa.edu/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/cpi/cpi_k0/1992/ge_k0_cpi_19920908_v03.cdf. The most common cadence, 64000 [ms] = PT1M4S, occurred for 84.5703% of the 433 timesteps. 

Ion Bulk Flow Velocity, ~GSE X-Y components (Hot Plasma 2D Anal) 

SPDF/CDAWeb. Please also acknowledge the data producer: K. Tsuruda at ISAS

SPDF/SSCWeb. Please also acknowledge the data producer: K. Tsuruda at ISAS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Tsuruda at ISAS

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/efd/efd_k0/1992/ge_k0_efd_19920908_v01.cdf. The most common cadence, 64000 [ms] = PT1M4S, occurred for all 845 timesteps. 

Electric Field Detector (from all.xml/instrument/description/@short)

Geotail Energetic Particles & Ion Composition (EPIC), Key Parameters

EPIC Instrument Description:  A) Supra-Thermal Ion Composition Spectrometer (STICS) Subsystem:     1) Ion Head/Telescope Coverage        Apperature Width:  53.4 polar deg        Apperature Center: Spacecraft spin plane B) Ion Composition Spectrometer (ICS) Subsystem:     1) Ion Head Coverage        Apperature Width:  60.0 polar deg excluding center 16.0 deg        Apperature Center: Spacecraft spin plane    2) Electron Detector Coverage        Apperature Width:  60.0 polar deg        Apperature Center: Spacecraft spin plane    3) Caution        ICS Ion channels can change between two sets of energy pass        bands from record to record; consult the associated energy        information to determine what the current values are.Anisotropy Calculation Qualification:  A) a1, a2, phi1 and phi2 are not    calculated when the count rate    is below a threshhold, currently    8 counts/96 seconds.

SPDF/CDAWeb. Please also acknowledge the data producer: D. Williams at APL/JHU

SPDF/SSCWeb. Please also acknowledge the data producer: D. Williams at APL/JHU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Williams at APL/JHU

Energetic Particles and Ion Composition (from all.xml/instrument/description/@short)

Ion Diff. Intensity, at 12 energies 67-1361 keV (EPIC/ICS) - spectrogram

Electron Energy,  time-varying lower bound (between 34-50 keV) on electron integral flux (EPIC/ICS), scalar 

He/H Ratio, of (82keV He/67keV H) & (233keV He/67keV H) Diff.  Intens. (EPIC/ICS)

O/H Ratio, at (247keV O/67keV H) & (1244keV O/67keV H) Diff. Intens. (EPIC/ICS)

He++/H+ Ratio, of (9.4-212keV He++/67keV H+) Diff. Inten. (EPIC/STICS), scalar

O+/H+ Ratio, of (9.4-212keV O+/67keV H+) Diff. Inten. (EPIC/STICS), scalar

>38keV Electron anis. param. (a0/a1/a2/phi1/phi2 from Fourier fit to elec. int. flux

9-212 keV/e H Anis. param. (a0/a1/a2/phi1/phi2 from Fourier fit to H flux , EPIC/STICS)

67 keV H Anis. param. (a0/a1/a2/phi1/phi2 from Fourier fit to H flux , EPIC/ICS)

129 keV H Anis. param. (a0/a1/a2/phi1/phi2 from Fourier fit to H flux , EPIC/ICS)

Electron Flux at 32 energies (100ev - 40keV) and 4 look directions (0/sun, 90/dusk, 180/tail, 270/dawn deg)

Ion Flux at 32 energies (100ev - 40keV) and 4 look directions (0/sun, 90/dusk, 180/tail, 270/dawn deg)

Key Parameters GE_K0_MGF from the Geotail Magnetic Field Instrument (MGF) in CDF

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/mgf/mgf_k0/1992/ge_k0_mgf_19920904_v01.cdf. The most common cadence, 64000 [ms] = PT1M4S, occurred for 92.8571% of the 13 timesteps. 

Standard deviation of sin fitting for magnetic field, in sensor coordinates

Text description of the experiment need to be defined by the developer

SPDF/CDAWeb. Please also acknowledge the data producer: H. Matsumoto at Kyoto Univ.

SPDF/SSCWeb. Please also acknowledge the data producer: H. Matsumoto at Kyoto Univ.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: H. Matsumoto at Kyoto Univ.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/pwi/pwi_k0/1992/ge_k0_pwi_19920908_v01.cdf. The most common cadence, 64000 [ms] = PT1M4S, occurred for 98.6951% of the 832 timesteps. 

Peak of spectral intensity for Efield comp (MCA) at 5 frequencies (.01-100 kHz)

Average of spectral intensity for Efield comp (MCA) at 5 frequencies (.01-100 kHz)

Peak of spectral intensity for Bfield comp (MCA) at 4 frequencies (.01-10 kHz)

Average of spectral intensity for Bfield comp (MCA) at 4 frequencies (.01-10 kHz)

Peak of the spectral intensities averaged over 64 sec for SFA, scalar

Average of the spectral intensities averaged over 64 sec for SFA, scalar

Frequency corresponding to the peak of the spectral intensities, scalar

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/orbit/spha/1992/ge_k0_spha_19920908_v02.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 901 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/orbit/pre_or/2022/ge_or_pre_20221230_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

Distributions and Plasma Moments, Definitive, Geotail CPI/SWA (Comprehensive Plasma Instrument / Solar Wind Analyzer)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/geotail/cpi/cpi_swa/1992/ge_sw_cpi_19921006_v01.cdf. The most common cadence, 48312 [ms] = PT48.312S, occurred for 48.7044% of the 827 timesteps. 

---> Ion Bulk Flow Polar angle Theta in degrees (0 toward North Ecliptic Pole, H only when in solar wind)

---> Ion Bulk Flow Azimuthal sector angle Phi in degrees (0 toward Sun, 90 toward Dusk, H only when in solar wind)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/giacobini_helio1day_position_19840101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 13514 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/giacobini_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/giotto/helio1day/giotto_helio1day_position_19920101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 366 timesteps. 

The hourly data are made by the linear interpolation of old daily files

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/giotto/helio1hr/giotto_helio1hr_position_19920101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 8783 timesteps. 

Satellite Situation Center Web, SSCWeb, System and Services Home Page

This Center is an Operational Unit of the Space Physics Data Facility (SPDF), and the National Space Science Data Center International Counterpart, World Data Center A for Rockets and Satellites (WDC-A-R&S). SSC Personnel and Software Systems support NASA and International Space Physics Activities by maintaining an Ephemeris Data Base for Scientific Satellites in Geocentric or Heliocentric Orbits which can be used to plan and support Analysis of coordinated Science Observations by multiple Satellites. The Space Physics Data Facility (SPDF), which now provide Software Development and Operational Support for SSC, are Part of the Heliophysics Science Division at NASA Goddard Space Flight Center with primary Contractor Support from ADNET Systems.

SPDF/CDAWeb. Please also acknowledge the data producer: SPDF at Goddard Space Flight Center

SPDF/SSCWeb. Please also acknowledge the data producer: SPDF at Goddard Space Flight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: SPDF at Goddard Space Flight Center

SPDF/SSCWeb and the HAPI project. Please also acknowledge the data producer: SPDF at Goddard Space Flight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes10/orbit/1997/goes10_ephemeris_ssc_19970101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 6147354 timesteps. 

---> Field line trace to the North Geographic Footprint - Longitude

---> The arc length of the line from the spacecraft to the north geographic magnetic field footprint

---> Field line trace to the South Geographic Footprint - Latitude

---> Field line trace to the South Geographic Footprint - Longitude 

---> The arc length of the line from the spacecraft to the south geographic magnetic field footprint

---> Field line trace to the North Geomagnetic Footprint - Longitude

---> The arc length of the line from the spacecraft to the north geomagnetic footprint

---> Field line trace to the South Geomagnetic Footprint - Latitude

---> Field line trace to the South Geomagnetic Footprint - Longitude

---> The arc length of the line from the spacecraft to the south geomagnetic field footprint

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes11/orbit/2000/goes11_ephemeris_ssc_20000101_v01.cdf. The most common cadence, 180000 [ms] = PT3M, occurred for all 2739360 timesteps. 

The NOAA Geostationary Operational  Environmental Satellite (GOES) key parameters are obtained from the Energetic Particle Sensor (EPS) and the magnetometer (MAG).  The key parameters are a subset of the  data available from the GOES Space Environment Monitor (SEM) instruments.The energetic particle fluxes are  given as five-minute averaged values and the vector magnetic field is given as one-minute average values.Flux values for three integral electron channels (E >0.6 MeV, E >2.0 MeV, and E >4.0 MeV) and one differential proton channel(0.7 MeV < E <4 MeV) are provided. These data are used by NOAA Space Environment Center (SEC) for the real-time monitoring and prediction of the conditions in the Earth's space environment.  A new series of GOES spacecraft began with GOES-8 launched on 4/13/94, GOES-9 launched on 5/23/95, GOES-10 launched on 4/25/97, GOES-11 launched on 5/3/2000, and  GOES-12 launched on 7/23/2001. Typically two satellites are maintained operational,one at about 135 degrees geographic west longitude and one at about 75 degrees geographic west longitude. The satellite inclination is typically within a few tenths of a degree of the geographic equator.However, the satellites can be moved, especially during the six months to one year following launch, and the inclination can increase after years of satellite operation.Instrument data quality flags are set from real-time telemetry, or, in the case of historically-processed data sets when telemetry is not available, fixed to a level-1 instrument status flag for all dataReference: Geostationary Operational Environmental Satellite GOES I-M System Description, compiled by John Savides, Space Systems/Loral, Palo Alto, California, December 1992. Dr. Terrance Onsager, NOAA/SEC, Terry.Onsager@noaa.gov, 303-497-5713, 325 Broadway, Boulder CO 80305 USA, or Ann Newman, NOAA/SEC, Ann.Newman@noaa.gov, 303-497-5100, 325 Broadway, Boulder CO 80305 USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes11/ep8_k0/2006/goes11_k0_ep8_20060623_v03.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Geostationary Operational Environmental Satellite 11 (from all.xml/observatory/description/@short)

The NOAA Geostationary Operational  Environmental Satellite (GOES) key parameters are obtained from the Energetic Particle Sensor (EPS) and and the magnetometer (MAG).  The key parameters are a subset of the  data available from the GOES Space Environment Monitor (SEM) instruments.The vector magnetic field is  given as one-minute averaged values in three coordinate systems: (1) Spacecraft (s/c) P,E,N, (2) GSM x,y,z, (3) GSE x,y,zs/c mag. field is defined as: Hp, perpendicular to the satellite orbital plane or parallel to the Earths spin axis in the case of a zero degree inclination orbit; He, perpendicular to Hp and directed earthwards; and Hn, perpendicular to both Hp and directed eastwards.These data are used by NOAA Space Environment Center (SEC) for the real-time monitoring and prediction of the conditions in the Earth's space environment.  A new series of GOES spacecraft began with GOES-8 launched on 4/13/94, GOES-9 launched on 5/23/95, GOES-10 launched on 4/25/97, GOES-11 launched on 5/3/2000, and GOES-12 launched on 7/23/2001.Typically two satellites are operational,one at about 135 degrees geographic west longitude and one at about 75 degrees geographic west longitude. The satellite inclination is typically within a few tenths of a degree of the geographic equator. However, the satellites can be moved, especially during the six months to one year following launch, and the inclination can increase after years of satellite operation.Instrument data quality flags are set from real-time telemetry, or, in the case of historically-processed data sets when telemetry is not available, fixed to a level-1 instrument status flag for all dataReference: Monitoring Space Weather with GOES Magnetometers, Singer, H.J, L. Matheson, R.Grubb A.Newman, and S.D.Bouwer, SPIE Proceedings, Volume 2812, 4-9 Aug 1996.  For more info, contact:Dr. Howard Singer, NOAA/SEC, Howard.Singer@noaa.gov,303-497-6959 325 Broadway,Boulder CO 80305 USA, or Ann Newman, NOAA/SEC, Ann.Newman@noaa.gov, 303-497-5100, 325 Broadway, Boulder CO 80305 USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes11/mag_k0/2006/goes11_k0_mag_20060623_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes12/orbit/2006/goes12_ephemeris_ssc_20060101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 525600 timesteps. 

The NOAA Geostationary Operational  Environmental Satellite (GOES) key parameters are obtained from the Energetic Particle Sensor (EPS) and and the magnetometer (MAG).  The key parameters are a subset of the  data available from the GOES Space Environment Monitor (SEM) instruments.The vector magnetic field is  given as one-minute averaged values in three coordinate systems: (1) Spacecraft (s/c) P,E,N, (2) GSM x,y,z, (3) GSE x,y,zs/c mag. field is defined as: Hp, perpendicular to the satellite orbital plane or parallel to the Earths spin axis in the case of a zero degree inclination orbit; He, perpendicular to Hp and directed earthwards; and Hn, perpendicular to both Hp and directed eastwards.These data are used by NOAA Space Environment Center (SEC) for the real-time monitoring and prediction of the conditions in the Earth's space environment.  A new series of GOES spacecraft began with GOES-8 launched on 4/13/94, GOES-9 launched on 5/23/95, and GOES-10 launched on 4/25/97.Typically two satellites are operational,one at about 135 degrees geographic west longitude and one at about 75 degrees geographic west longitude. The satellite inclination is typically within a few tenths of a degree of the geographic equator. However, the satellites can be moved, especially during the six months to one year following launch, and the inclination can increase after years of satellite operation.Instrument data quality flags are set from real-time telemetry, or, in the case of historically-processed data sets when telemetry is not available, fixed to a level-1 instrument status flag for all dataReference: Monitoring Space Weather with GOES Magnetometers, Singer, H.J, L. Matheson, R.Grubb A.Newman, and S.D.Bouwer, SPIE Proceedings, Volume 2812, 4-9 Aug 1996.  For more info, contact:Dr. Howard Singer, NOAA/SEC, Howard.Singer@noaa.gov,303-497-6959 325 Broadway,Boulder CO 80305 USA, or Ann Newman, NOAA/SEC, Ann.Newman@noaa.gov, 303-497-5100, 325 Broadway, Boulder CO 80305 USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes12/mag_k0/2003/goes12_k0_mag_20030408_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Geostationary Operational Environmental Satellite 12 (from all.xml/observatory/description/@short)

GOES Energetic Proton Electron and Alpha Detector Electron Fluxes reprocessed for scientific use 

Data has been recast from original NOAA netCDF files by SPDF. DATA CAVEATS/WARNINGS:integral electron flux corrected and flagged using complete set of Sauer coefficients and flagged when data are bad due to solar proton contamination; channel E3 not included in this version.

archive and instrument documentation at NOAA National Geophysical Data Center (NGDC)

SPDF/CDAWeb. Please also acknowledge the data producer: NOAA NGDC and SWPC at sem.goes@noaa.gov

SPDF/SSCWeb. Please also acknowledge the data producer: NOAA NGDC and SWPC at sem.goes@noaa.gov

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: NOAA NGDC and SWPC at sem.goes@noaa.gov

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes13/epead-electrons/e13ew_1min/2010/goes13_epead-science-electrons-e13ew_1min_20100501_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 44639 timesteps. 

Energetic Proton Electron and Alpha Detector Reprocessed Electron Fluxes for Science Use (from all.xml/instrument/description/@short)

EPEAD orientation flag. 0: A/W faces East and B/E faces West. 1: A/W faces West and B/E faces East. 2: yaw-flip in progress.

A/W Detector: Electron integral flux E1 >0.8 MeV (dead time corrected)

A/W Detector: Electron integral flux E2 >2 MeV (dead time corrected)

A/W Detector: Electron integral flux E1 >0.8 MeV (background, contamination and dead time corrected)

A/W Detector: Electron integral flux E2 >2 MeV (background, contamination and dead time corrected)

A/W Detector: Standard deviation, electron integral flux E1 >0.8 MeV (background, contamination and dead time corrected)

A/W Detector: Standard deviation, electron integral flux E2 >2 MeV (background, contamination and dead time corrected)

A/W Detector: Data quality flag pertaining to solar proton contamination for fluxes with energy E1 >.8 MeV (0 if contamination is sufficiently small that the correction and electron fluxes are valid; 1 if contamination is too large and the electron fluxes are not valid.)

A/W Detector: Data quality flag pertaining to solar proton contamination for fluxes with energy E2 >2 MeV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes13/orbit/2006/goes13_ephemeris_ssc_20060101_v01.cdf. The most common cadence, 180000 [ms] = PT3M, occurred for all 98400 timesteps. 

GOES-13 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 1 minute electron fluxes 40-475 keV

Data has been recast from original NOAA netCDF files by SPDF. DATA CAVEATS/WARNINGS: The MagED data may not be accurate at times due to instrument limitations such as dead time and proton contamination. Every effort is made to reduce these effects but uncertainties are inevitable. Additionally, the detectors may suffer from intermittent noise problems. Please contact Juan V. Rodriguez (sem.goes@noaa.gov) with questions or concerns.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes13/eps-maged/19me15_1min/2006/goes13_eps-maged_1min_20060601_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for 82.2218% of the 35519 timesteps. 

Energetic Particle Sensor - Magnetospheric Electron Detector (from all.xml/instrument/description/@short)

Average Electron Flux in Telescope 9 (oriented 70+Y, pointing North or South depending on yaw state) for 5 energy bands 40-475 keV (as time-series plots; corrected for dead-time errors and other contamination sources)

---> Electron Flux in Telescope 6 (oriented 35+Y, pointing N or S)

---> Electron Flux in Telescope 3 (oriented 70-X, pointing equatorial E or W)

---> Electron Flux in Telescope 4 (oriented 35-X, pointing equatorial E or W)

---> Electron Flux in Telescope 2 (oriented 35+X, pointing equatorial W or E)

---> Electron Flux in Telescope 5 (oriented 70+X, pointing equatorial W or E)

---> Electron Flux in Telescope 8 (oriented 35-Y, pointing S or N)

---> Electron Flux in Telescope 7 (oriented 70-Y, pointing S or N)

Average Electron Flux at 40 keV for 9 directions ordered north to south (101 to 109) or south to north depending on yaw state in time-series plots; corrected for dead-time errors and other contamination sources

Electron Fluxes uncorrected for contamination (as flux by energy spectrograms for each telescope in orientation order; corrected for dead-time errors)

---> [NO PLOTS] Quality flag (non-zero value indicates a telemetry processing issue)

Inclination -- the angle between the plane of the orbit and the equatorial plane measured counter-clockwise from true East

GOES-13 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 5 minute electron fluxes 40-475 keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes13/eps-maged/19me15_5min/2011/goes13_eps-maged_5min_20110101_v01.cdf. The most common cadence, 300000000000 [ns] = PT5M, occurred for all 8927 timesteps. 

[NO PLOTS] Quality flag (non-zero value indicates a telemetry processing issue)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes13/eps-pitch-angles_1min/2010/goes13_eps-pitch-angles_1min_20100501_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 44639 timesteps. 

Pitch angles of MAGED and MAGPD telescopes 1-9 calculated from GOES magnetometer field vector

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes14/epead-electrons/e13ew_1min/2012/goes14_epead-science-electrons-e13ew_1min_20121001_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 44639 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes14/orbit/2009/goes14_ephemeris_ssc_20090101_v01.cdf. The most common cadence, 180000 [ms] = PT3M, occurred for all 84480 timesteps. 

GOES-14 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 1 minute electron fluxes 40-475 keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes14/eps-maged/19me15_1min/2009/goes14_eps-maged_1min_20090701_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for 82.2218% of the 36703 timesteps. 

GOES-14 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 5 minute electron fluxes 40-475 keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes14/eps-maged/19me15_5min/2010/goes14_eps-maged_5min_20100401_v01.cdf. The most common cadence, 300000000000 [ns] = PT5M, occurred for all 8639 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes14/eps-pitch-angles_1min/2012/goes14_eps-pitch-angles_1min_20121001_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 44639 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes15/epead-electrons/e13ew_1min/2010/goes15_epead-science-electrons-e13ew_1min_20100301_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 8639 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes15/orbit/2010/goes15_ephemeris_ssc_20100101_v01.cdf. The most common cadence, 180000 [ms] = PT3M, occurred for all 137280 timesteps. 

GOES-15 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 1 minute electron fluxes 40-475 keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes15/eps-maged/19me15_1min/2010/goes15_eps-maged_1min_20100301_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for 82.2218% of the 36703 timesteps. 

GOES-15 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 5 minute electron fluxes 40-475 keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes15/eps-maged/19me15_5min/2011/goes15_eps-maged_5min_20110201_v01.cdf. The most common cadence, 300000000000 [ns] = PT5M, occurred for all 8063 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes15/eps-pitch-angles_1min/2010/goes15_eps-pitch-angles_1min_20100301_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 8639 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes16/orbit/2016/goes16_ephemeris_ssc_20160101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 41104 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes17/orbit/2018/goes17_ephemeris_ssc_20180101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 411840 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes18/orbit/2022/goes18_ephemeris_ssc_20220101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 416160 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes08/orbit/1994/goes8_ephemeris_ssc_19940101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 11865600 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/goes/goes09/orbit/1995/goes9_ephemeris_ssc_19950101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 7666560 timesteps. 

The GOLD mission of opportunity flies an ultraviolet (UV) imaging spectrograph on a geostationary satellite to measure densities and temperatures in Earth's thermosphere and ionosphere and to understand the global-scale response to forcing in the integrate Sun-Earth system. Visit 'https://gold.cs.ucf.edu' for more details.

This is a data product from the NASA Global-scale Observations of the Limb and Disk (GOLD) mission, an Heliophysics Explorer mission of opportunity launched in January 2018.  Responsibility of the mission science falls to the Principal Investigator, Dr. Richard Eastes at University of Colorado/LASP.  Validation of the L1B data products falls to the instrument lead investigators/scientists. * EUV  Dr. Bill McClintock Validation of the L2 data products falls to Computational Physics, Inc. * Dr. Jerry Lumpe  (https://gold.cs.ucf.edu/). Overall validation of the products is overseen by the GOLD Project Scientist Dr. Alan Burns. Users of these data should contact and acknowledge the Principal Investigator Dr. Richard Eastes and the party directly responsible for the data product and the NASA Explorers Project Office.

Eastes, R.W., McClintock, W.E., Burns, A.G. et al. Space Sci. Rev. (2017) vol. 212, pp.383.

SPDF/CDAWeb. Please also acknowledge the data producer: Richard Eastes at University of Colorado/LASP

SPDF/SSCWeb. Please also acknowledge the data producer: Richard Eastes at University of Colorado/LASP

Global-scale Observations of the Limb and Disk (from all.xml/observatory/description/@short)

Peak electron density (from all.xml/instrument/description/@short)

Global-scale Observations of the Limb and Disk (from Master/CDFglobalAttributes/Source_name)

GOLD Application ID 0x?: Level 2 Day Disk Science Data (from Master/CDFglobalAttributes/Data_type)

Column density ratio of atomic oxygen to molecular nitrogen (from all.xml/instrument/description/@short)

Journal article on disk images of neutral temperature from the Global‐scale Observations of the Limb and Disk (GOLD) mission

Evans  J. S., Lumpe, J. D., Eastes, R. W., Correira, J., Aryal, S., Laskar, F., et al., Journal of Geophysical Research: Space Physics, 129, e2024JA032424.

Disk neutral temperature (from all.xml/instrument/description/@short)

Vertical Total Electron Content (from all.xml/instrument/description/@short)

GPS-deduced ROTI index: standard deviation of rate of change of Total Electron Content (TEC) in a 5 min interval every 15 min; world maps and movies

The ROTI index is the standard deviation of the Rate of change of TEC (ROT) during a 5-minute interval. TEC is the Total Electron Content measured between a GPS satellite and ground receiver station.

Jet Propulsion Laboratory, JPL, Ionospheric and Atmospheric Remote Sensing Web Site

SPDF/CDAWeb. Please also acknowledge the data producer: Xiaoqing Pi at Jet Propulsion Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Xiaoqing Pi at Jet Propulsion Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Xiaoqing Pi at Jet Propulsion Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/gps/roti15min_jpl/2012/gps_roti15min_jpl_20121129_v01.cdf. The most common cadence, 900000 [ms] = PT15M, occurred for all 95 timesteps. 

Global Positioning System (from all.xml/observatory/description/@short)

ROTI index 15 minute (from all.xml/instrument/description/@short)

Global Positioning System (from Master/CDFglobalAttributes/Source_name)

GPS-deduced 15-minute Total Electron Content (TEC) global maps and movies, UPC= U Politec. Catalonia Barcelona Spain

The IGS global system of satellite tracking stations, Data Centers, and Analysis Centers puts high-quality GPS data and data products on line in near real time to meet the objectives of a wide range of scientific and engineering applications and studies.  The IGS collects, archives, and distributes GPS observation data sets of sufficient accuracy to satisfy the objectives of a wide range of applications and experimentation.  These data sets are used by the IGS to generate the data products mentioned above which are made available to interested users through the Internet.  In particular, the accuracies of IGS products are sufficient for the improvement and extension of the International Terrestrial Reference Frame (ITRF), the monitoring of solid Earth deformations, the monitoring of Earth rotation and variations in the liquid Earth (sea level, ice-sheets, etc.), for scientific satellite orbit determinations, ionosphere monitoring, and recovery of precipitable water vapor measurements.  The primary mission of the International GPS Service, as stated in the organization's 2002-2007 Strategic Plan, is     The International GPS Service is committed to providing the highest quality data and products as the standard for global navigation satellite systems (GNSS) in support of Earth science research, multidisciplinary applications, and education. These activities aim to advance scientific understanding of the Earth system components and their interactions, as well as to facilitate other applications benefiting society.The IGS Terms of Reference (comparable to the by-laws of the organization) describes in broad terms the goals and organization of the IGS.  To accomplish its mission, the IGS has a number of components: an international network of over 350 continuously operating dual-frequency GPS stations, more than a dozen regional and operational data centers, three global data centers, seven analysis centers and a number of associate or regional analysis centers. The Central Bureau for the service is located at the Jet Propulsion Laboratory, which maintains the Central Bureau Information System (CBIS) and ensures access to IGS products and information. An international Governing Board oversees all aspects of the IGS.  The IGS is an approved service of the International Association of Geodesy since 1994 and is recognized as a member of the Federation of Astronomical and Geophysical Data Analysis Services (FAGS) since 1996. The IGS collects, archives, and distributes GPS observation data sets of sufficient accuracy to meet the objectives of a wide range of scientific and engineering applications and studies. These data sets are used to generate the following products:  * GPS satellite ephemerides  * GLONASS satellite ephemerides  * Earth rotation parameters  * IGS tracking station coordinates and velocities  * GPS satellite and IGS tracking station clock information  * Zenith tropospheric path delay estimates  * Global ionospheric mapsIGS products support scientific activities such as improving and extending the International Earth Rotation Service (IERS) Terrestrial Reference Frame (ITRF), monitoring deformations of the solid Earth and variations in the liquid Earth (sea level, ice sheets, etc.), and in Earth rotation, determining orbits of scientific satellites and monitoring the ionosphere. For example, geodynamics investigators who use GPS in local regions can include data from one or more nearby IGS stations, fix the site coordinates from such stations to their ITRF values, and more importantly, use the precise IGS orbits without further refinement. Data from an investigator's local network can then be analyzed with maximum accuracy and minimum computational burden. Furthermore, the results will be in a well-defined global reference frame.  An additional aspect of IGS products is for the densification of the ITRF at a more regional level. This is accomplished through the rigorous combination of regional or local network solutions utilizing the Solution Independent Exchange Format (SINEX) and a process defined in the densification section.  In the future, the IGS infrastructure could become a valuable asset for support of new ground-based applications -- and could also contribute to space-based missions in which highly accurate flight and ground differential techniques are required.

SPDF/CDAWeb. Please also acknowledge the data producer: International Global Navigation Satellite Systems (GNSS) Service Iono Working Group at 

SPDF/SSCWeb. Please also acknowledge the data producer: International Global Navigation Satellite Systems (GNSS) Service Iono Working Group at 

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: International Global Navigation Satellite Systems (GNSS) Service Iono Working Group at 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/gps/tec15min_igs/1995/gps_tec15min_igs_19950516_v01.cdf. The most common cadence, 900000 [ms] = PT15M, occurred for all 95 timesteps. 

Total Electron Content 15minute (from all.xml/instrument/description/@short)

UPC, Num. Stations Rapid-15min, Number of Ground Stations Used, (Rapid product, 15 min res., 24 hr latency)

UPC, Num satellites Rapid-15min, Number of GPS satellites used, (Rapid product, 15 min res., 24 hrs latency)

GPS-deduced 1-hour Total Electron Content (TEC) global maps and movies, UPC= U Politec. Catalonia Barcelona Spain, ESA= ESOC Darmstadt Germany (starting 20 Feb 2011) 

SPDF/CDAWeb. Please also acknowledge the data producer: International Global Navigation Satellite Systems (GNSS) Service Ionosphere Working Group at 

SPDF/SSCWeb. Please also acknowledge the data producer: International Global Navigation Satellite Systems (GNSS) Service Ionosphere Working Group at 

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: International Global Navigation Satellite Systems (GNSS) Service Ionosphere Working Group at 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/gps/tec1hr_igs/1995/gps_tec1hr_igs_19950516_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

Total Electron Content 1hour (from all.xml/instrument/description/@short)

UPC, Num. Stations Rapid-1h, Number of ground stations used, (Rapid product, 1 hr res., 24 hrs latency)

UPC, Num satellites Rapid-1h, Number of GPS satellites used, (Rapid product, 1 hr, 24 hrs latency)

GPS-deduced 2-hour Total Electron Content (TEC) maps and movies, IGS= Average of 4 methods, incl. CODE= U Bern Switzerland, ESA= ESOC Darmstadt Germany, JPL= Jet Propulsion Lab. Pasadena USA, UPC= U Politec. Catalonia Barcelona Spain

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/gps/tec2hr_igs/1998/gps_tec2hr_igs_19980601_v01.cdf. The most common cadence, 7200000 [ms] = PT2H, occurred for all 11 timesteps. 

Total Electron Content 2hour (from all.xml/instrument/description/@short)

IGS, Num Stations Final-2h, Number of ground stations used, (Final product, 2 hr res., 12 day latency)

IGS, Num stations Rapid-2h, Number of ground stations used, (Rapid product, 2 hr res., 12 hr latency)

IGS, Num satellites Final-2h, Number of GPS satellites used, (Final product, 2 hr res., 12 day latency)

IGS, Num satellites Rapid-2h, Number of GPS satellites used, (Rapid product, 2 hr res., 12 hr latency)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/halebopp_helio1day_position_19960101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 8400 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/halebopp_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/halley_helio1day_position_19840101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 13514 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/halley_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9990% of the 306720 timesteps. 

This dataset contains high resolution interplanetary magnetic field data in six-second averages as measured by the Helios 1 tri-axial fluxgate magnetometer experiment. Magnetic field vector components in nanotelsa [nT] are given in solar-ecliptic (SE) spacecraft-centered coordinates with one file for each day.  The magnetic field magnitude and standard deviations of the vector components are also included. 

SPDF/CDAWeb. Please also acknowledge the data producer: Mariani/Ness at University of Rome, CNR/Istituto Fisica Interplanetario, and NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Mariani/Ness at University of Rome, CNR/Istituto Fisica Interplanetario, and NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Mariani/Ness at University of Rome, CNR/Istituto Fisica Interplanetario, and NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/mag/6sec_nessmag_cdaweb/1974/hel1_6sec_nessmag_19741215_v01.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for 99.7334% of the 11597 timesteps. 

High Time Resolution 6sec (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/mag/6sec_nessmag_cdaweb/1976/hel2_6sec_nessmag_19760117_v01.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for 99.7734% of the 8365 timesteps. 

General information about initial ascii files: This subdirectory contains daily files of 40.5 sec Helios magnetic field and plasma data described below.  It also contains a file of software written by Aaron Roberts, readhelios40s_dat.pro, for creating alfvenicity graphs.       The Helios mission consisted of two spacecraft launched into the inner heliosphere, both executing orbits from 0.3 to 1 AU with roughly a six month orbital period.     Magnetic field data were recorded at high resolution, with plasma data recorded  at approximately 40.5 s resolution.  These datasets give the highest resolution  plasma (proton and helium) moments with the corresponding average magnetic field  for each plasma measurement.  There are results from two plasma sensors, one of  which gives the vector velocity.         The coverage is best in the early years and varies considerably for the rest of the mission.  The files Helios1_stats and Helios2_stats give the year, day of  year, number of points, and percentage of possible points for the days included  in the sets.  There is no coverage for many days, with the main reason being that  the spacecraft pass behind the Sun with respect to the Earth, thus cutting off  communication.              The overall intervals covered are:  Helios 1:  1974 day 346 to                     1985 day 247              Helios 2:  1976 day 017 to               1980 day 068       The present set of files were produced by R. Schwenn and obtained from J. Luhmann. They have been reformatted by Aaron Roberts to assure spaces between the variables,  and in the process the HGI longitude and the RTN versions of the variables were added for convenience.  Also, spacecraft positions were interpolated to make them  distinct. The fill value for missing data in the original files was either -1 or 0;  all these have been changed to 0. The other entries are directly from the original  files.            R. Schwenn should be acknowledged for plasma data and F. Neubauer for magnetic field data.  GSFC/SPDF nssdcftp (or successor) should be acknowledged as the immediate  source of the data.               * The RTN components were calculated from the SSE XYZ components using R -> -X, T -> -Y, and N -> Z.  The Cartesian coordinates for B and the angles for V are the  original variables in the file, and no correction was made in the conversion to RTN  for the actual spacecraft position.  Since RTN and SSE are defined relative to the helioequatorial plane and to the ecliptic plane, respectively, and since these planes are inclined by 7.25 degrees relative to each other (heliocentric orbits of Earth,  Helios 1 and Helios 2 are virtually co-planar), this introduces errors of up to 100% * (1 - cos 7.25) = 1% in the RTN components.  However, the V and B are consistent with each other and can be compared directly.                 (text by Aaron Roberts, with edits by Joe King; October, 2008)  

SPDF/CDAWeb. Please also acknowledge the data producer: R. Schwenn, F. M. Neubauer at Max Planck Institute for Solar System Research, University of Cologne

SPDF/SSCWeb. Please also acknowledge the data producer: R. Schwenn, F. M. Neubauer at Max Planck Institute for Solar System Research, University of Cologne

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Schwenn, F. M. Neubauer at Max Planck Institute for Solar System Research, University of Cologne

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/merged/mag_plasma/40sec_cdf/1974/helios1_40sec_mag-plasma_19741212_v01.cdf. The most common cadence, 41000 [ms] = PT41S, occurred for 47.7011% of the 664 timesteps. 

Merged magnetic field, plasma, trajectory (from all.xml/instrument/description/@short)

40 sec Helios magnetic field and plasma data (from Master/CDFglobalAttributes/Data_type)

Helios-1 merged hourly magnetic field, plasma, proton fluxes, and ephermis data

The HELIOS-1 spacecraft was one of the pair of deep space probes developed by the Federal Republic of Germany (FRG) in a cooperative program with NASA.  The purpose of the mission was to make pioneering measurements of the interplanetary medium from the vicinity of the Earth's orbit to 0.3 AU. (The planet Mercury is at 0.4 AU.)Data coverage for selected parameters for this data set is: interplanetary  magnetic  field (1974-12-14 - 1981-06-14), solar wind plasma (1974-12-12 - 1980-12-31), and spacecraft trajectory coordinates (1974-12-10 - 1981-06-14).Magnetic field data were provided by Prof. F. Mariani, Istituto di Fisica G. Marconi, Rome, Italy; Plasma data - by Dr. R. Schwenn, Max-Planck-Institut fur Aeronomie, Lindau, Germany.Time Coverage of merged files: December 10, 1974 - June 14, 1981.Helios-1 data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions:All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.Magnetic field components were transformed to RTN system.Trajectory data, interplanetary magnetic field data, and plasma data were merged into individual hourly records.Data gaps were filled with dummy numbers for the missing hours or entire days to make all files of equal length.  The character '9' is used to fill all fields for missing data according to their format, e.g. ' 9999.9' for a field with the FORTRAN format F7.1. Note that format F7.1 below really means (1X,F6.1),etc.

SPDF/CDAWeb. Please also acknowledge the data producer: N. Ness, F. Neubauer, F. Mariani (magnetic field), H. Rosenbauer, R. Schwenn (plasma) and J. Freeman at all affiliated with ESA or NASA

SPDF/SSCWeb. Please also acknowledge the data producer: N. Ness, F. Neubauer, F. Mariani (magnetic field), H. Rosenbauer, R. Schwenn (plasma) and J. Freeman at all affiliated with ESA or NASA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: N. Ness, F. Neubauer, F. Mariani (magnetic field), H. Rosenbauer, R. Schwenn (plasma) and J. Freeman at all affiliated with ESA or NASA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/coho1hr_magplasma/1974/helios1_coho1hr_merged_mag_plasma_19740101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Merged Trajectory, Magnetic Field, Plasma, and Proton Fluxes (from all.xml/instrument/description/@short)

1 Hour Time Resolution from cohoweb (from Master/CDFglobalAttributes/Data_type)

HELIOS-A and -B spacecrafts were the pair of deep space probes developed by the Federal Republic of Germany (FRG) in a cooperative program with NASA. The purpose of the mission was to make pioneering measurments of the interplanetary medium from the vicinity of the earth"s orbit to 0.3 AU. The objective of experiment (E6) was to study high-energy, charged, cosmic-ray particles of solar, planetary, and galactic origin in interplanetary space. Protons and alpha particles with eneries >1.3 MeV/nucleon, and electrons >0.3 MeV were measured within interplanetary space over the range from 0.3 to 1.0 AU. The instrument, a particle telescope with 55-deg field of view, consisted of five semiconductor detectors, one sapphire Cherenkov counter, and one scintillation counter, all enclosed by an anticoincidence cylinder. The telescope was calibrated prior to launch using radioactive sources, particle acceletors, and ground-level muons. It measured protons and alpha particles in six channels (1.3-3.3, 3.3-13, 13-27, 27-37, 37-45, and >45 MeV/nucleon) and electrons in five energy channels (0.3-0.8, 0.8-2, 2-3, 3-4, and >4 MeV). For more detail see pp.253-257 of Raumfahrtforschung, v.19, n. 5, 1975. The h-a-cr*.dat and h-b-cr*.dat files contains hourly averaged fluxes of electrons, protons and alpha particles in the MeV ranges. The files were written in ASCII-codes. Each record contains 10 hourly averages. The differential fluxes (particles/sq.m, s, sr, MeV) cover, in several bands, the energy range 0.3-2.0 MeV for electrons, 4.0-51 MeV for protons, and 2.0-48 MeV for alpha particles.  Also provided are the integral fluxes of alphas above 48 MeV, and protons above 51 MeV. For some of the energy channels, the standard deviations of the averages are also provided. Each file is preceded by a header record, providing the start and stop times of the data in the file. The acronyms for the rate channels are composed of a letter and an indication of the energy range in MeV/nucleon for protons and alpha particles respectively. MeV for electrons. The counting rates are given as particles/m^2  sec sr MeV/N, except for the integral channels P>51 and A>48 which are given as particles/ m^2 sec sr. Note: 1. Negative rates (-0.99999E+04) indicate missing or invalid data. 2. The energy boundaries for the electron channels E 0.2-0.8 and E 0.8-2are only rough estimates.

SPDF/CDAWeb. Please also acknowledge the data producer:  H. Kunow at University of Kiel

SPDF/SSCWeb. Please also acknowledge the data producer:  H. Kunow at University of Kiel

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer:  H. Kunow at University of Kiel

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/e6_particle_flux/1hour_cdf/1974/helios1_e6_1hour_particle_flux_19741212_v01.cdf. The most common cadence, 840000 [ms] = PT14M, occurred for 14.4691% of the 12532 timesteps. 

E6 - Merged proton, electron and alpha particle fluxes. (from all.xml/instrument/description/@short)

Helios Hourly Cosmic Ray Particles (from Master/CDFglobalAttributes/Data_type)

HELIOS-A and -B spacecrafts were the pair of deep space probes developed by the Federal Republic of Germany (FRG) in a cooperative program with NASA. The purpose of the mission was to make pioneering measurments of the interplanetary medium from the vicinity of the earth"s orbit to 0.3 AU. The objective of experiment (E6) was to study high-energy, charged, cosmic-ray particles of solar, planetary, and galactic origin in interplanetary space. Protons and alpha particles with eneries >1.3 MeV/nucleon, and electrons >0.3 MeV were measured within interplanetary space over the range from 0.3 to 1.0 AU. The instrument, a particle telescope with 55-deg field of view, consisted of five semiconductor detectors, one sapphire Cherenkov counter, and one scintillation counter, all enclosed by an anticoincidence cylinder. The telescope was calibrated prior to launch using radioactive sources, particle acceletors, and ground-level muons. It measured protons and alpha particles in six channels (1.3-3.3, 3.3-13, 13-27, 27-37, 37-45, and >45 MeV/nucleon) and electrons in five energy channels (0.3-0.8, 0.8-2, 2-3, 3-4, and >4 MeV). For more detail see pp.253-257 of Raumfahrtforschung, v.19, n. 5, 1975. The h-a-cr*.dat and h-b-cr*.dat files contains hourly averaged fluxes of electrons, protons and alpha particles in the MeV ranges. The files were written in ASCII-codes. Each record contains 10 hourly averages. The differential fluxes (particles/sq.m, s, sr, MeV) cover, in several bands, the energy range 0.3-2.0 MeV for electrons, 4.0-51 MeV for protons, and 2.0-48 MeV for alpha particles.  Also provided are the integral fluxes of alphas above 48 MeV, and protons above 51 MeV. For some of the energy channels, the standard deviations of the averages are also provided. Each file is preceded by a header record, providing the start and stop times of the data in the file. The acronyms for the rate channels are composed of a letter and an indication of the energy range in MeV/nucleon for protons and alpha particles respectively. MeV for electrons. Note: 1. Negative rates (-0.99999E+04) indicate missing or invalid data. 2. The energy boundaries for the electron channels E 0.2-0.8 and E 0.8-2are only rough estimates.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/e6_particle_flux_kunow/1hour_cdf/1974/helios1_e6_kunow_1hour_particle-flux_19741212_v01.cdf. The most common cadence, 840000 [ms] = PT14M, occurred for 12.7292% of the 9644 timesteps. 

Merged proton, electron and alpha particle fluxes. (from all.xml/instrument/description/@short)

Helios E6 Experiment (Kunow) (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/helio1day/helios1_helio1day_position_19741210_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 4038 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios1/helio1hr/helios1_helio1hr_position_19741210_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 96935 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/merged/mag_plasma/40sec_cdf/1976/helios2_40sec_mag-plasma_19760117_v01.cdf. The most common cadence, 41000 [ms] = PT41S, occurred for 48.9068% of the 850 timesteps. 

Helios-2 merged hourly magnetic field, plasma, proton fluxes, and ephermis data

The HELIOS-1 spacecraft was one of the pair of deep space probes developed by the Federal Republic of Germany (FRG) in a cooperative program with NASA.  The purpose of the mission was to make pioneering measurements of the interplanetary medium from the vicinity of the Earth's orbit to 0.3 AU. (The planet Mercury is at 0.4 AU.)Data coverage for selected parameters for this data set is: interplanetary  magnetic  field (1976-01-18 - 1980-03-04), solar wind plasma (1976-01-18 - 1980-03-04), and spacecraft trajectory coordinates (1976-01-18 - 1980-03-04).Magnetic field data were provided by Prof. F. Mariani, Istituto di Fisica G. Marconi, Rome, Italy; Plasma data - by Dr. R. Schwenn, Max-Planck-Institut fur Aeronomie, Lindau, Germany.Time Coverage of merged files: January 1, 1976 - March 4, 1980.Helios-2 data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions:All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.Magnetic field components were transformed to RTN system.Trajectory data, interplanetary magnetic field data, and plasma data were merged into individual hourly records.Data gaps were filled with dummy numbers for the missing hours or entire days to make all files of equal length.  The character '9' is used to fill all fields for missing data according to their format, e.g. ' 9999.9' for a field with the FORTRAN format F7.1. Note that format F7.1 below really means (1X,F6.1),etc.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/coho1hr_magplasma/1976/helios2_coho1hr_merged_mag_plasma_19760101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/e6_particle_flux/1hour_cdf/1976/helios2_e6_1hour_particle_flux_19760117_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 18.6221% of the 7901 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/e6_particle_flux_kunow/1hour_cdf/1976/helios2_e6_kunow_1hour_particle-flux_19760117_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 18.6221% of the 7901 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/helio1day/helios2_helio1day_position_19760101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 3652 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/helios/helios2/helio1hr/helios2_helio1hr_position_19760101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 87671 timesteps. 

Gurnett, D. A., and L. A. Frank, A region of intense plasma wave turbulences on auroral field lines, JGR, 82, 1031, 1977Farrell, W. M., and J. A. Van Allen, Observations of the Earth"s  polar cleft at large radial distances with Hawkeye 1 magnetometer, JGR, 95, 20945, 1990

SPDF/CDAWeb. Please also acknowledge the data producer: J. Van Allen at University of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: J. Van Allen at University of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Van Allen at University of Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/hawkeye/mag/mag_h0/1974/hk_h0_mag_19740606_v01.cdf. The most common cadence, 1890 [ms] = PT1.89S, occurred for 66.5155% of the 20977 timesteps. 

High resolution level-0 Data (from Master/CDFglobalAttributes/Data_type)

Despin Method (0:not despun; 1 optical aspect; 2:sun pulse; 3:array voltage; 4 mag field model; 4/5 - solar array method)

Estimate of the angular uncertainty in Mag Field direction (set to zero for despin = 1 or 2), scalar

Hk Electric and Magnetic Field Radio Frequency Spectrum Analyzer High Time Resolution

BUILD_DATE:                     1974-01-01INSTRUMENT_MASS:         0.23 (LESS BOOMS) kgINSTRUMENT_HEIGHT:       0.058 mtINSTRUMENT_LENGTH:       0.140 mtINSTRUMENT_WIDTH:         0.140 mtINSTRUMENT_MANUFACTURER_NAME:   UNIV IOWAINSTRUMENT_SERIAL_NUMBER:     VLF-05                         Electric AntennaThe electric antenna on HAWKEYE consisted of two extendible beryllium copper elements 0.025 inch in diameter which could be extended to a maximum tip-to-tip length of 42.7 m. Except for the outermost 6.1 m of each element, which had a conducting surface, the antenna was coated with Pyre-ML to electrically insulate the antenna from the surrounding plasma. The insulating coating was required to insulate the antenna from the perturbing effects of the plasma sheath surrounding the spacecraft body. At high altitudes, the thickness of the plasma sheath surrounding  the spacecraft body was quit large, on the order of 9 m. Since the conducting portion of the antenna must extend beyond the plasma sheath, it was necessary that the antenna be rather long, at least 30 m. tip-to-tip. The antenna mechanism used on HAWKEYE was the Dual-Tee extendible antenna manufactured by Fairchild Industries. The antenna length was 42.49 meters after final deployment until the last orbit, when an attempt was made to retract the antenna to reduce the spacecraft drag.                   Magnetic Antenna The magnetic antenna for this experiment consisted of a search coil with a high permeability core mounted on a boom approximately 1.5 m. from the centerline of the spacecraft body. The boom was a three element telescoping device developed at the University of Iowa. The boom supporting the flux gate magnetometer on the opposite side of the spacecraft was the same type. Both booms were extended simultaneously by an electric motor.           The search coil core was .305 m. long and was wound with approximately 20,000 turns of copper wire. The axis of the search coil was parallel to the spin axis of the spacecraft. A preamplifier was located with the sensor to provide low-impedance signals to the main electronics package in the spacecraft body. The frequency range of the search coil antenna was from 1.0 Hz to 10.0 kHz.                         Electronics The potential difference between the electric antenna elements was amplified by a high input impedance differential amplifier to provide a 0 to 5 volt analog voltage, V-Diff, to the spacecraft encoder. As the spacecraft rotated the potential difference between the antenna elements  varied sinusoidally at the spacecraft rotation rate, with an amplitude proportional to the electric field strength and a phase determined by the direction of the electric field. The frequency response of the differential amplifier was 0.05 Hz to 10 Hz and included the entire range of spin rates expected as the antenna was deployed. The V-Diff signal was sampled 6 times each frame by the encoder. The gain of the differential amplifier could be controlled by command to provide dynamic ranges of +/-0.5 and +/-8.0 volts for the antenna potential difference measurements.           Signals from the electric antenna in the frequency range from 10 kHz to 200 kHz were analyzed by the narrow band step frequency receiver. The primary purpose of this receiver was to provide very good frequency resolution in the neighborhood of the electron plasma frequency and upper hybrid resonance frequency. The step frequency receiver consisted of 8 narrow band filters (+/-5% band-width) which were sequentially switched into a log compressor. The  log compressor provided a 0 to 5 volt analog voltage, SFR, to the spacecraft encoder. The switch (S4) position was controlled by clock lines from the spacecraft encoder and was stepped through 8 frequencies, 13.3, 17.8, 23.7, 31.1, 42.2, 56.2, 100, and 178 kHz, at a rate of four frequencies per telemetry frame (5.76 seconds). The log compressor provided a 0 to 5 volt analog voltage, SFR, to the spacecraft encoder which was proportional to the logarithm of the signal strength over a dynamic range of 100 db.           The 8-channel spectrum analyzer  provided relatively coarse frequency spectrum measurements of both electric and magnetic fields over a broad frequency range of 1.0 Hz to 10.0 kHz. The primary purpose of the 8-channel spectrum analyzer was to provide field strength measurements to complement the high-resolution frequency-time spectra from the wide-band receiver.           Switches S1 and S2 were controlled by clock lines from the spacecraft encoder and commutate the filter outputs to two log compressors which provided field strength measurements SA-1 and SA-2 (0 to 5 volts) to the spacecraft encoder. These outputs were sampled twice per telemetry frame. Switch S3, which was controlled by a clock line, commutates the electric and magnetic field signals to the 8-channel spectrum analyzer.          Approximately every 5 minutes the impedance of the electric antenna was determined at a frequency of 17 Hz by driving a small AC current into the antennas and measuring the resultant voltage on the antennas with the 8-channel spectrum analyzer. The 17 Hz oscillator was gated on for 1 frame out of every 64 frames by a clock line.           Immediately following the impedance measurement the pulser circuit produced a 10 volt pulse with a duration of 20 micro- seconds. This pulse was to stimulate local plasma resonances, such as plasma oscillation, from which the electron density could be determined. A pulse of +10 volts was applied to one antenna element and a -10 volt pulse was applied to the opposite antenna element. The pulser was switched on by command. The pulser was on when the experiment was in VLF45 mode and off when the experiment was in the VLF10 mode. The pulser voltage was coupled to the antenna through a 220 pf capacitor which would have allowed some meaningful data to be obtained from the experiment even if the pulser output were to short to ground. The pulse was applied at the end of the impedance measurement frame. The potential difference between the electric antenna elements was amplified by a high input impedance differential amplifier to provide a 0 to 5 volt analog voltage, V-Diff, to the spacecraft encoder. As the spacecraft rotated the potential difference between the antenna elements  varied sinusoidally at the spacecraft rotation rate, with an amplitude proportional to the electric field strength and a phase determined by the direction of the electric field. The frequency response of the differential amplifier was 0.05 Hz to 10 Hz and included the entire range of spin rates expected as the antenna was deployed. The V-Diff signal was sampled 6 times each frame by the encoder. The gain of the differential amplifier could be controlled by command to provide dynamic ranges of +/-0.5 and +/-8.0 volts for the antenna potential difference measurements.           Signals from the electric antenna in the frequency range from 10 kHz to 200 kHz were analyzed by the narrow band step frequency receiver. The primary purpose of this receiver was to provide very good frequency resolution in the neighborhood of the electron plasma frequency and upper hybrid resonance frequency. The step frequency receiver consisted of 8 narrow band filters (+/-5% band-width) which were sequentially switched into a log compressor. The  log compressor provided a 0 to 5 volt analog voltage, SFR, to the spacecraft encoder. The switch (S4) position was controlled by clock lines from the spacecraft encoder and was stepped through 8 frequencies, 13.3, 17.8, 23.7, 31.1, 42.2, 56.2, 100, and 178 kHz, at a rate of four frequencies per telemetry frame (5.76 seconds). The log compressor provided a 0 to 5 volt analog voltage, SFR, to the spacecraft encoder which was proportional to the logarithm of the signal strength over a dynamic range of 100 db.           The 8-channel spectrum analyzer  provided relatively coarse frequency spectrum measurements of both electric and magnetic fields over a broad frequency range of 1.0 Hz to 10.0 kHz. The primary purpose of the 8-channel spectrum analyzer was to provide field strength measurements to complement the high-resolution frequency-time spectra from the wide-band receiver.           Switches S1 and S2 were controlled by clock lines from the spacecraft encoder and commutate the filter outputs to two log compressors which provided field strength measurements SA-1 and SA-2 (0 to 5 volts) to the spacecraft encoder. These outputs were sampled twice per telemetry frame. Switch S3, which was controlled by a clock line, commutates the electric and magnetic field signals to the 8-channel spectrum analyzer.          Approximately every 5 minutes the impedance of the electric antenna was determined at a frequency of 17 Hz by driving a small AC current into the antennas and measuring the resultant voltage on the antennas with the 8-channel spectrum analyzer. The 17 Hz oscillator was gated on for 1 frame out of every 64 frames by a clock line.           Immediately following the impedance measurement the pulser circuit produced a 10 volt pulse with a duration of 20 micro- seconds. This pulse was to stimulate local plasma resonances, such as plasma oscillation, from which the electron density could be determined. A pulse of +10 volts was applied to one antenna element and a -10 volt pulse was applied to the opposite antenna element. The pulser was switched on by command. The pulser was on when the experiment was in VLF45 mode and off when the experiment was in the VLF10 mode. The pulser voltage was coupled to the antenna through a 220 pf capacitor which would have allowed some meaningful data to be obtained from the experiment even if the pulser output were to short to ground. The pulse was applied at the end of the impedance measurement frame.

Hawkeye page maintained by NASA GSFC with science and instrument descriptions, data, software, and publication lists

Information about the ELF/VLF Receivers experiment on the Hawkeye 1 mission.

Electric and Magnetic Field Radio Frequency Spectrum Analyzer Data 

SPDF/CDAWeb. Please also acknowledge the data producer: D. Gurnett at University of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: D. Gurnett at University of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Gurnett at University of Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/hawkeye/vlf/vlf_h0/1974/hk_h0_vlf_19740608_v01.cdf. The most common cadence, 23040 [ms] = PT23.04S, occurred for 97.4779% of the 2203 timesteps. 

Electric and Magnetic Field Radio Frequency Spectrum Analyzer (from all.xml/instrument/description/@short)

Electric Spectral Power Density at 16 Frequencies (2 Hz - 178 kHz)

Hawkeye position in Earth radii, SM magnetic latitude, SM magnetic local time

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/hyakutake_helio1day_position_19950101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 9496 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/hyakutake_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

This ionogram was digitized from the original ISIS 1 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 673). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at https://spdf.gsfc.nasa.gov/isis/isis-status.html

ISIS 1 Data Restoration and Enhancement Project, Radio Science publication

Benson, R.F., D. Bilitza, S.F. Fung, V. Truhlik, and Y. Wang (2018), Enhancing the ISIS-I topside digital ionogram database, Radio Sci., 53, DOI: 10.1029/2018RS006659

Information about the Swept Frequency Sounder, SFS, Experiment on ISIS 1

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_new_i1_cdf/isis1/ott_45n_284e/1969/030/i1_av2_ott_1969030145012_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 88.5457% of the 688 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_new_i1_cdf/isis1/qui_01s_281e/1969/031/i1_av2_qui_1969031042004_v01.cdf. The most common cadence, 34 [ms] = PT0.034S, occurred for 56.8627% of the 377 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_new_i1_cdf/isis1/snt_33s_298e/1969/031/i1_av2_snt_1969031043248_v01.cdf. The most common cadence, 34 [ms] = PT0.034S, occurred for 59.8734% of the 473 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_new_i1_cdf/isis1/ula_65n_212e/1975/004/i1_av2_ula_1975004181550_v01.cdf. The most common cadence, 34 [ms] = PT0.034S, occurred for 68.5289% of the 368 timesteps. 

ISIS-1 Topside sounder ionograms, all stations merged into a single dataset

This ionogram was digitized from the original ISIS 1 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at https://nssdc/space/isis/isis-status.html

ISIS/Alouette page maintained by NASA GSFC with science and instrument descriptions, data access, software, and publication lists

Information about the Sweep Frequency Sounder experiment on ISIS-1.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch2d, @1 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch2d, @1 => Epoch.)

all stations merged (from all.xml/instrument/description/@short)

IONOGRAM: expandable thumbnails of color-coded relative amplitude (0-255) on ionogram time (x) vs. apparent range from satellite down (y) grid

IONOGRAM: continuous-film display of color-coded relative amplitude (0-255) on ionogram time (x) vs. apparent range from satellite down (y) grid

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/all/1969/030/i1_av_all_1969030145012_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 99.4438% of the 894 timesteps. 

-- Sounder frequency in MHz (incl. fixed and swept frequency parts) - ONLY positively identified frequencies are shown

-- Scan line number of start of swept portion (before is fixed portion)

-- Magnetic inclination (Dip angle of magnetic field direction) in degrees

CODES & MODES: Satellite-ID: 1=Alouette-1, 2=Aloutte-2,  3=ISIS-1, 4=ISIS-2

-- Telemetry station ID (nn) (https://nssdc.gsfc.nasa.gov/space/isis/isis-table1-new.html

-- DMODE (transmitter on/off for alternate frame pairs): 0 = off, 1 = on

-- GMODE (transmission of alternate frames of swept and fixed frequency): 0 = off, 1 = on

-- Fixed frequency code: 0=off, 1=0.25, 2=0.48, 3=1.00, 4=1.95, 5=4.00, 6=9.303 MHz

ISIS-1 Topside Sounder Ionograms over Kerguelen Island, France (Lat=-49, Long=70)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/KER_49S_070E/1983/236/i1_av_ker_1983236152121_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 899 timesteps. 

ISIS-1 Topside Sounder Ionogram over Kashima, Japan (lat/lon=36/141)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/KSH_36N_141E/1978/006/i1_av_ksh_1978006045217_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 99.6736% of the 916 timesteps. 

ISIS-1 Topside Sounder Ionogram over Kwajalein, Marshall Is. (lat/lon=9/168)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/KWA_09N_168E/1978/003/i1_av_kwa_1978003041325_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 909 timesteps. 

ISIS-1 Topside Sounder Ionogram over Ouagadougou, Burkina Faso (lat/lon=14/359)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/ODG_14N_359E/1969/034/i1_av_odg_1969034132725_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 847 timesteps. 

ISIS-1 Topside Sounder Ionogram over Orroral, Australia (lat/lon=-36/149)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/ORR_36S_149E/1970/028/i1_av_orr_1970028094709_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 99.5647% of the 915 timesteps. 

ISIS-1 Topside Sounder Ionogram over Ottawa, Canada (lat/lon=45/284)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/OTT_45N_284E/1969/030/i1_av_ott_1969030145012_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 99.4438% of the 894 timesteps. 

ISIS-1 Topside Sounder Ionogram over Quito, Equador (lat/lon=-1/281)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/QUI_01S_281E/1969/031/i1_av_qui_1969031042004_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 99.7778% of the 898 timesteps. 

ISIS-1 Topside Sounder Ionogram over Resolute Bay, Canada (lat/lon=75/265)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/RES_75N_265E/1969/030/i1_av_res_1969030211814_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 99.3333% of the 447 timesteps. 

ISIS-1 Topside Sounder Ionogram over Santiago, Chile (lat/lon=-33/298)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/SNT_33S_298E/1969/031/i1_av_snt_1969031012939_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 876 timesteps. 

ISIS-1 Topside Sounder Ionogram over Sodankyla, Finland (lat/lon=67/27)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/SOD_67N_027E/1977/348/i1_av_sod_1977348223046_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for 98.2143% of the 495 timesteps. 

ISIS-1 Topside Sounder Ionogram over Tromso, Norway (lat/lon=70/19)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/TRO_70N_019E/1969/036/i1_av_tro_1969036181549_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 919 timesteps. 

ISIS-1 Topside Sounder Ionogram over Fairbanks, Alaska (lat/lon=65/212)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/ULA_65N_212E/1975/004/i1_av_ula_1975004181516_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 899 timesteps. 

ISIS-1 Topside Sounder Ionogram over Winkfield, U.K. (lat/lon=51/359)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis1/WNK_51N_359E/1969/034/i1_av_wnk_1969034010210_v01.cdf. The most common cadence, 33 [ms] = PT0.033S, occurred for all 869 timesteps. 

ISIS-1 Topside Electron Density Profiles, manually scaled at CRC

This data set, provided by the Communications Research Centre (CRC) in Ottawa, Canada, consists of electron density profiles for the ionosphere above the F2 maximum (topside ionosphere). The data were computed from the orginal ionograms using Jackson's method (Jackson, Proceedings of the IEEE., p. 960, June 1969).ISIS-1 was launched on 1969-01-30 into an elliptical orbit (500-3500km) with an inclination of 88.4 degrees and ISIS-2 was launched on 1971-04-01 into an circular orbit at 1400 km with an inclination of 88.1 degrees.Both satellites were fully instrumented ionospheric observatories including sweep- and fixed-frequequency ionosondes, a VLF receiver, energetic and soft particle detectors, an ion mass spectrometer, an electrostatic analyzer, an Langmuir probe, a beacon transmitter, a cosmic noise experiment and ISIS 2 also carried two photometers. A tape recorder with 1-h capacity was included on both satellites. Data were also collected during overflights of several telemetry stations. The telemetry stations were in areas that provided primary data coverage near the 80-deg-W meridian and in areas near Hawaii, Singapore, Australia, the UK, Norway, India, Japan, Antarctica, New Zealand, and Central Africa.

 J. E. Jackson, "The reduction of topside ionograms to electron-density profiles", Proceedings of the IEEE., p. 960, June 1969

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/crc_ne_profile_cdf/isis1/1969/i1_neprof_tops_19690201_v01.cdf. The most common cadence, 29000 [ms] = PT29S, occurred for 36.2047% of the 1946 timesteps. 

ISIS-2 Topside Sounder Ionogram over Ascension Is., U.K. (lat/lon= -8/346)

This ionogram was digitized from the original ISIS 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at https://nssdc/space/isis/isis-status.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/ACN_08S_346E/1975/009/i2_av_acn_1975009012259_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 89.2920% of the 1009 timesteps. 

Sounder amplitude at 223 virtual heights for fixed & swept frequency

ISIS-2 Topside Sounder Ionogram over Terre Adelie, Antarctica (lat/lon=-67/140)

A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been digitized using the GSFC facilities of the Data Evaluation Laboratory (DEL) within the Mission Operations and Data Systems Directorate (Code 500) at Goddard.  The digitization was performed using an A/D converter board and software device driver compatible with the OS/2 operating system used by the 486-based Programmable Telemetry Processor (PTP) associated software has been installed on their PTP and de-bugged so that we now have a working system for making digital ISIS ionograms directly from the telemetry tapes.  Earlier, we successfully digitized the PCM and NASA 36 bit time-code data from this same tape. The ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz appropriate for the post-detection ISIS 2 sounder-receiver video output which extends from DC to 15 kHz (see p. 50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples between each of the approximately 1015 sounder pulses per ionogram (including the fixed-frequency portion) or nearly 10**6 16-bit samples/ionogram (approximately 1.8 MBytes) for just the sounder-receiver video data. Adding header information, and the pcm data containing data from the other instruments, yields about 2 MBytes of data for the 22.5 s period corresponding to one ionogram. Two steps were taken in order to reduce this large volume of nearly 2 MBytes/ionogram.  First, every four 25 microsecond samples following the sounder pulse were averaged.  Second, the 16 bit samples were reduced to 8 bit samples.  The first step decreased the apparent-range resolution to 15 km, but yielded high-quality ionograms because of the improved S/N due to the averaging. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/ADL_67S_140E/1973/012/i2_av_adl_1973012101821_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 50.1494% of the 1007 timesteps. 

ISIS-2 Topside Sounder Ionogram over Ahmedabad, India (lat/lon=23/73)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/AME_23N_073E/1973/034/i2_av_ame_1973034040026_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 50.4587% of the 55 timesteps. 

ISIS-2 Topside Sounder Ionogram over Brazzavillle, Congo (lat/lon=-4/15)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/BRZ_04S_015E/1972/218/i2_av_brz_1972218161740_v01.cdf. The most common cadence, 17 [ms] = PT0.017S, occurred for 24.3478% of the 28 timesteps. 

ISIS-2 Topside Sounder Ionogram over Johannesburg, South Africa (lat/lon=-26/28)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/BUR_26S_028E/1972/220/i2_av_bur_1972220152603_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 99.1211% of the 1015 timesteps. 

ISIS-2 Topside Sounder Ionogram over Las Palmas,  Canary Is., Spain (lat/lon=28/345)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/CNA_28N_345E/1974/016/i2_av_cna_1974016174239_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 1009 timesteps. 

ISIS-2 Topside Sounder Ionogram over Kerguelen Is., France (lat/lon=-49/70)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/KER_49S_070E/1977/001/i2_av_ker_1977001000137_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 82.6970% of the 1018 timesteps. 

ISIS-2 Topside Sounder Ionogram over Kourou, French Guyana (lat/lon=5/307)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/KRU_05N_307E/1973/037/i2_av_kru_1973037011608_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 99.8024% of the 1010 timesteps. 

ISIS-2 Topside Sounder Ionogram over Kashima, Japan (lat/lon=36/141)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/KSH_36N_141E/1972/001/i2_av_ksh_1972001000110_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 1011 timesteps. 

ISIS-2 Topside Sounder Ionogram over Kwajalein, Marshall Is. (lat/lon=9/168)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/KWA_09N_168E/1978/010/i2_av_kwa_1978010084653_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 636 timesteps. 

ISIS-2 Topside Sounder Ionogram over Lauder, New Zealand (lat/lon=-45/170)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/LAU_45S_170E/1973/001/i2_av_lau_1973001041429_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 1009 timesteps. 

ISIS-2 Topside Sounder Ionogram over Ouagadougou, Burkina Faso (lat/lon=14/359)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/ODG_14N_359E/1972/219/i2_av_odg_1972219053637_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 99.3769% of the 638 timesteps. 

ISIS-2 Topside Sounder Ionogram over Orroral Australia (lat/lon=-36/149)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/ORR_36S_149E/1973/074/i2_av_orr_1973074033311_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 95.6656% of the 927 timesteps. 

ISIS-2 Topside Sounder Ionogram over Ottawa, Canada (lat/lon=45/284)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/OTT_45N_284E/1971/315/i2_av_ott_1971315181816_v02.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 82.9175% of the 864 timesteps. 

ISIS-2 Topside Sounder Ionogram over Quito, Equador (lat/lon=-1/281)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/QUI_01S_281E/1973/003/i2_av_qui_1973003022210_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 80.0182% of the 881 timesteps. 

ISIS-2 Topside Sounder Ionogram over Resolute Bay, Canada (lat/lon=75/265)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/RES_75N_265E/1971/091/i2_av_res_1971091092252_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 176 timesteps. 

ISIS-2 Topside Sounder Ionogram over Santiago, Chile (lat/lon=-33/298) 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/SNT_33S_298E/1973/166/i2_av_snt_1973166094817_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 636 timesteps. 

ISIS-2 Topside Sounder Ionogram over Sodankyla, Finland (lat/lon=67/27)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/SOD_67N_027E/1977/345/i2_av_sod_1977345214750_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 92.3077% of the 48 timesteps. 

ISIS-2 Topside Sounder Ionogram over Falkland Is., U.K. (lat/lon=-52/302)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/SOL_52S_302E/1972/012/i2_av_sol_1972012163105_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 1013 timesteps. 

ISIS-2 Topside Sounder Ionogram over Syowa Base, Antartica (lat/lon=-69/40)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/SYO_69S_040E/1973/034/i2_av_syo_1973034054937_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 50.9137% of the 1003 timesteps. 

ISIS-2 Topside Sounder Ionogram over Tromso, Norway (lat/lon=70/19)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/TRO_70N_019E/1973/019/i2_av_tro_1973019103836_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for all 640 timesteps. 

ISIS-2 Topside Sounder Ionogram over Fairbanks, Alaska (lat/lon=65/212)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/ULA_65N_212E/1972/366/i2_av_ula_1972366000000_v01.cdf. The most common cadence, 21 [ms] = PT0.021S, occurred for 55.0725% of the 76 timesteps. 

ISIS-2 Topside Sounder Ionogram over Winkfield, U.K. (lat/lon=51/359)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/ionogram_cdf/isis2/WNK_51N_359E/1973/073/i2_av_wnk_1973073115535_v01.cdf. The most common cadence, 22 [ms] = PT0.022S, occurred for 96.8992% of the 125 timesteps. 

ISIS-2 TOPIST produced electron density profiles, of highest quality (quality flag = 2 and 3

ISIS 2 was an ionospheric observatory instrumented with a sweep- and a fixed-frequency ionosonde, a VLF receiver, energetic and soft particle detectors, an ion mass spectrometer, an electrostatic probe, a retarding potential analyzer, a beacon transmitter, a cosmic noise experiment, and two photometers. Two long crossed-dipole antennas (73 and 18.7 m) were used for the sounding, VLF, and cosmic noise experiments.The spacecraft was spin-stabilized to about 2 rpm after antenna deployment. There were two basic orientation modes for the spacecraft, cartwheel and orbit-aligned. The spacecraft operated approximately the same length of time in each mode, remaining in one mode typically 3 to 5 months. The cartwheel mode with the axis perpendicular to the orbit plane was made available to provide ram and wake data for some experiments for each spin period, rather than for each orbit period. Attitude and spin information was obtained from a three-axis magnetometer and a sun sensor. Control of attitude and spin was possible by means of magnetic torquing.The experiment package also included a programmable tape recorder with a one hour capacity. For non-recorded observations, data from satellite and subsatellite regions were telemetered when the spacecraft was in the line of sight of a telemetry station. Telemetry stations were located so that primary data coverage was near the 80-deg-W meridian and near Hawaii, Singapore, Australia, England, France, Norway, India, Japan, Antarctica, New Zealand, and Central Africa. NASA support of the ISIS project was terminated on October 1, 1979.  A significant amount of experimental data, however, was acquired after this date by the Canadian project team. ISIS 2 operations were terminated in Canada on March 9, 1984. The Radio Research Laboratories (Tokyo, Japan) then requested and received permission to reactivate ISIS 2. Regular ISIS 2 operations were started from Kashima, Japan, in early August 1984. ISIS 2 was deactivated effective 24, 1990. A data restoration effort began in the late 1990s and successfully saved a considerable portion of the high-resolution data before the telemetry tapes were discarted.The data set was generated from the averaged ionogram binary data (SPIO-00318) recorded by the Topside Sounder. The data are obtained with the TOPIST program, which analyzes the data, automatically scales the ionogram traces and resonances, and inverts the traces into an electron density profile. The same program is available for use to hand-scale the data if desired. Output data items include spacecraft position, electron density profile, assessment of quality, resonance and cut-off frequencies, and both the O-trace and X-trace.

SPDF/CDAWeb. Please also acknowledge the data producer: X. Huang and B. Reinisch at University of MassachusettsLowell

SPDF/SSCWeb. Please also acknowledge the data producer: X. Huang and B. Reinisch at University of MassachusettsLowell

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: X. Huang and B. Reinisch at University of MassachusettsLowell

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/topist_ne_profile_cdf/isis2/1971/i2_neprof_topist_19711111_v01.cdf. The most common cadence, 67000 [ms] = PT1M7S, occurred for 25.0000% of the 3 timesteps. 

Generated by TOPIST program, quality flags 2 and 3 (from all.xml/instrument/description/@short)

Invdip - A new coordinate that combines Invariant Latitude and Dip Latitude

ISIS-2 Topside Electron Density Profiles, manually scaled at CRC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isis/crc_ne_profile_cdf/isis2/1971/i2_neprof_tops_19710408_v01.cdf. The most common cadence, 23000 [ms] = PT23S, occurred for 26.5170% of the 1276 timesteps. 

This 15.36s data set was created in 2008-9 at GSFC/SPDF from a newly created 320ms data set, with some gaps filled with data from the prior 15.36s data set. Full documentation may be found at https://spdf.gsfc.nasa.gov/pub/data/imp/imp8/mag/15s_ascii_v3/00_IMP8_15s_data_docum.txt Creation of the new 320ms and 15.36s data sets was done by N. Papitashvili and J. King, with guidance from Adam Szabo. 

A web site hosting instrument information and providing access to the data

SPDF/CDAWeb. Please also acknowledge the data producer: A. Szabo / R.P. Lepping at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: A. Szabo / R.P. Lepping at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Szabo / R.P. Lepping at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/imp/imp8/mag/mag_15sec_cdaweb/1973/i8_15sec_mag_19731030_v03.cdf. The most common cadence, 15360 [ms] = PT15.36S, occurred for 99.2532% of the 5582 timesteps. 

Interplanetary Monitoring Platform 8 (from all.xml/observatory/description/@short)

Interplanetary Monitoring Platform 8 (from Master/CDFglobalAttributes/Source_name)

15.36 sec Resolution (from Master/CDFglobalAttributes/Data_type)

CDF time standard. Time of last data sequence in the 15.36-second average.

Data source flag =1 if based on 320ms data, = 2 if based  on old V2 15.36s data

Number of points in 15.36 second average. Max. number is 48(12) for data source flag equal 1(2)

Variances; off-diagonal elements Byx, Bzx, Bzy; GSE coordinates 

Difference between record time tag and start of average,Relevant to data source flag = 2 records only.

For detailed documentation on the creation of this data set see https://spdf.gsfc.nasa.gov/pub/data/imp/imp8/mag/320ms_ascii/doc/imp8_mag_320ms_proc.txt

SPDF/CDAWeb. Please also acknowledge the data producer: Adam Szabo, Joe King and Natalia Papitashvili at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Adam Szabo, Joe King and Natalia Papitashvili at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Adam Szabo, Joe King and Natalia Papitashvili at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/imp/imp8/mag/mag_320msec_cdaweb/1973/i8_320msec_mag_19731030_v01.cdf. The most common cadence, 319 [ms] = PT0.319S, occurred for 32.4821% of the 30807 timesteps. 

320msec Time Resolution (from Master/CDFglobalAttributes/Data_type)

SPDF/CDAWeb. Please also acknowledge the data producer: R.E. McGuire at SPDF/Code 612.4, NASA's GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: R.E. McGuire at SPDF/Code 612.4, NASA's GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R.E. McGuire at SPDF/Code 612.4, NASA's GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/imp/imp8/particles_gme/data/flux/gme_h0/1973/i8_h0_gme_19731101_v01.cdf. The most common cadence, 1800000 [ms] = PT30M, occurred for all 2927 timesteps. 

Goddard Medium Energy Investigation (from all.xml/instrument/description/@short)

(Spectrogram-Full List) Proton Diff Intens (no bckgrd subtract), 30 energies 0.5-500 MeV, spin-avg

(Individual time-series) Uncertainty, Proton Differential  Intensity

(Spectrogram-Full List) Alpha Diff Intens (no bckgrd subtract), 21 energies 1-80 MeV/nuc, spin-avg

(Individual time-series) Uncertainty, Alpha Differential Intensity

IMP-8 MIT Plasma Investigation, High Resolution Definitive Data  

SPDF/CDAWeb. Please also acknowledge the data producer: A. Lazarus at MIT

SPDF/SSCWeb. Please also acknowledge the data producer: A. Lazarus at MIT

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Lazarus at MIT

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/imp/imp8/plasma_mit/mitplasma_h0/1973/i8_h0_mitplasma_19731031_v01.cdf. The most common cadence, 28000 [ms] = PT28S, occurred for 13.8889% of the 5 timesteps. 

MIT Plasma Investigation (from all.xml/instrument/description/@short)

Region flag (1=Solar Wind, 2= Solar Wind or Magnetosheath, 3= Not Solar Wind)

Operating mode flag [1:Non-tracking (NTMS), 2:Tracking (TMS), 3:Acquisition (AQM)]

(Fits-based, no region selected) Proton most-probable thermal speed 

--> (Fits-based, solar wind only) Proton most-probable thermal speed

--> (Moments-based, no region selected) Proton most-probable thermal speed

--> (Moments-based, solar wind only) Proton most-probable thermal speed

(Fits-based, no region selected) Proton East/West flow angle (aberration corrected)

--> (Fits-based, solar wind only) Proton East/West flow angle (aberration corrected)

--> (Moments-based, no region selected) Proton East/West flow angle (no aberration correction)

--> (Moments-based, solar wind only) Proton East/West flow angle (no aberration correction)

(Fits-based, no region selected) Proton flow elevation angle (from currents above noise threshold)

--> (Fits-based, solar wind only) Proton flow elevation angle (from currents above noise threshold)

--> (Moments-based, no region selected) Proton flow elevation angle (all currents)

--> (Moments-based, solar wind only) Proton flow elevation angle (all currents)

 IMP-8 orbital position (multiple coordinate systems, from April 2003 updated I8 orbit model)

Generated by SSCWeb from Heather Franz's "Second Experimental Ephemeris" as approved by IMP-8 PIs 

SPDF/CDAWeb. Please also acknowledge the data producer:  SSC at SPDF/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer:  SSC at SPDF/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer:  SSC at SPDF/GSFC

SPDF/SSCWeb and the HAPI project. Please also acknowledge the data producer:  SSC at SPDF/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/imp/imp8/orbit/or_ssc/i8_or_ssc_19731030_v01.cdf. The most common cadence, 720000 [ms] = PT12M, occurred for all 7559 timesteps. 

Satellite Situation Center (from all.xml/instrument/description/@short)

Orbit (I8 updated 4/03) (from Master/CDFglobalAttributes/Data_type)

Interball Auroral Probemeasurements of spectra and anisotropy of electrons SKA-3, Key Parameters

Measurements of spectra and anisotropy of electrons witin energy ranges 20-40 keV from two time-of-flight detectors EM-1-1 and EM-1-2. The field of view of these detectors are directed oppositely and perpendicular to the satellite  rotation axis. Data description:  http://www.iki.rssi.ru/inte rball.html 

Interball Auroral Probe SKA3, electron number flux, E=20-40 keV 

SPDF/CDAWeb. Please also acknowledge the data producer: Yu. Galperin, R. Kovrazhkin,  A. Kuzmin,  F. Shuiskaya at IKI RAN, Russia

SPDF/SSCWeb. Please also acknowledge the data producer: Yu. Galperin, R. Kovrazhkin,  A. Kuzmin,  F. Shuiskaya at IKI RAN, Russia

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Yu. Galperin, R. Kovrazhkin,  A. Kuzmin,  F. Shuiskaya at IKI RAN, Russia

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/aurora/enf/1996/ia_k0_enf_19960920_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 90.2439% of the 37 timesteps. 

Interball Auroral Probe (from all.xml/observatory/description/@short)

SKA3 electron number flux (from all.xml/instrument/description/@short)

Interball Auroral Probe (from Master/CDFglobalAttributes/Source_name)

SPDF/CDAWeb. Please also acknowledge the data producer: DOK-2: K.Kudela at DOK-2: Institute of experimental physics Slovak Acad. Sci., Kosize, Slovakia

SPDF/SSCWeb. Please also acknowledge the data producer: DOK-2: K.Kudela at DOK-2: Institute of experimental physics Slovak Acad. Sci., Kosize, Slovakia

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: DOK-2: K.Kudela at DOK-2: Institute of experimental physics Slovak Acad. Sci., Kosize, Slovakia

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/aurora/epi/1996/ia_k0_epi_19960903_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 99.4764% of the 380 timesteps. 

Auroral Probe Energetic Particle Instrument (from all.xml/instrument/description/@short)

Interball Auroral Probe Ion Composition Experiment PROMICS, Key Parameters

Count rate of H+, O+ ions in 2 min, three directions, (1-30 keV) Status flag shows instrument mode.Data description:  http://www.iki.rssi.ru/interball.html

SPDF/CDAWeb. Please also acknowledge the data producer: I.Sandahl at IRF, Kiruna, Sweden

SPDF/SSCWeb. Please also acknowledge the data producer: I.Sandahl at IRF, Kiruna, Sweden

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: I.Sandahl at IRF, Kiruna, Sweden

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/aurora/icd/1996/ia_k0_icd_19960918_v01.cdf. The most common cadence, 140000 [ms] = PT2M20S, occurred for all 1 timesteps. 

Auroral Probe Ion Composition Data (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: V.Petrov at IMAP:IZMIRAN,Troitsk,  Russia.

SPDF/SSCWeb. Please also acknowledge the data producer: V.Petrov at IMAP:IZMIRAN,Troitsk,  Russia.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V.Petrov at IMAP:IZMIRAN,Troitsk,  Russia.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/aurora/mfi/1996/ia_k0_mfi_19960901_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for all 57 timesteps. 

Interball  auroralprobe (from all.xml/observatory/description/@short)

Magnetic Field Data (from all.xml/instrument/description/@short)

Interball  auroralprobe (from Master/CDFglobalAttributes/Source_name)

SPDF/CDAWeb. Please also acknowledge the data producer: V.Prokhorenko at Space Research Inst., Russian Acad. Sci., Moscow, Russia.

SPDF/SSCWeb. Please also acknowledge the data producer: V.Prokhorenko at Space Research Inst., Russian Acad. Sci., Moscow, Russia.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V.Prokhorenko at Space Research Inst., Russian Acad. Sci., Moscow, Russia.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/aurora/orbit/1996/ia_or_def_19960919_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 1007 timesteps. 

IBEX-Hi Release 2; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 17 releases of IBEX-HI and/or IBEX-LO data covering 2009-2020. 2: This data set is from the Release 2 (6 months-cadence) IBEX-Hi map data for the year 2009 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 2 map numbers (1-2) with mission year 1Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/20098: This particular data set, denoted in the original ascii files as mapN for N=1-2, which indicates a map number, includes pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence. 

Please acknowledge the IBEX Mission Principal Investigator, Dr. David J McComas of Princeton University. 

IBEX Data Release 2, IBEX-Hi six-month maps in ascii list and image formats

The IBEX data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. David J. McComas at Princeton University

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. David J. McComas at Princeton University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. David J. McComas at Princeton University

Interstellar Boundary Explorer (from all.xml/observatory/description/@short)

Energetic Neutral Atom (from all.xml/instrument/description/@short)

Interstellar Boundary Explorer (from Master/CDFglobalAttributes/Source_name)

CDF epoch time for the start of the  six-month measurement period

Sequential number 1 - 6 for six-month maps from IBEX Data Release 4

IBEX-Hi Release 2; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 17 releases of IBEX-HI and/or IBEX-LO data covering 2009-2020. 2: This data set is from the Release 2 (6 months-cadence) IBEX-Hi map data for the year 2009 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 2 map numbers (1-2) with mission year 1Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/20098: This particular data set, denoted in the original ascii files as mapN for N=1-2, which indicates a map number, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

IBEX-Hi Release 4; Compton-Getting, no Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of antiram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_yearN_cg for N  1 - 3, includes pixel map data from antiram direction (antiram-directional), CG, no SP, 1 year cadence. 

The IBEX Release 4 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

CDF epoch time for the start of the  one-year measurement period

Sequential starting number 1 - 22 for six-month map from IBEX Data Release 16

IBEX-Hi Release 4; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (6 months-cadence) IBEX-Hi map data for the years 2009-2012 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_mapX for N=1-6, in which N indicates a map number, includes pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence. 

IBEX-Hi Release 4; Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of ram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_yearN_cg  for N = 1 - 3, includes pixel map data from ram direction (ram-directional), CG, no SP, 1 year cadence. 

IBEX-Hi Release 4; Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of antiram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_yearN_cg for N = 1 - 3, includes pixel map data from antiram direction (antiram-directional), CG, SP, 1 year cadence. 

IBEX-Hi Release 4; Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (6 months-cadence) IBEX-Hi map data for the years 2009-2012 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_mapN for N = 1 - 6, in which N indicates a map number, includes pixel map data from all directions (omnidirectional), CG, SP, 6 month cadence. 

IBEX-Hi Release 4; Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of ram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_yearN_cg for N = 1 - 3, includes pixel map data from ram direction (ram-directional), CG, SP, 1 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4, 7.5 day-cadence IBEX-Hi data for the  years 2009-2012 in the form of Survival Probabilities tables. Each data directory related to survival probability has information about a different aspect of the transport through the heliosphere: a) deflection - angular deflection experienced between the termination shock and the observer. b) eloss - energy loss (or gain) between the termination shock and the observer. c) survpro - survival probability that an ENA passing through the termination shock will make it to 1AU. 3. For this release, the survival probabilities are only applied to the IBEX-HI data stream. Note that the energy loss is negligible, and the deflection angles in the inertial system are always smaller than 0.6 degrees or so. 4. Each directory has contains correction factors for data in the spacecraft frame (scf) and the inertial frame (1AU). The inertial frame (1AU) survival probabilities are used for the CG corrected data. The spacecraft frame factors are used for uncorrected data. The spacecraft frame files have the energy/direction shifts caused by the Earth/Spacecraft motion. This has a small effect on the survival probabilities (simply due to the energy shifts), but the deflection angles and energy shifts caused by this motion can be significant. 5. The deflection and energy shift files are not applied by the IBEX pipeline software. In theory, these could be applied to the CG corrected data after the fact. However, it is important to note that the spacecraft frame correction factors for energy and angle contain elements of the CG correction and 6. can yield confusing results when applied to the pipeline results. The data layout per frame consists of the following. For the spacecraft frame, there is a column for each ESA step, and a row for each angle bin (1 degree bins). Each number gives the probability at that angle and ESA for survival. The probability per angle is interpolated to the center of any particular angular bin being evaluated. In the inertial frame, the columns are the energies rather than ESA steps. 7. These are applied to the IBEX images that are given on the variable energy grid. For each image pixel, we take the energy and angle and use a 2D interpolation to get the survival probability.8. The data consist of Survival Probabilities tables. Details of the data and enabled science from Release 10 are given in the following journal publication:9: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 10: http://doi.org/10.3847/1538-4365/aa66d8 8: This particular data set, denoted in the original ascii files as Data_Release_4\hs_transport\surv\o0NNNx.defl1au , where NNN=006-150 is an orbit number, and x = a or b for the orbit 130 or higher, indicates the first or the second half of the orbit, Survival Probabilities tables

IBEX Data Release 4, IBEX-Hi 7.5 days survival probabilities plots in ascii list and image formats

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4, 7.5 day-cadence IBEX-Hi data for the  years 2009-2012 in the form of Survival Probabilities tables. Each data directory related to survival probability has information about a different aspect of the transport through the heliosphere: a) deflection - angular deflection experienced between the termination shock and the observer. b) eloss - energy loss (or gain) between the termination shock and the observer. c) survpro - survival probability that an ENA passing through the termination shock will make it to 1AU. 3. For this release, the survival probabilities are only applied to the IBEX-HI data stream. Note that the energy loss is negligible, and the deflection angles in the inertial system are always smaller than 0.6 degrees or so. 4. Each directory has contains correction factors for data in the spacecraft frame (scf) and the inertial frame (1AU). The inertial frame (1AU) survival probabilities are used for the CG corrected data. The spacecraft frame factors are used for uncorrected data. The spacecraft frame files have the energy/direction shifts caused by the Earth/Spacecraft motion. This has a small effect on the survival probabilities (simply due to the energy shifts), but the deflection angles and energy shifts caused by this motion can be significant. 5. The deflection and energy shift files are not applied by the IBEX pipeline software. In theory, these could be applied to the CG corrected data after the fact. However, it is important to note that the spacecraft frame correction factors for energy and angle contain elements of the CG correction and 6. can yield confusing results when applied to the pipeline results. The data layout per frame consists of the following. For the spacecraft frame, there is a column for each ESA step, and a row for each angle bin (1 degree bins). Each number gives the probability at that angle and ESA for survival. The probability per angle is interpolated to the center of any particular angular bin being evaluated. In the inertial frame, the columns are the energies rather than ESA steps. 7. These are applied to the IBEX images that are given on the variable energy grid. For each image pixel, we take the energy and angle and use a 2D interpolation to get the survival probability.8. The data consist of Survival Probabilities tables. Details of the data and enabled science from Release 10 are given in the following journal publication:9: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 10: http://doi.org/10.3847/1538-4365/aa66d8 8: This particular data set, denoted in the original ascii files as Data_Release_4\hs_transport\surv\o0NNNx.deflscf , where NNN=006-150 is an orbit number, and x = a or b for the orbit 130 or higher, indicates the first or the second half of the orbit, Survival Probabilities tables

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4, 7.5 day-cadence IBEX-Hi data for the  years 2009-2012 in the form of Survival Probabilities tables. Each data directory related to survival probability has information about a different aspect of the transport through the heliosphere: a) deflection - angular deflection experienced between the termination shock and the observer. b) eloss - energy loss (or gain) between the termination shock and the observer. c) survpro - survival probability that an ENA passing through the termination shock will make it to 1AU. 3. For this release, the survival probabilities are only applied to the IBEX-HI data stream. Note that the energy loss is negligible, and the deflection angles in the inertial system are always smaller than 0.6 degrees or so. 4. Each directory has contains correction factors for data in the spacecraft frame (scf) and the inertial frame (1AU). The inertial frame (1AU) survival probabilities are used for the CG corrected data. The spacecraft frame factors are used for uncorrected data. The spacecraft frame files have the energy/direction shifts caused by the Earth/Spacecraft motion. This has a small effect on the survival probabilities (simply due to the energy shifts), but the deflection angles and energy shifts caused by this motion can be significant. 5. The deflection and energy shift files are not applied by the IBEX pipeline software. In theory, these could be applied to the CG corrected data after the fact. However, it is important to note that the spacecraft frame correction factors for energy and angle contain elements of the CG correction and 6. can yield confusing results when applied to the pipeline results. The data layout per frame consists of the following. For the spacecraft frame, there is a column for each ESA step, and a row for each angle bin (1 degree bins). Each number gives the probability at that angle and ESA for survival. The probability per angle is interpolated to the center of any particular angular bin being evaluated. In the inertial frame, the columns are the energies rather than ESA steps. 7. These are applied to the IBEX images that are given on the variable energy grid. For each image pixel, we take the energy and angle and use a 2D interpolation to get the survival probability.8. The data consist of Survival Probabilities tables. Details of the data and enabled science from Release 10 are given in the following journal publication:9: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 10: http://doi.org/10.3847/1538-4365/aa66d8 8: This particular data set, denoted in the original ascii files as Data_Release_4\hs_transport\surv\o0NNNx.loss1au , where NNN=006-150 is an orbit number, and x = a or b for the orbit 130 or higher, indicates the first or the second half of the orbit, Survival Probabilities tables

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4, 7.5 day-cadence IBEX-Hi data for the  years 2009-2012 in the form of Survival Probabilities tables. Each data directory related to survival probability has information about a different aspect of the transport through the heliosphere: a) deflection - angular deflection experienced between the termination shock and the observer. b) eloss - energy loss (or gain) between the termination shock and the observer. c) survpro - survival probability that an ENA passing through the termination shock will make it to 1AU. 3. For this release, the survival probabilities are only applied to the IBEX-HI data stream. Note that the energy loss is negligible, and the deflection angles in the inertial system are always smaller than 0.6 degrees or so. 4. Each directory has contains correction factors for data in the spacecraft frame (scf) and the inertial frame (1AU). The inertial frame (1AU) survival probabilities are used for the CG corrected data. The spacecraft frame factors are used for uncorrected data. The spacecraft frame files have the energy/direction shifts caused by the Earth/Spacecraft motion. This has a small effect on the survival probabilities (simply due to the energy shifts), but the deflection angles and energy shifts caused by this motion can be significant. 5. The deflection and energy shift files are not applied by the IBEX pipeline software. In theory, these could be applied to the CG corrected data after the fact. However, it is important to note that the spacecraft frame correction factors for energy and angle contain elements of the CG correction and 6. can yield confusing results when applied to the pipeline results. The data layout per frame consists of the following. For the spacecraft frame, there is a column for each ESA step, and a row for each angle bin (1 degree bins). Each number gives the probability at that angle and ESA for survival. The probability per angle is interpolated to the center of any particular angular bin being evaluated. In the inertial frame, the columns are the energies rather than ESA steps. 7. These are applied to the IBEX images that are given on the variable energy grid. For each image pixel, we take the energy and angle and use a 2D interpolation to get the survival probability.8. The data consist of Survival Probabilities tables. Details of the data and enabled science from Release 10 are given in the following journal publication:9: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 10: http://doi.org/10.3847/1538-4365/aa66d8 8: This particular data set, denoted in the original ascii files as Data_Release_4\hs_transport\surv\o0NNNx.lossscf , where NNN=006-150 is an orbit number, and x = a or b for the orbit 130 or higher, indicates the first or the second half of the orbit, Survival Probabilities tables

IBEX-Hi Release 4; no Compton-Getting, no Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_yearN for N = 1 - 3, includes pixel map data from antiram direction (antiram-directional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 4; no Compton-Getting, no Survival-Probability, omni-direction 3-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2011. 2: This data set is from the Release 4 three-year IBEX-Hi map data for 2009-2011, in the form of omni-direction fluxes with no corrections for spacecraft motion (nocg: Compton-Getting) and with no corrections (nosp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 4 map numbers (1-6) with mission year (1-3) each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20118: This particular data set, denoted in the original ascii files as comb-year123, includes pixel map data from omni direction, noCG, noSP, 3 year cadence. 

Sequential number 1 - 14 for six-month maps from IBEX Data Release 10

IBEX-Hi Release 4; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (6 months-cadence) IBEX-Hi map data for the  years 2009-2012 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_mapN for N=1-6, which indicates a map number, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

The IBEX Release 16 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2011. 2: This data set is from the Release 4 three-year IBEX-Hi map data for 2009-2011, in the form of omni-direction fluxes with no corrections for spacecraft motion (nocg: Compton-Getting) and with no corrections (nosp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.)5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 4 map numbers (1-6) with mission year (1-3) each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20118: This particular data set, denoted in the original ascii files as comb-map1to6, includes pixel map data from omni direction, noCG, noSP, 6 maps or 3 year cadence. 

IBEX Data Release 4, IBEX-Hi six-month maps in ascii list and image formats

IBEX-Hi Release 4; no Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of ram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_N for N = 1 - 3, includes pixel map data from ram direction (ram-directional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 4; no Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2012 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and withcorrection for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_yearN for N = 1 - 3, includes pixel map data from antiram direction (antiram-directional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 4; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 6 (6 months-cadence) IBEX-Hi map data for the years 2009-2012 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_mapN for N=1 - 6, which indicates a map number, includes pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Hi Release 4; no Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and withcorrection for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_yearN for N = 1 - 3, includes pixel map data from ram direction (ram-directional), no CG, SP, 1 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4, 7.5 day-cadence IBEX-Hi data for the  years 2009-2012 in the form of Survival Probabilities tables. Each data directory related to survival probability has information about a different aspect of the transport through the heliosphere: a) deflection - angular deflection experienced between the termination shock and the observer. b) eloss - energy loss (or gain) between the termination shock and the observer. c) survpro - survival probability that an ENA passing through the termination shock will make it to 1AU. 3. For this release, the survival probabilities are only applied to the IBEX-HI data stream. Note that the energy loss is negligible, and the deflection angles in the inertial system are always smaller than 0.6 degrees or so. 4. Each directory has contains correction factors for data in the spacecraft frame (scf) and the inertial frame (1AU). The inertial frame (1AU) survival probabilities are used for the CG corrected data. The spacecraft frame factors are used for uncorrected data. The spacecraft frame files have the energy/direction shifts caused by the Earth/Spacecraft motion. This has a small effect on the survival probabilities (simply due to the energy shifts), but the deflection angles and energy shifts caused by this motion can be significant. 5. The deflection and energy shift files are not applied by the IBEX pipeline software. In theory, these could be applied to the CG corrected data after the fact. However, it is important to note that the spacecraft frame correction factors for energy and angle contain elements of the CG correction and 6. can yield confusing results when applied to the pipeline results. The data layout per frame consists of the following. For the spacecraft frame, there is a column for each ESA step, and a row for each angle bin (1 degree bins). Each number gives the probability at that angle and ESA for survival. The probability per angle is interpolated to the center of any particular angular bin being evaluated. In the inertial frame, the columns are the energies rather than ESA steps. 7. These are applied to the IBEX images that are given on the variable energy grid. For each image pixel, we take the energy and angle and use a 2D interpolation to get the survival probability.8. The data consist of Survival Probabilities tables. Details of the data and enabled science from Release 10 are given in the following journal publication:9: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 10: http://doi.org/10.3847/1538-4365/aa66d8 8: This particular data set, denoted in the original ascii files as Data_Release_4\hs_transport\surv\o0NNNx.survscf , where NNN=006-150 is an orbit number, and x = a or b for the orbit 130 or higher, indicates the first or the second half of the orbit, Survival Probabilities tables

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Antiram-directional 1-to-5-year Average West Ecliptic Maps in Mono Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Mono Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_year_1to5combinedMonoInertialFrame are pixel map data antiram-directional in Mono Inertial Frame, CG, no SP, 5 year cadence. 

IBEX Data Release-7, IBEX-Hi 5-year average maps in ascii list and image formats

The IBEX Release 7 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

Sequential number 1 - 22 for six-month maps from IBEX Data Release 16

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Antiram-directional 1-to-5-year Average West Ecliptic Maps in Var Energy Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_year_1to5combinedVarEnergyInertialFrame are pixel map data antiram-directional in Var Energy Inertial Frame, CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_mapX, where X = 1-10 are pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence. 

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Mono Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Mono Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_map_1to10combinedMonoInertialFrame are pixel map data from all directions (omnidirectional) in Mono Inertial Frame, CG, no SP, 5 year cadence. 

IBEX Data Release-7, IBEX-Hi 10 map average maps in ascii list and image formats

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Var Energy Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_map_1to10combinedVarEnergyInertialFrame are pixel map data from all directions (omnidirectional) in Var Energy Inertial Frame, CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of ram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_yearN for N=1,5, includes pixel map data from ram direction (ram-directional), CG, no SP, 1 year cadence. 

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Ram-directional 1-to-5-year Average West Ecliptic Maps in Mono Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Mono Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SCF Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_year_1to5combinedMonoInertialFrame are pixel map data ram-directional in Mono Inertial Frame, CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, no Survival-Probability, Ram-directional 1-to-5-year Average West Ecliptic Maps in Var Energy Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_year_1to5combinedVarEnergyInertialFrame are pixel map data ram-directional in Var Energy Inertial Frame, CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of antiram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_yearN for N=1,5, includes pixel map data from antiram direction (antiram-directional), CG, SP, 1 year cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, Antiram-directional 1-to-5-year Average West Ecliptic Maps in Mono Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Mono Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SCF Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_year_1to5combinedMonoInertialFrame are pixel map data antiram-directional in Mono Inertial Frame, CG, SP, 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_year_1to5combinedVarEnergyInertialFrame are pixel map data antiram-directional in Var Energy Inertial Frame, CG, SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (6 months-cadence) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_mapX, where X = 1-10 are pixel map data from all directions (omnidirectional), CG, SP, 6 month cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, Omnidirectional 1-to-10 map Average West Ecliptic Maps in Mono Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Mono Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_map_1to10combinedMonoInertialFrame are pixel map data from all directions (omnidirectional) in Mono Inertial Frame, CG, no SP, 5 year cadence. 

IBEX Data Release-7, IBEX-Hi 1-to-10-map average maps in ascii list and image formats

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Var Energy Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_map_1to10combinedVarEnergyInertialFrame are pixel map data from all directions (omnidirectional) in Var Energy Inertial Frame, CG, SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of ram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_yearN for N=1,5, includes pixel map data from ram direction (ram-directional), CG, SP, 1 year cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, Ram-directional 1-to-5-year Average West Ecliptic Maps in Mono Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Mono Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_year_1to5combinedMonoInertialFrame are pixel map data ram-directional in Mono Inertial Frame, CG, SP, 5 year cadence. 

IBEX-Hi Release 7; Compton-Getting, Survival-Probability, Ram-directional 1-to-5-year Average West Ecliptic Maps in Var Energy Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_year_1to5combinedVarEnergyInertialFrame are pixel map data ram-directional in Var Energy Inertial Frame, CG, SP, 5 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, no Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_yearN for N=1,5, includes pixel map data from antiram direction (antiram-directional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, no Survival-Probability, Antiram-directional 1-to-5-year Average West Ecliptic Maps in Var Energy SC Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of antiram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_year_1to5combinedVarEnergySCFrame are pixel map data antiram-directional in Var Energy SC Frame, no CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_mapX, where X = 1-10 are pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

IBEX-Hi Release 7; no Compton-Getting, no Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Var Energy SC Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with noCompton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_map_1to10combinedVarEnergySCFrame are pixel map data from all directions (omnidirectional) in Var Energy SC Frame, no CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of ram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_yearN for N=1,5, includes pixel map data from ram direction (ram-directional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, no Survival-Probability, Ram-directional 1-to-5-year Average West Ecliptic Maps in Var Energy Inertial Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy Inertial Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_year_1to5combinedVarEnergyInertialFrame are pixel map data ram-directional in Var Energy Inertial Frame, no CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_SP_antiram_nocg_yearN for N=1,5, includes pixel map data from antiram direction (antiram-directional), no CG, SP, 1 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of antiram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_year_1to5combinedVarEnergySCFrame are pixel map data antiram-directional in Var Energy SC Frame, no CG, no SP, 5 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft motion and correction (sp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_mapX, where X = 1-10 are pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Hi Release 7; no Compton-Getting, Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Var Energy SC Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Hi map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with noCompton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_map_1to10combinedVarEnergySCFrame are pixel map data from all directions (omnidirectional) in Var Energy SC Frame, no CG, SP, 5 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1 year-cadence) IBEX-Hi map data for the years 2009-2013 in the form of ram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and with correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_yearN for N=1,5, includes pixel map data from ram direction (ram-directional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 7; no Compton-Getting, Survival-Probability, Ram-directional 1-to-5-year Average West Ecliptic Maps in Var Energy SC Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-5-year-average) IBEX-Hi map data for the years 2009-2014 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_year_1to5combinedVarEnergySCFrame are pixel map data antiram-directional in Var Energy SC Frame, no CG, SP, 5 year cadence. 

IBEX-Hi Release-08; omni-direction 5-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Hi map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f2-ribbonMapsGAL includes f2 ribbon pixel map data from all directions (omnidirectional), 5 year cadence. 

IBEX Data Release 8, IBEX-Hi five-year maps in ascii list and image formats

The IBEX Release 8 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Hi map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f2-ribbonMapsJ2000 includes f2 ribbon pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Hi map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f2-ribbonMaps includes f2 ribbon pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Hi map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional GDF (Globally Distributed Flux) ENA (hydrogen) fluxes between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. gdf = Globally Distributed Flux. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f3-gdfGALACTIC includes f3 GDF (Globally Distributed Flux) pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Hi map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional GDF (Globally Distributed Flux) ENA (hydrogen) fluxes between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. gdf = Globally Distributed Flux. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f3-gdfJ2000 includes f3 GDF (Globally Distributed Flux) pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Hi map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional GDF (Globally Distributed Flux) ENA (hydrogen) fluxes between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. gdf = Globally Distributed Flux. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f3-gdfmaps includes f3 GDF (Globally Distributed Flux) pixel map data from all directions (omnidirectional), 5 year cadence. 

IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 one-year IBEX-Hi map data for the first seven years, 2009-2015, in the form of antiram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_yearN for N=1,7, includes pixel map data from antiram direction, CG, noSP, 1 year cadence. 

IBEX Mission, Instrument, and Data Release Description, Princeton

Interstellar Boundary Explorer, IBEX, Mission, Instrument, and Data Release Description, hosted by Princeton, Princeton

Interstellar Boundary Explorer, IBEX, Mission, Data Release 10, IBEX-Hi Maps in ASCII List Format and Image Format, hosted by the Space Physics Data Facility, SPDF, NASA

IBEX Data Release 10 Description, Astrophys. J. Suppl. Ser. Publication

McComas, D.J., Zirnstein, E.J., Bzowski, M., Dayeh, M.A., Funsten, H.O., Fuselier, S.A., Janzen, P.H., Kubiak, M.A., Kucharek, H., Mobius, E., Reisenfeld, D.B., Schwadron, N.A., Sokol, J.M., Szalay, J.R., and M. Tokumaru, Astrophysical Journal Supplement Series, 229:41, DOI:10.3847/1538-4365/aa66d8, 2017

IBEX High Energy Neutral Atom Imager, IBEX-Hi, Instrument Description, Space Sci. Rev. Publication

Funsten, H.O., Allegrini, F., Bochsler, P., Dunn, G., Ellis, S., Everett, D., Fagan, M.J., Fuselier, S.A., Granoff, M., Gruntman, M., Guthrie, A.A., Hanley, J., Harper, R.W., Heirtzler, D., Janzen, P., Kihara, K.H., King, B., Kucharek, H., Manzo, M.P., Maple, M., Mashburn, K., McComas, D.J., Moebius, E., Nolin, J., Piazza, D., Pope, S., Reisenfeld, D.B., Rodriguez, B., Roelof, E.C., Saul, L., Turco, S., Valek, P., Weidner, S., Wurz, P., and S. Zaffke, The Interstellar Boundary Explorer High Energy (IBEX-Hi) Neutral Atom Imager, Space Science Review, 146: 75-103, DOI:10.1007/s11214-009-9504-y, 2009

The IBEX Release 10 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of antiram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_ single, includes pixel map data from antiram direction, CG, noSP, 7 year cadence. 

IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for the first seven years, 2009-2015, with multiple versions of data sets including no corrections, full corrections for spacecraft  motion, and corrections for ENA survival probability between 1 and 100 AU. 3: The data consist of all-sky maps in Solar West Ecliptic angles of ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication: 4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6: cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. 7: nocg = no Compton-Getting corrections 8: sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. 9: noSP - no survival probability corrections have been applied to the data. 10: omni = data from all directions. 11: ram = data was collected when the spacecraft was ramming into the incoming ENAs. 12: antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 13: The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015). 14: Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/200915: Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/200916: Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/201017: Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/201018: Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/201119: Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/201120: Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/201221: Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/201222: Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/201323: Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/201324: Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/201425: Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/201426: Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/201527: Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/201528: This particular data set, denoted in the original ascii files as hvset_cg_mapN for N=1,14, includes pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence. 

IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of omni-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_cg_ single, includes pixel map data from omni direction, CG, noSP, 7 year cadence. 

IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 one-year IBEX-Hi map data for the first seven years, 2009-2015, in the form of ram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_yearN for N=1,7, includes pixel map data from RAM direction (ram-direction), CG, noSP, 1 year cadence. 

IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, ram-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of ram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_ single, includes pixel map data from ram direction, CG, noSP, 7 year cadence. 

IBEX-Hi Release-10; Compton-Getting, Survival-Probability, AntiRAMdirectional 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (1-year-cadence) IBEX-Hi map data for the first seven years, 2009-2015, in the form of anti-RAM-directional fluxes with corrections for spacecraft motion (cg: Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_yearN for N=1,7, includes pixel map data from antiRAM direction (antiRAMdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release-10; Compton-Getting, Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of antiram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_single, includes pixel map data from antiram direction, CG,SP, 7 year cadence. 

IBEX-Hi Release-10; Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes with corrections (cg) for spacecraft motion (Compton-Getting) and corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_cg_tabular_mapN for N=1,14, includes pixel map data from all directions (omnidirectional), CG, SP, 6 month cadence. 

IBEX-Hi Release-10; Compton-Getting, Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of omni-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_cg_tabular_ single, includes pixel map data from omni direction, CG,SP, 7 year cadence. 

IBEX-Hi Release-10; Compton-Getting, Survival-Probability, RAMdirectional 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (1-year-cadence) IBEX-Hi map data for the first seven years, 2009-2015, in the form of RAM-directional fluxes with corrections for spacecraft motion (cg: Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_yearN for N=1,7, includes pixel map data from RAM direction (RAMdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release-10; Compton-Getting, Survival-Probability, ram-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of ram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_single, includes pixel map data from ram direction, CG,SP, 7 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 one-year IBEX-Hi map data for the first seven years, 2009-2015, in the form of antiram-direction fluxes with no corrections for spacecraft motion (nocg: no Compton-Getting) and with no corrections (nosp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_yearN for N=1,7, includes pixel map data from antiram direction, CG, noSP, 1 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of antiram-direction fluxes with no corrections for spacecraft motion (nocg: Compton-Getting) and with no corrections (nosp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_single, includes pixel map data from antiram direction, noCG, noSP, 7 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes without any corrections (nocg) for spacecraft motion (Compton-Getting) and ENA survival probability (nosp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_mapN for N=1,14, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of omni-direction fluxes with no corrections for spacecraft motion (nocg: Compton-Getting) and with no corrections (nosp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_single, includes pixel map data from omni direction, noCG, noSP, 7 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 one-year IBEX-Hi map data for the first seven years, 2009-2015, in the form of ram-direction fluxes with no corrections for spacecraft motion (nocg: no Compton-Getting) and with no corrections (nosp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_noSP_ram_yearN for N=1,7, includes pixel map data from antiram direction, CG, noSP, 1 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 one-year IBEX-Hi map data for the first seven years, 2009-2015, in the form of antiram-direction fluxes with no corrections for spacecraft motion (nocg: no Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_noSP_antiram_yearN for N=1,7, includes  pixelmap data from anti ramdirection, noCG, SP, 1 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of antiram-direction fluxes with no corrections for spacecraft motion (nocg: Compton-Getting) but with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_single, includes pixel map data from antiram direction, noCG, SP, 7 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for the first seven years, 2009-2015, with multiple versions of data sets including no corrections, full corrections for spacecraft  motion, and corrections for ENA survival probability between 1 and 100 AU. 3: The data consist of all-sky maps in Solar West Ecliptic angles of ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication: 4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6: cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. 7: nocg = no Compton-Getting corrections 8: sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. 9: noSP - no survival probability corrections have been applied to the data. 10: omni = data from all directions. 11: ram = data was collected when the spacecraft was ramming into the incoming ENAs. 12: antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 13: The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015). 14: Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/200915: Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/200916: Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/201017: Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/201018: Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/201119: Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/201120: Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/201221: Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/201222: Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/201323: Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/201324: Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/201425: Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/201426: Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/201527: Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/201528: This particular data set, denoted in the original ascii files as hvset_tabular_mapN for N=1,14, includes pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 seven-year IBEX-Hi map data for 2009-2015, in the form of omni-direction fluxes with no corrections for spacecraft motion (nocg: Compton-Getting) but with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_single, includes pixel map data from omni direction, noCG, noSP, 7 year cadence. 

IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 one-year IBEX-Hi map data for the first seven years, 2009-2015, in the form of ram-direction fluxes with no corrections for spacecraft motion (nocg: no Compton-Getting) and with corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: This particular data set, denoted in the original ascii files as hvset_tabular_noSP_ram_yearN for N=1,7, includes  pixelmap data from ramdirection, noCG, SP, 1 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the IBEX-Hi Release 12 Count Data for Magnetospheric Imaging. This release provides data for various IBEX orbits from 23 (2009-03-26) to 207b (2013-05-30). The data include 21 orbits from IBEX-Hi 6-degree histogram ENA count data, which is primarily what have been used in IBEX magnetospheric studies.3. The data consist of IBEX-Hi Count Data for Magnetospheric Imaging during instrument pointing in spin angle 0 - 360 degrees between the north and south Ecliptic poles. Spin angle zero corresponds to the north Ecliptic pole. Counts come from IBEX-Hi energy bands 2-6 in numerical data form corresponding to energy bins 2-6: 2) ~0.71, 3) ~1.11, 4) ~1.74, 5) ~2.73, 6) ~4.3 keV. Background counts have not been removed. Counts are separated into 6-degree latitudinal bins, with each # angle label representing the center of the bin. Details of the data and enabled science from Release 12 are given in the following journal publications: McComas et al. 2011,2012b; Fuselier et al. 2010, 2015; Petrinec et al. 2011; Ogasawara et al. 2013, 2019; and Dayeh et al. 2015Data Location: http://ibex.swri.edu/ibexpublicdata/Data_Release_12/index.htmlContact: Maher Dayeh, Southwest Research Institute, San Antonio, TX maldayeh@swri.edu Orbit Start and End Times:23: 2009-03-26 21:09:00.318 to 2009-04-03 16:07:51.74324: 2009-04-03 12:10:21.253 to 2009-04-11 08:15:09.66925: 2009-04-11 05:06:40.967 to 2009-04-18 22:05:11.12527: 2009-04-26 08:27:40.916 to 2009-05-04 05:31:06.51928: 2009-05-04 02:02:57.673 to 2009-05-11 21:13:47.59629: 2009-05-11 17:27:02.484 to 2009-05-19 19:27:18.83151: 2009-10-26 08:19:34.905 to 2009-11-03 02:38:01.73052: 2009-11-02 22:34:07.792 to 2009-11-10 19:03:55.23053: 2009-11-10 15:46:22.161 to 2009-11-18 10:58:17.67455: 2009-11-25 23:44:19.069 to 2009-12-03 11:26:37.15156: 2009-12-03 08:22:31.792 to 2009-12-10 22:03:52.60457: 2009-12-10 18:55:33.969 to 2009-12-18 06:58:47.24772: 2010-04-04 11:17:28.386 to 2010-04-12 09:13:51.00874: 2010-04-19 14:09:01.851 to 2010-04-27 03:44:14.91377: 2010-05-12 01:33:51.796 to 2010-05-19 20:43:01.58378: 2010-05-19 17:33:48.047 to 2010-05-27 13:02:03.396103: 2010-11-26 07:56:05.324 to 2010-12-04 04:11:44.879187a: 2012-11-21 00:17:13.430 to 2012-11-25 00:40:26.707188b: 2012-12-03 12:46:18.859 to 2012-12-08 00:44:50.846206a: 2013-05-13 23:15:27.433 to 2013-05-17 12:19:58.215207b: 2013-05-26 12:21:08.868 to 2013-05-30 23:14:44.989For the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~7.5 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 7.5 apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b'. Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV).

Interstellar Boundary Explorer, IBEX, Mission, Data Release 12, IBEX-Hi Count Data for Magnetospheric Imaging in ASCII Format, hosted by the Space Physics Data Facility, SPDF, NASA

Fuselier, S.A., H.O. Funsten, D. Heirtzler, P. Janzen, H. Kucharek, D.J. McComas, E. Mobius, T.E. Moore, S.M. Petrinec, D.B. Reisenfeld, N.A. Schwadron, K.J. Trattner, and P. Wurz, Energetic neutral atoms from the Earth's subsolar magnetopause, Geophys. Res. Lett., 37, doi:10.1029/2010GL044140, 2010.

McComas, D.J., M.A. Dayeh, H.O. Funsten, S.A. Fuselier, J. Goldstein, J.M. Jahn, P. Janzen, D.G. Mitchell, S.M. Petrinec, D.B. Reisenfeld, and N.A. Schwadron, First IBEX observations of the terrestrial plasma sheet and a possible disconnection event, J. Geophys. Res., 116, doi:10.1029/2010JA016138, 2011.

Petrinec et al. 2011 Journal of Geophysical Research Publication

Petrinec, S.M., M.A. Dayeh, H.O. Funsten, S.A. Fuselier, D. Heirtzler, P. Janzen, H. Kucharek, D.J. McComas, E. Mobius, T.E. Moore, D.B. Reisenfeld, N.A. Schwadron, K.J. Trattner, and P. Wurz, Neutral atom imaging of the magnetospheric cusps, J. Geophys. Res., 116, doi:10.1029/2010JA016357, 2011.

McComas D.J., N. Buzulukova, M.G. Connors, M.A. Dayeh, J. Goldstein, H.O. Funsten, S. Fuselier, N.A. Schwadron, and P. Valek, Two Wide-Angle Imaging Neutral-Atom Spectrometers and Interstellar Boundary Explorer energetic neutral atom imaging of the 5 April 2010 substorm, J. Geophys. Res., doi:10.1029/2011JA017273, 2012.

Ogasawara et al. 2013 Journal of Geophysical Research Publication

Ogasawara, K., V. Angelopoulos, M.A. Dayeh, S.A. Fuselier, G. Livadiotis, D.J. McComas, J.P. McFadden, Characterizing the dayside magnetosheath using energetic neutral atoms: IBEX and THEMIS observations, J. Geophys. Res., doi:10.1002/jgra.50353, 2013.

Dayeh, M.A., S.A. Fuselier, H.O. Funsten, D.J. McComas, K. Ogasawara, S.M. Petrinec, N.A. Schwadron, and P. Valek, Shape of the terrestrial plasma sheet in the near-Earth magnetospheric tail as imaged by the Interstellar Boundary Explorer, Geophys. Res. Lett., 42, 7, 2115-2122, doi:10.1002/2015GL063682, 2015.

Fuselier S.A., M.A. Dayeh, G. Livadiotis, D.J. McComas, K. Ogasawara, P. Valek, H.O. Funsten, and S.M. Petrinec, Imaging the development of the cold dense plasma sheet, Geophys. Res. Lett., doi:10.1002/2015GL065716, 2015.

The IBEX Release 12 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release12/ena_hi_magnetosphere_24min/ibex_h3_ena_hi_r12_magnetosphere_24min_20090326_orbit0023_v01.cdf. The most common cadence, 4194304 [ms] = PT1H9M54.304S, occurred for 32.5203% of the 160 timesteps. 

Total Counts for Spin Angle Bins at Hi Energy Channel 2 ~0.71 keV

Total Counts for Spin Angle Bins at Hi Energy Channel 3 ~1.11 keV

Total Counts for Spin Angle Bins at Hi Energy Channel 4 ~1.74 keV

Total Counts for Spin Angle Bins at Hi Energy Channel 5 ~2.73 keV

Total Counts for Spin Angle Bins at Hi Energy Channel 6 ~4.29 keV

IBEX-Hi Release-13; Compton-Getting, no Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the Release 13 one-year IBEX-Hi map data for the nine years, 2009-2018, in the form of antiram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 13 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 13 map numbers (1-20) with mission year (1-10), orbits (11-431bb), and dates (12/25/2008-12/26/2018); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015-06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016-12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016-06/25/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017-12/25/2017Map 19: year 10, orbits 391a-411b, dates 12/25/2017-06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018-12/26/20188: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_yearN for N=8, includes pixel map data from antiram direction, CG, noSP, 1 year cadence. 

Interstellar Boundary Explorer, IBEX, Mission, Data Release 13, IBEX-Hi Maps in ASCII List Format and Image Format, hosted by the Space Physics Data Facility, SPDF, NASA

The IBEX Release 13 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

IBEX-Hi Release-13; Compton-Getting, no Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the Release 13 one-year IBEX-Hi map data for the nine years, 2009-2018, in the form of ram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU.  3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 13 map numbers (1-20) with mission year (1-10), orbits (11-431bb), and dates (12/25/2008-12/26/2018); each year is associated with two consecutive maps;Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015-06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016-12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016-06/25/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017-12/25/2017Map 19: year 10, orbits 391a-411b, dates 12/25/2017-06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018-12/26/20188: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_yearN for N=8, includes pixel map data from antiram direction, CG, noSP, 1 year cadence. 

IBEX-Hi Release-14; Compton-Getting, no Survival-Probability, ram-direction 3-year-Average West Ecliptic Pressure andFlux Power-Law Slope Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is derived from the Release 14 three-year IBEX-Hi map data with two-year overlaps to adjacent maps, 2009-2011, 2010-2012, 2011-2013, and so forth through 2015-2017 from ram-direction fluxes with corrections for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival probability between 1 and 100 AU. The data set parameters include line-of-sight (LOS) integrated pressures separately computed from the Global Distributed Flux (GDF), the ribbon flux, and the total of both LOS pressures. Additionally there are signal/noise ratios for the GDF, ribbon, and total pressures. Finally, there are power-law slope and values for the GDF differential flux, also including signal/noise of the slope.  3: The data consist of ram-direction sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for the above parameters. 4: Details of the data and enabled science from Release 14 are given in the following journal publication: Schwadron, N. A., et al. (2018), Time Dependence of the IBEX Ribbon and the Globally Distributed Energetic Neutral Atom Flux Using the First 9 Years of Observationshttps://iopscience.iop.org /article/10.3847/1538-4365/aae48e/meta5: The following codes are used to define dataset types in the multiple IBEX data releases:  cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 6: This particular dataset denoted in the original ascii files as:-- GDFPressure: Globally Distributed Flux Line-of-Sight Integrated Pressure in pdyne-au/cm^2-- GDFSlope: Power-Law Slope of the differential flux spectrum for the Globally Distributed Flux-- GDFSlopeSN: Signal/Noise ratio of the GDF differential flux power-law slope where noise represents uncertainty -- GDFSN: Globally Distributed Flux Signal/Noise, where Noise is defined as the uncertainty and the Signal is GDF Line-of-Sight -integrated pressure-- RibbonPressure: Ribbon Line-of-Sight Integrated Pressure in pdyne-au/cm^2-- RibbonSN: Ribbon Signal/Noise, where Noise is defined as the uncertainty and the Signal is GDF  Line-of-Sight -integrated pressure-- TotPressure: Total Pressure in ENA maps including both the GDF and Ribbon. Line-of-Sight Integrated Pressure in pdyne-au/cm^2-- TotSN: Total Pressure Signal-to-Noise where noise represents uncertainty and signal represents the total LOS-integrated pressure

The IBEX Release 14 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

Sequential number 1 - 10 for six-month maps from IBEX Data Release 10

Total Pressure in ENA maps including both the GDF and Ribbon. Line-of-Sight Integrated Pressure in pdyne-au/cm^2 - mapped

IBEX-Hi Release 15; Compton-Getting, Survival-Probability, in a ribbon centered frame, 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 15 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. ribcen = maps are in a ribbon centered frame. 7. The following list associates Release 15 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: Data Release 15 description:  Maps are in a ribbon centered frame. Data are Compton-Getting and Survival Probability corrected.  Centers for different energies are as follows (following Funsten et al. 2013):  Map Centers for each energy (in eclipticJ2000; [lon,lat]):  ESA2 ribbon center : b_lon_lat_ec = [218.5, 43.1]  ESA3 ribbon center : b_lon_lat_ec = [220.3, 40.5]  ESA4 ribbon center : b_lon_lat_ec = [219.6, 39.8]  ESA5 ribbon center : b_lon_lat_ec = [217.9, 37.7]  ESA6 ribbon center : b_lon_lat_ec = [214.2, 32.4] 9: This particular data set, denoted in the original ascii files as ribcen_esaN_hvset_tabular_cg_YYYY for N=2-6, and YYYY = 2009-2017, includes pixel map data from ribbon centered frame, CG, SP, 1 year cadence.

IBEX Data Release-16, IBEX-Hi one-year-maps in ascii list and image formats

The IBEX Release 15 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

IBEX-Hi Release 15; Compton-Getting, Survival-Probability, in a ribbon centered frame, 2-Year-Averaged West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 15 (2 or 3 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. ribcen = maps are in a ribbon centered frame. Combined maps information: years01-03 refers to 2009, 2010, 2011  years04-05 refers to 2012, 2013;  years06-07 refers to 2014, 2015;  years08-09 refers to 2016, 2017. 7. The following list associates Release 15 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: Data Release 15 description:  Maps are in a ribbon centered frame. Data are Compton-Getting and Survival Probability corrected.  Centers for different energies are as follows (following Funsten et al. 2013):  Map Centers for each energy (in eclipticJ2000; [lon,lat]):  ESA2 ribbon center : b_lon_lat_ec = [218.5, 43.1]  ESA3 ribbon center : b_lon_lat_ec = [220.3, 40.5]  ESA4 ribbon center : b_lon_lat_ec = [219.6, 39.8]  ESA5 ribbon center : b_lon_lat_ec = [217.9, 37.7]  ESA6 ribbon center : b_lon_lat_ec = [214.2, 32.4] 9: This particular data set, denoted in the original ascii files as ribcen_esa2_hvset_tabular_cg_single_yearsYYY for YYY = 123 refers to 2009, 2010, 2011; YYY = 45 refers to 2012, 2013; YYY = 67 refers to 2014, 2015; YYY = 89 refers to 2016, 2017; For instance, ribcen_esa5_hvset_tabular_cg_single_years45 contains data for combined years 2012 and 2013 at ESA 5. The set includes pixel map data from ribbon centered frame, CG, SP, 2 or 3 year cadence.

IBEX Data Release-15, IBEX-Hi one-year-maps in ascii list and image formats

Sequential starting number 1 - 22 for six-month map from IBEX Data Release 15

IBEX-Hi Release 15; Compton-Getting, Survival-Probability, in a ribbon centered frame, 3-Year-Averaged West Ecliptic Maps

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, ANTIRAMdirectional 11-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11-year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_antiram_cg_single includes pixel map data from antiram direction (antiram-directional), CG, NOSP, 11 year cadence. 

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_antiram_cg_N for N=2009,2019, includes pixel map data from antiram direction (antiram-directional), CG, NOSP, 1 year cadence. 

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, ANTIRAMdirectional mono-energy 11-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_single\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, no SP, mono-energy, 11 year cadence.

IBEX Data Release-16, IBEX-Hi 11-year-maps in ascii list and image formats

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, ANTIRAMdirectional mono-energy 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2019, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, no SP, mono-energy, 1 year cadence.

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, Omnidirectional 11-year-Average West Ecliptic Maps

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_NX for N=2009,2019, which indicates a year data collected, and X = A or B, showing first or second half of the year, includes pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence. 

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, Omnidirectional, mono-energy 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11 year-cadence) IBEX-Hi map data averaged for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_single/hv60.hide-trp-mono_80-m-v, where m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from all directions (omnidirectional), CG, no SP, mono-energy, 11 year cadence.

IBEX Data Release-16, IBEX-Hi 11 year maps in ascii list and image formats

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, Omnidirectional, mono-energy 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_NX/hv60.hide-trp-mono_80-m-v, where N=2009 - 2019, which indicates a year data collected, and X = A or B, showing first or second half of the year, m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from all directions (omnidirectional), CG, NOSP, mono-energy, 6 month cadence.

IBEX Data Release-16, IBEX-Hi six-month maps in ascii list and image formats

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, ram-directional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_single, includes pixel map data from ram direction, CG, no SP, 11 year cadence. 

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_N for N=2009,2019, includes pixel map data from ram direction (ram-directional), CG, no SP, 1 year cadence. 

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, RAMdirectional mono-energy 11-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_single\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, no SP, mono-energy, 11 year cadence.

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, RAMdirectional mono-energy 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2019, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, no SP, mono-energy, 1 year cadence.

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, Antiram-directional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_single, includes pixel map data from antiram direction, CG, SP, 11 year cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_N for N=2009,2019, includes pixel map data from antiram direction (antiram-directional), CG, SP, 1 year cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, ANTIRAMdirectional, mono-energy 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11 year-cadence) IBEX-Hi map data averaged for the years 2009-2019 in the form of ANTIRAMdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_single/hv60.hide-trp-mono_80-m-v, where m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from ANTIRAM direction (ANTIRAMdirectional), CG, SP, mono-energy, 11 year cadence.

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, ANTIRAMdirectional mono-energy 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2019, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, Omnidirectional 11-year-Average West Ecliptic Maps

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, Omnidirectional 2-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 (2 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_single_Nyears, where N = 2 or 3, shows number of years of averaging, includes pixel map data from all directions (omnidirectional), CG, SP, 2 year cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, Omnidirectional 3-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 (3 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_single_Nyears, where N = 2 or 3, shows number of years of averaging, includes pixel map data from all directions (omnidirectional), CG, SP, 3 year cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_NX for N=2009,2019, which indicates a year data collected, and X = A or B, showing first or second half of the year, includes pixel map data from all directions (omnidirectional), CG, SP, 6 month cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, Omnidirectional, mono-energy 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11 year-cadence) IBEX-Hi map data averaged for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_single/hv60.hide-trp-mono_80-m-v, where m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from all directions (omnidirectional), CG, SP, mono-energy, 11 year cadence.

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, Omnidirectional, mono-energy 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp)mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_NX/hv60.hide-trp-mono_80-m-v, where N=2009 - 2019, which indicates a year data collected, and X = A or B, showing first or second half of the year, m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from all directions (omnidirectional), CG, SP, mono-energy, 6 month cadence.

IBEX-Hi Release 16; Compton-Getting, no Survival-Probability, Ram-directional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_single, includes pixel map data from ram direction, CG, SP, 11 year cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directionl ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_N for N=2009,2019, includes pixel map data from ram direction (ram-directional), CG, SP, 1 year cadence. 

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, RAMdirectional, mono-energy 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (11 year-cadence) IBEX-Hi map data averaged for the years 2009-2019 in the form of RAMdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_cg_tabular_single/hv60.hide-trp-mono_80-m-v, where m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from RAM direction (RAMdirectional), CG, SP, mono-energy, 11 year cadence.

IBEX-Hi Release 16; Compton-Getting, Survival-Probability, RAMdirectional mono-energy 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2019, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_single, includes pixel map data from antiram direction, no CG, no SP, 11 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, no Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_N for N=2009,2019, includes pixel map data from antiram direction (antiram-directional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, no Survival-Probability, Omnidirectional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_single, includes pixel map data from all directions (omnidirectional), noCG, noSP, 11 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (6 months-cadence) IBEX-Hi map data for the  years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_NX for N=2009,2019, which indicates a year data collected, and X = A or B, showing first or second half of the year, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_single, includes pixel map data from ram direction, no CG, no SP, 11 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_noSP_ram_N for N=2009,2019, includes pixel map data from ram direction (ram-directional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, Antiram-directional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_single, includes pixel map data from antiram direction, no CG, SP, 11 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of antiram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and withcorrection for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_N for N=2009,2019, includes pixel map data from ram direction (ram-directional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, Omnidirectional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and with correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_single, includes pixel map data from all directions (omnidirectional), noCG, SP, 11 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (6 months-cadence) IBEX-Hi map data for the years 2009-2019 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_NX for N=2009,2019, which indicates a year data collected, and X = A or B, showing first or second half of the year, includes pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, Ram-directional 11-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_single, includes pixel map data from ram direction, no CG, SP, 11 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 (1 year-cadence) IBEX-Hi map data for the years 2009-2019 in the form of ram-directionl ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and withcorrection for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_N for N=2009,2019, includes pixel map data from ram direction (ram-directional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, Ram-directional 11-year-Average West Ecliptic Maps in Equatorial coordinates

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU in Equatorial Coordinates. 3. The data consist of all-sky maps in Solar Equatorial Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_equatorial_single, includes pixel map data from ram direction, no CG, SP, 11 year cadence in equatorial coordinates. 

IBEX-Hi Release 16; no Compton-Getting, Survival-Probability, Ram-directional 11-year-Average West Maps in Galactic coordinates

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 16 IBEX-Hi map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU in Galactic Coordinates. 3. The data consist of all-sky maps in Solar Galactic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_tabular_ram_galactic_single, includes pixel map data from ram direction, no CG, SP, 11 year cadence in galactic coordinates. 

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, Antiram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, no SP, 14 year cadence. 

IBEX Data Release-18, IBEX-Hi six-month maps in ascii list and image formats

The IBEX Release 18 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, Antiramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, no SP, 1 year cadence. 

IBEX Data Release 18, IBEX-Hi 1-year maps in ascii list and image formats

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, ANTIRAMdirectional mono-energy 14-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (14 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_2009-2022\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, no SP, mono-energy, 14 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, ANTIRAMdirectional mono-energy 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, no SP, mono-energy, 1 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX Data Release-18, IBEX-Hi one-year-maps in ascii list and image formats

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, omni-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of omni-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_cg_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from OMNI direction (omnidirectional), CG, no SP, 14 year cadence. 

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (6 months-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_cg_NM/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, M = 'A' or 'B' showing the first or second half of the year, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence. 

IBEX Data Release 18, IBEX-Hi six-month maps in ascii list and image formats

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, OMNIdirectional mono-energy 14-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (14 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_noSP_omni_cg_2009-2022\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from omni direction, CG, no SP, mono-energy, 14 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, Omnidirectional mono-energy 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (6 months-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_cg_NM/hv60.hide-trp-mono_80-m-v, where N=2009-2022, which indicates a year data collected, and M = A or B, showing first or second half of the year, m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from all directions (omnidirectional), CG, no SP, mono-energy, 6 month cadence.

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, ram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), CG, no SP, 14 year cadence. 

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, Ramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), CG, no SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, RAMdirectional mono-energy 14-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (14 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_2009-2022\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, no SP, mono-energy, 14 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, no Survival-Probability, RAMdirectional mono-energy 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, no SP, mono-energy, 1 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_cg_tabular_antiram_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 14 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional lower gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_antiram_cg_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional lower gdf mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_antiram_cg_gdf_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional lower ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_antiram_cg_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional lower ribbon mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_antiram_cg_ribbon_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional median gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_antiram_cg_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional median gdf mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_antiram_cg_gdf_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional median ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_antiram_cg_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional median ribbon mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_antiram_cg_ribbon_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, ANTIRAMdirectional mono-energy 14-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (14 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_2009-2022\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 14 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional upper gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_antiram_cg_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional upper gdf mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_antiram_cg_gdf_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional upper ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_antiram_cg_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Antiramdirectional upper ribbon mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_antiram_cg_ribbon_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from antiram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, omni-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of omni-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_cg_tabular_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from OMNI direction (omnidirectional), CG, SP, 14 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (6 months-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_cg_tabular_NM/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, M = 'A' or 'B' showing the first or second half of the year, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from all directions (omnidirectional), CG, SP, 6 month cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, OMNIdirectional mono-energy 14-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (14 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_tabular_omni_cg_2009-2022\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from omni direction, CG, SP, mono-energy, 14 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Omnidirectional mono-energy 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (6 months-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_cg_tabular_NM/hv60.hide-trp-mono_80-m-v, where N=2009-2022, which indicates a year data collected, and M = A or B, showing first or second half of the year, m = 0.71, 1.11, 1.74, 2.73, or 4.29 showing the energy of the channel, and v = 'flux', 'fvar', or 'fsnr', includes pixel map data from all directions (omnidirectional), CG, SP, mono-energy, 6 month cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, ram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_cg_tabular_ram_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), CG, SP, 14 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional lower gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_ram_cg_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, ramdirectional lower gdf mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_ram_cg_gdf_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional lower ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_ram_cg_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, ramdirectional lower ribbon mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_ram_cg_ribbon_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional median gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_ram_cg_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, ramdirectional median gdf mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_ram_cg_gdf_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional median ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_ram_cg_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, ramdirectional median ribbon mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_ram_cg_ribbon_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, RAMdirectional mono-energy 14-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (14 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_2009-2022\hv60.hide-trp-mono_80-M-V , where M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 14 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/20197: This particular data set, denoted in the original ascii files as hvset_tabular_ram_cg_N\hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/2022

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional upper gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_ram_cg_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional upper gdf mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_ram_cg_gdf_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional upper ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_ram_cg_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), CG, SP, 1 year cadence. 

IBEX-Hi Release 18; Compton-Getting, Survival-Probability, Ramdirectional upper ribbon mono-energy 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) mono-energy (mono) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_ram_cg_ribbon_N/hv60.hide-trp-mono_80-M-V , where N=2009,2022, M = 0.71, 1.11, 1.74, 2.73,  4.29 showing the energy of the channel, and V = 'flux', 'fvar', or 'fsnr', includes pixel map data from ram direction, CG, SP, mono-energy, 1 year cadence.

IBEX-Hi Release 18; no Compton-Getting, no Survival-Probability, Antiram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of antiram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, no SP, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, no Survival-Probability, Antiramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, no SP, 6 month cadence. 

IBEX-Hi Release 18; no Compton-Getting, no Survival-Probability, omni-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of omni-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from OMNI direction (omnidirectional), no CG, no SP, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (6 months-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_NM/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, M = 'A' or 'B' showing the first or second half of the year, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

IBEX-Hi Release 18; no Compton-Getting, no Survival-Probability, ram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_noSP_ram_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), no CG, no SP, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, no Survival-Probability, Ramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_noSP_ram_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), no CG, no SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of antiram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_noSP_antiram_cg_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_tabular_antiram_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional lower gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_antiram_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional lower ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_antiram_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional median gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_antiram_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional median ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_antiram_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional upper gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_antiram_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Antiramdirectional upper ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_antiram_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from ANTIRAM direction (antiramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, omni-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of omni-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from OMNI direction (omnidirectional), no CG, SP, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (6 months-cadence) IBEX-Hi map data for the years 2009-2022 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and with correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_tabular_NM/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, M = 'A' or 'B' showing the first or second half of the year, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, ram-directional 14-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_noSP_ram_cg_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as hvset_tabular_ram_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, ram-directional 14-year-Average West Ecliptic Maps in Equatorial coordinates

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU in equatorial coordinates. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_tabular_ram_equatorial_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), no CG, SP, in equatorial coordinates, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, ram-directional 14-year-Average West Ecliptic Maps in galactic coordinates

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 IBEX-Hi map data for the years 2009-2022 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU in galactic coordinates. 3. The data consist of all-sky maps in Solar Galactic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 4. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 5. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20226: This particular data set, denoted in the original ascii files as hvset_tabular_ram_galactic_2009-2022/hv60.hide-trp-flux100-hi-R-F.txt, where R shows the energy level from 2 to 6, and F shows the variable: 'cnts', 'flux', 'fexp', 'ener', 'fsnr', 'fvar', or 'numb' includes pixel map data from RAM direction (ramdirectional), no CG, SP, in galactic coordinates, 14 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional lower gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_ram_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional lower ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonlower/hvset_tabular_ram_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional median gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_ram_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional median ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonmedian/hvset_tabular_ram_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional upper gdf 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_ram_gdf_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

IBEX-Hi Release 18; no Compton-Getting, Survival-Probability, Ramdirectional upper ribbon 1-year-average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of ramdirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. gdf = globally distributed flux maps ribbon = ribbon maps 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as ribbonupper/hvset_tabular_ram_ribbon_N/hv60.hide-trp-flux100-hi-R-F.txt, where N is the year from 2009 to 2022, R shows the energy level from 2 to 6, and F shows the variable: 'flux', 'fexp', 'fvar' includes pixel map data from RAM direction (ramdirectional), no CG, SP, 1 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2022. 2: This data set is from the Release 3, 7.5 days cadence, IBEX-Lo data for the years 2009 - 2010 contains data used in the publication of Moebius et al., 2012, Interstellar Gas Flow Parameters Derived from IBEX-Lo Observations in 2009 and 2010 Analytical Analysis and Bzowski et al., 2012, Neutral interstellar helium parameters based on IBEX-Lo observations and test particle calculations. The data are the 6 degree resolution corrected histogram data and the observation time periods in one csv file for each orbit for both the angular fit analysis and the count rate analysis. 3: Additional publications: Bzowski et al., 2012, Neutral interstellar helium parameters based on IBEX-Lo observations and test particle calculations; and Hlond et al., 2012, Precision Pointing of IBEX-Lo Observations. 4: Data Selection: In order to determine accurately the interstellar gas flow vector, the pointing of IBEX-Lo has to be known to about 0.1 degree accuracy for the observations used in this analysis. It is demonstrated that the pointing of the IBEX-Lo star sensor and of the spacecraft star tracker agree within this prescribed accuracy for time periods of simultaneous good observations (Hlond et al., 2012). The data used from time periods when the IBEX star tracker, which provides precision pointing information for the routine data processing, was operating within its specifications for all analysis that requires exact pointing knowledge, such as the evaluation of the flow distributions in latitude. However, the determination of the ISM flow maximum in ecliptic longitude only requires the use of the count rates, obtained over plus-minus 3 sigma of the angular distribution from the latitude peak position, as a function of longitude, so this requirement can be relaxed. 5: During the analysis, it was found that the data transfer through the CEU that formats the information for the telemetry slows down because of the total traffic across the interface and the computational load event rates that exceed about 10 counts/s, as observed during the He ISM flow peak. This slow down produces a modulation in the high-resolution data according to the accumulation scheme into 6 deg sectors. Therefore, the only data integrated 6-deg sector for He used in this analysis. In addition, IBEX-Lo detects background electrons, which are identified as invalid events by the TOF spectrometer, but they have to be removed by the CEU, which adds to its load and the slow down when electron rates increase.  6: For this analysis, a list of valid time periods was compiled for the ISM flow analysis that is used throughout this paper and also in the analysis by Bzowski et al. (2012). Excluded from this list are time periods, for which the following conditions apply: 7: IBEX is close to the magnetosphere, where IBEX-Lo observes high count rates of magnetospheric ENAs and ions, based on angular ranges outside the ISM flow distribution. 8: The Moon is in the IBEX FoV. These times are taken from the ISOC command files, which contain special commanding for the star sensor. 9: The electron rates for IBEX-Lo are high. These times are identified in the IBEX-Lo TOF count rates, when the otherwise very stable base count rate outside the ISM flow direction is exceeded by more than a factor of 1.6 (safely above any stochastic fluctuations of the base count rate, but low enough to indicate any significant electron rate increases). 10: The star tracker function has been impaired. This affects the determination of the ISM peak location and width in latitude. 11: No further culling for increased background counts (routinely performed for suprathermal ENA observations (McComas et al. 2009b) is necessary for ISM flow observations because of the concentrated angular distributions at much higher rates. The angular distribution analysis, in general, is performed on much shorter .good. time periods than the count rate analysis because nominal operation of the star tracker is required. Because the rate analysis requires contiguous time sections of fixed length to achieve approximately comparable counting statistics for each data point, very small portions at the beginning or end of the .good. time intervals may be unused, which accounts for the occasional foreshortening of the .good. time intervals for the rate analysis at the beginning or the end. 12: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 This particular data set is denoted in the original ascii files in https://ibex.princeton.edu/DataRelease3 as Interstellar Gas Flow Parameters Accumulated Count Data Used in the Count Rate Analysis. 

The IBEX Release 3 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release03/ena_lo_angular_analysis_7day/ibex_h3_ena_lo_r03_angular_analysis_7day_20090103_orb0012_v01.cdf. The most common cadence, 32400000 [ms] = PT9H, occurred for 88.8889% of the 8 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release03/ena_lo_ct_rate_analysis_7day/ibex_h3_ena_lo_r03_ct_rate_analysis_7day_20090102_orb0012_v01.cdf. The most common cadence, 11544597 [ms] = PT3H12M24.597S, occurred for 75.0000% of the 30 timesteps. 

Flux Distribution Map (from Master/CDFglobalAttributes/Data_type)

IBEX-Lo Release 4; Compton-Getting, Survival-Probability, ANTIRAM direction, 3-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (3-year-average of 6-month-cadence maps) IBEX-Lo map data for the first s3 years, 2009-2012, in the form of fluxes with correction for spacecraft motion (cg) (Compton-Getting) and with applied ENA survival probability correction (sp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, are located in the original ascii files in the map_wake folder, includes pixel map data, CG, SP, 3 year cadence. 

Signal/Noise Ratio, IBEX-Lo Energy Channel 1 ~0.015 keV - mapped

Signal/Noise Ratio, IBEX-Lo Energy Channel 2 ~0.029 keV - mapped

Signal/Noise Ratio, IBEX-Lo Energy Channel 3 ~0.055 keV - mapped

Signal/Noise Ratio, IBEX-Lo Energy Channel 5 ~0.209 keV - mapped

Signal/Noise Ratio, IBEX-Lo Energy Channel 6 ~0.439 keV - mapped

Signal/Noise Ratio, IBEX-Lo Energy Channel 7 ~0.872 keV - mapped

Signal/Noise Ratio, IBEX-Lo Energy Channel 8 ~1.821 keV - mapped

IBEX-Lo Release 4; Compton-Getting, Survival-Probability, RAM-directional 3-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 4 (3-year-average of 6-month-cadence maps) IBEX-Lo map data for the first s3 years, 2009-2012, in the form of ramdirectional fluxes with correction for spacecraft motion (cg) (Compton-Getting) and with applied ENA survival probability correction (sp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files in the map_ram folder, includes pixel map data from ram direction (ramdirectional), CG, SP, 3 year cadence. 

This data set is from the IBEX-Lo Release 6 Primary Hydrogen Data Rate Files. The IBEX sixth data release contains data and related information connected with the publication of Schwadron et al., 2014, SOLAR RADIATION PRESSURE AND LOCAL INTERSTELLAR MEDIUM FLOW PARAMETERS FROM INTERSTELLAR BOUNDARY EXPLORER LOW ENERGY HYDROGEN MEASUREMENTS. Neutral hydrogen atoms that travel into the heliosphere from the local interstellar medium (LISM) experience strong effects due to charge exchange and radiation pressure from resonant absorption and re-emission of Lya. The radiation pressure roughly compensates for the solar gravity. As a result, interstellar hydrogen atoms move along trajectories that are quite different than those of heavier interstellar species such as helium and oxygen, which experience relatively weak radiation pressure. Charge exchange leads to the loss of primary neutrals from the LISM and the addition of new secondary neutrals from the heliosheath. IBEX observations show clear effects of radiation pressure in a large longitudinal shift in the peak of interstellar hydrogen compared with that of interstellar helium. Here, we compare results from the Lee et al. interstellar neutral model with IBEX-Lo hydrogen observations to describe the distribution of hydrogen near 1 AU and provide new estimates of the solar radiation pressure. We find over the period analyzed from 2009 to 2011 that radiation pressure divided by the gravitational force (.) has increased slightly from mu = 0.94 +- 0.04 in 2009 to mu = 1.01 +- 0.05 in 2011. We have also derived the speed, temperature, source longitude, and latitude of the neutral H atoms and find that these parameters are roughly consistent with those of interstellar He, particularly when considering the filtration effects that act on H in the outer heliosheath. Thus, our analysis shows that over the period from 2009 to 2011, we observe signatures of neutral H consistent with the primary distribution of atoms from the LISM and a radiation pressure that increases in the early rise of solar activity. Data rate files are listed by orbit number: o00XX-rate12.txt where XX corresponds to the orbit number. The data rate files contain five data columns correspond to: isector, rate (ESA1), uncertainty(ESA1), rate(ESA2), uncertainty (ESA2). All rates in counts/sec. The methods used to estimate these background-corrected count rates are discussed by Schwadron et al. (2013). Because of background correction some of the listed rates are negative, but these are typically negative values near 0 within statistical uncertainties. isector: 0 - 30 isector corresponds to the spin-sector of the IBEX-Hi sensor The spinning spacecraft moves the sensors from 0 to 360 in a great-circle where the spin-axis is directed with RA and DEC coordinates given in the inertial pointing file. Sector 0 corresponds to the spin sector whose center in spin angle points exactly to the North Ecliptic Pole (NEP). hi-spinphase (deg) = isector*6.0 lo-spinphase (deg) = hi-spinphase +/- 180.0 In the current compilation, the time periods have been sub-divided into 512-spin time periods and thus synchronized with the internal accumulation periods of the onboard Histograms reported here and with the prescribed 512-spin accumulation. Therefore, some of the periods have slightly different start times and truncated to match the last complete 512-spin period at the end. Orbit 13 was omitted from the current compilation because several data gaps due to still ongoing commanding during that orbit cut into the prescribed 512 spin cadence. Also, in Data Release 3, the start and end times were slightly different from Table 1 to match the cadence chosen for the data. As used in the 2012 ApJ Suppl publications, Golden Triple Hydrogen counts detected in IBEX-Lo energy step 2 in 6o resolution are reported, which reflect H sputtered off the IBEX-Lo conversion surface by incoming interstellar He, as described in Moebius et al. (2012). The data rate files are organized as follows: The first line in the header contains column labels for 6 data columns, as listed below The next header line includes the start time (in GPS), end time (in GPS), and accumulated time (in seconds). This line is repeated for each 512-spin time period.For the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~7.5 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 7.5 apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b'. Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV).

The IBEX Release 6 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

ENA Count Rate Distribution (from Master/CDFglobalAttributes/Data_type)

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the IBEX-Lo Release 6 He Data (Sputtered H) Counts.. Data files are listed by orbit number: IBEX_Lo_o00XX_Y_HB_and_DE_report.csv where XX corresponds to the orbit number and Y to the sequence number of separately listed time periods in the respective orbit. The format in the file is listed below. The data are given accumulated over 512 spins each (. 2 hours) in time blocks separated by dashed lines. Provided are the data for Good Times of Angular Distributions. given in Table 1 of Moebius et al. (2012, ApJ Suppl, 198, 11, doi:10.1088/0067-0049/198/2/11). The description of the data selection is found in the file Moebius_etal_2012-ApJ-Suppl_Data-Description.pdf. These data were released as aggregate data for the entire time periods listed along with the publication of the 2012 ApJ Suppl publications. See IBEX Data Release 3: http://ibex.swri.edu/researchers/publicdata.shtml#dr3 In the current compilation, the time periods have been sub-divided into 512-spin time periods and thus synchronized with the internal accumulation periods of the onboard Histograms reported here and with the prescribed 512-spin accumulation. Therefore, some of the periods have slightly different start times and truncated to match the last complete 512-spin period at the end. Orbit 13 was omitted from the current compilation because several data gaps due to still ongoing commanding during that orbit cut into the prescribed 512 spin cadence. Also, in Data Release 3, the start and end times were slightly different from Table 1 to match the cadence chosen for the data. As used in the 2012 ApJ Suppl publications, Golden Triple Hydrogen counts detected in IBEX-Lo energy step 2 in 6o resolution are reported, which reflect H sputtered off the IBEX-Lo conversion surface by incoming interstellar He, as described in Moebius et al. (2012). The data rate files are organized as follows: The first line in the header contains column labels for 6 data columns, as listed below The next header line includes the start time (in GPS), end time (in GPS), and accumulated time (in seconds). This line is repeated for each 512-spin time period. Column 1 : The center of each 6 degree angular bin in NEP as calculated using the phase in the HB file. 0 . 354 Degrees corresponds to the spin-angle counted from the North Ecliptic Pole (NEP). The spinning spacecraft moves both sensors from 0 to 360 in a great-circle where the spin-axis is directed with RA and DEC coordinates given in the inertial pointing file. Spin angle 0 corresponds to the spin sector whose center in spin angle points exactly to the North Ecliptic Pole(NEP). RA and DEC refer here to solar Ecliptic east longitude and latitude. Column 2 : Start time of the 512 spin bin in GPS Column 3 : Start time of the 512 spin bin in YYYY/MM:DD:HH:MM:SS format Column 4 : Counts in the Hydrogen histogram bins (HB-Counts) Column 5 : Same as column 1 except this was determined from the DE file, here as a check to make sure there were no missing bins in the HB file Column 6 : Counts listed as GOLDEN HYDROGEN in the direct events (DE_Counts) Note: The HB_Counts are used in the analysis to normalized DE_Counts for digital buffer and telemetry limitations during high count rate time periods, as they occur during the interstellar flow observations. Usually, HB_Counts = DE_Counts. However, during times when the count rates do not exceed the telemetry capability or not by much, occasionally DE_Counts > HB_Counts due to the finite digital angular binning by time increments of 4.1 ms, equivalent to . 0.075o in spin angle, which can lead to different binning in DE and HB at the boundaries of the 6o angular bins. Still, the HB_Count normalization should be used. The related angular uncertainty of the accumulated counts is =0.075o and thus smaller than the overall pointing accuracy as reported by Hlond et al. (2012, ApJ Suppl, 198, 9, doi:10.1088/0067-0049/198/2/9)For the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~7.5 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 7.5 apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b'. Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release06/ena_lo_r06_schwadron-he/ibex_h3_ena_lo_r06_schwadron-he_20090121_orbit0014_v01.cdf. The most common cadence, 7378000 [ms] = PT2H2M58S, occurred for 70.0000% of the 14 timesteps. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the IBEX-Lo Release 6  State Vectors Data files are listed by orbit number: ibex-state-gse.txtFor the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~7.5 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 7.5 apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b'. Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release06/ena_lo_r06_state_vectors/ibex_h3_ena_lo_r06_state_vectors_20090101_v01.cdf. The most common cadence, 7200000 [ms] = PT2H, occurred for all 13139 timesteps. 

Energetic Neutral Atom Count Rate Distribution (from Master/CDFglobalAttributes/Data_type)

IBEX-Lo Release-07; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 7 (6 months-cadence) IBEX-Lo map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes with no corrections (nocg) for spacecraft motion (Compton-Getting) and no ENA survival probability (nosp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.110, 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_mapN for N=1,10, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

Sequential number 1 - 10 for six-month maps from IBEX Data Release 7

IBEX-Lo Release 7; no Compton-Getting, no Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Var Energy SC Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Lo map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with noCompton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction (nosp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 3-8 in numerical data form. Energy channels 3-8 have FWHM ranges with the corresponding center-point energies respectively 0.055, 0.110, 0.209, 0.439, 0.872, 1.821 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_map_1to10combinedVarEnergySCFrame are pixel map data from all directions (omnidirectional) in Var Energy SC Frame, no CG, no SP, 5 year cadence. 

IBEX Data Release-7, IBEX-Lo 10 map average maps in ascii list and image formats

IBEX-Lo Release-07; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 7 (6 months-cadence) IBEX-Lo map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes with no corrections (nocg) for spacecraft motion (Compton-Getting) and with ENA survival probability (sp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.110, 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_mapN for N=1,10, includes pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Lo Release 7; no Compton-Getting, Survival-Probability, Omnidirectional 1-to-10-map Average West Ecliptic Maps in Var Energy SC Frame

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 7 (1-to-10-map-average) IBEX-Lo map data for the years 2009-2014 in the form of omnidirectional ENA (hydrogen) fluxes with noCompton-Getting correction (nocg) of flux spectra for spacecraft  motion and correction (sp) for ENA survival probability in Var Energy SC Frame between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 3-8 in numerical data form. Energy channels 3-8 have FWHM ranges with the corresponding center-point energies respectively 0.055, 0.110, 0.209, 0.439, 0.872, 1.821 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mif = Mono Inertial Frame veif = Var Energy Inertial Frame vescf = Var Energy SC Frame 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the original ascii files as hvset_map_1to10combinedVarEnergySCFrame are pixel map data from all directions (omnidirectional) in Var Energy SC Frame, no CG, SP, 5 year cadence. 

IBEX-Lo Release-08; omni-direction 5-year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Lo map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes between 1 and 100 AU. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f2-ribbonMapsGAL includes f2 ribbon pixel map data from all directions (omnidirectional), 5 year cadence. 

IBEX Data Release 8, IBEX-Lo five-year GA in ascii list and image formats

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Lo map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes between 1 and 100 AU. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f2-ribbonMapsJ2000 includes f2 ribbon pixel map data from all directions (omnidirectional), 5 year cadence. 

IBEX Data Release 8, IBEX-Lo five-year maps in ascii list and image formats

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Lo map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional ENA (hydrogen) fluxes between 1 and 100 AU. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f2-ribbonMaps includes f2 ribbon pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Lo map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional GDF (Globally Distributed Flux) ENA (hydrogen) fluxes between 1 and 100 AU. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. gdf = Globally Distributed Flux. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f3-gdfGALACTIC includes f3 GDF (Globally Distributed Flux) pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Lo map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional GDF (Globally Distributed Flux) ENA (hydrogen) fluxes between 1 and 100 AU. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. gdf = Globally Distributed Flux. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f3-gdfJ2000 includes f3 GDF (Globally Distributed Flux) pixel map data from all directions (omnidirectional), 5 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 8 IBEX-Lo map data for the years 2009-2014 (5 year-cadence) in the form of omnidirectional GDF (Globally Distributed Flux) ENA (hydrogen) fluxes between 1 and 100 AU. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. gdf = Globally Distributed Flux. 7. The following list associates Release 16 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: This particular data set, denoted in the f3-gdfMaps includes f3 GDF (Globally Distributed Flux) pixel map data from all directions (omnidirectional), 5 year cadence. 

IBEX Release-9; IBEX-Lo Interstellar Neutral Histogram Counts and Direct Event Counts

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: IBEX-Lo Interstellar Neutral Histogram Counts and Direct Event CountsData description: Interstellar neutral (ISN) histogram and direct event counts for each of the 60 IBEX-Lo angular bins. The data includes start and end times for each 512 spin period in GPS time as well as total accumulation times. Data files are in CSV format and are labelled according to their IBEX orbit and orbit arc. Data are collected for periods within the ISN goodtimes. The analyses of the IBEX He and H ISN flow distributions within this release are based on these data sets.1. Golden triples2. Hydrogen time-of-flight3. Energy Steps 1-3 are included during non-special mode periods.ISN data product QA checks: All ISN season orbits are checked for contaminating backgrounds around the ISN peak itself. Times with high backgrounds are eliminated.Background threshold for this test is determined orbit by orbit using sample quiet times. Times when the TOF 2 rate exceeds this background by 60% are excluded.Times with spin issues are excludedTimes with special operations are excluded (gain tests, etc.)Remaining times are included in ISN data products and the resulting ISN data products are checked for continuity (time and angle), and suppression (loss of direct events due to instrument throttling). 3: Reference: Schwadron et al. 2016, ApJ, 828:81, Determination of Interstellar O Parameters Using the First Two Years of Data from the Interstellar Boundary Explorer. 4: Data Location: https://ibex.princeton.edu/DataRelease 6: Orbit Start and End Times: 7: 23: 2009-03-26 21:09:00.318 to 2009-04-03 16:07:51.743 8:  24: 2009-04-03 12:10:21.253 to 2009-04-11 08:15:09.669 9:  25: 2009-04-11 05:06:40.967 to 2009-04-18 22:05:11.125 10:  27: 2009-04-26 08:27:40.916 to 2009-05-04 05:31:06.519 11:  28: 2009-05-04 02:02:57.673 to 2009-05-11 21:13:47.596 12:  29: 2009-05-11 17:27:02.484 to 2009-05-19 19:27:18.831 13:  51: 2009-10-26 08:19:34.905 to 2009-11-03 02:38:01.730 14:  52: 2009-11-02 22:34:07.792 to 2009-11-10 19:03:55.230 15:  53: 2009-11-10 15:46:22.161 to 2009-11-18 10:58:17.674 16:  55: 2009-11-25 23:44:19.069 to 2009-12-03 11:26:37.151 17:  56: 2009-12-03 08:22:31.792 to 2009-12-10 22:03:52.604 18:  57: 2009-12-10 18:55:33.969 to 2009-12-18 06:58:47.247  19:  72: 2010-04-04 11:17:28.386 to 2010-04-12 09:13:51.008 20:  74: 2010-04-19 14:09:01.851 to 2010-04-27 03:44:14.913 21:  77: 2010-05-12 01:33:51.796 to 2010-05-19 20:43:01.583 22:  78: 2010-05-19 17:33:48.047 to 2010-05-27 13:02:03.396 23:  103: 2010-11-26 07:56:05.324 to 2010-12-04 04:11:44.879 24:  187a: 2012-11-21 00:17:13.430 to 2012-11-25 00:40:26.707 25:  188b: 2012-12-03 12:46:18.859 to 2012-12-08 00:44:50.846 26:  206a: 2013-05-13 23:15:27.433 to 2013-05-17 12:19:58.215 27:  207b: 2013-05-26 12:21:08.868 to 2013-05-30 23:14:44.98928: For the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~7.5 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 7.5 degree apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b.' Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV). 

Please acknowledge the IBEX Mission Principal Investigator Dr. David J McComas of Princeton University

IBEX Release 09; Hydrogen count rates for different spin phase bins organized by orbit

Determination of Interstellar H Parameters Using the Data from the Interstellar Boundary Explorer

The IBEX Release 9 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release09/ena_lo_heirtzler-h_7day/ibex_h3_ena_lo_r09_heirtzler-h_7day_20081225_orb011_v01.cdf. The most common cadence, 7379000 [ms] = PT2H2M59S, occurred for 63.4615% of the 33 timesteps. 

IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral  maps: m1-to-m6 (map1 + map2 + map3 + map4 + map5 + map6) West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2008-2017. 2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo Heavy Neutral Maps data for combination and averaging of six-month maps 1-6 into three-year maps for each energy channel during 2008-2011 in the form of counting rates and supporting parameters. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles from the measured direct events identified as 'Oxygen', which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns (Park et al. 2015). Because there are no sputtering, corrections, the 'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps are produced by Pipeline code. There are energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from this part ofRelease 9 are given in the following journal publication:4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October. http://dx.doi.org/10.1088/0067-0049/220/2/34 5. The following list associates Release 9 map numbers (1-6) with mission year (1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20116: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV7: This particular data set, denoted in the original ascii files as comb-ot-m1m6 includes combined IBEX-Lo heavy neutral pixel maps data (map1 + map2 + map3 + map4 + map5 + map6) from all directions 

IBEX Data Release-9, Park et al. (2015) IBEX-Lo combined even six-month maps in ascii list and image formats

Sequential number 1 - 6 for six-month maps from IBEX Data Release 9

O ENA Total Exposure Time at Lo Energy Channel 5 ~0.209 keV - mapped

Standard deviation of count rate at Lo Energy Channel 5 ~0.209 keV - mapped

O ENA Total Exposure Time at Energy Channel 6 ~0.439 keV - mapped

O ENA Signal/Noise Ratio at Lo Energy Channel 6 ~0.439 keV - mapped

Standard deviation of count rate at Lo Energy Channel 6 ~0.439 keV - mapped

O ENA Total Exposure Time at Energy Channel 7 ~0.872 keV - mapped

O ENA Signal/Noise Ratio at Lo Energy Channel 7 ~0.872 keV - mapped

Standard deviation of count rate at Energy Channel 7 ~0.872 keV - mapped

O ENA Total Exposure Time at Energy Channel 8 ~1.821 keV - mapped

O ENA Signal/Noise Ratio at Lo Energy Channel 8 ~1.821 keV - mapped

Standard deviation of count rate at Energy Channel 8 ~1.821 keV - mapped

IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral even maps: m2m4m6 (map2 + map4 + map6) West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2008-2017. 2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo Heavy Neutral Maps (6 months-cadence) data from combined even maps (2,4,6) during 2009-2011 in the form of counting rates and supporting parameters. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles from the measured direct events identified as 'Oxygen', which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns (Park et al. 2015). Because there are no sputtering, corrections, the 'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps are produced by Pipeline code. There are energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from this part ofRelease 9 are given in the following journal publication:4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October. http://dx.doi.org/10.1088/0067-0049/220/2/34 4. The following list associates Release 9 map numbers (1-6) with mission year (1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20115: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV6: This particular data set, denoted in the original ascii files as comb-ot-m2m4m6 includes combined IBEX-Lo heavy neutral pixel even maps data (map2 + map4 + map6) from all directions 

O ENA Total Exposure Time at IBEX-Lo Energy Channel 5 ~0.209 keV - mapped

O ENA Signal/Noise Ratio at IBEX-Lo Energy Channel 5 ~0.209 keV - mapped

O ENA count rate at IBEX-Lo Energy Channel 5 ~0.209 keV - mapped

Standard deviation of count rate at IBEX-Lo Energy Channel 5 ~0.209 keV - mapped

O ENA Total Exposure Time at Energy Channel 6, Center Energy 0.439 keV - mapped

O ENA Signal/Noise Ratio at IBEX-Lo Energy Channel 6, Center Energy 0.439 keV - mapped

Standard deviation of count rate Energy Channel 6, Center Energy 0.439 keV; the energy resolution is delta-E/E = 0.8 for all channels.

O ENA Total Exposure Time (seconds) at Energy Channel 7, Center Energy 0.872 keV; the energy resolution is delta-E/E = 0.8 for all channels.

O ENA Signal/Noise Ratio at IBEX-Lo Energy Channel 7 ~0.872 keV  - mapped

Standard deviation of count rate Energy Channel 7 ~0.872 keV - mapped

O ENA Signal/Noise Ratio at IBEX-Lo Energy Channel 8 ~1.821 keV - mapped

Standard deviation of count rate Energy Channel 8, ~1.821 keV - mapped

IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral odd maps: m1m3m5 (map1 + map3 + map5) West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo Heavy Neutral Maps (6 months-cadence) data from combined odd maps (1,3,5) during 2008-2011 in the form of counting rates and supporting parameters. 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles from the measured direct events identified as 'Oxygen', which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns (Park et al. 2015). Because there are no sputtering, corrections, the 'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps are produced by Pipeline code. There are energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from this part ofRelease 9 are given in the following journal publication:4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October. http://dx.doi.org/10.1088/0067-0049/220/2/34 5. The following list associates Release 9 map numbers (1-6) with mission year (1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20116: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV7: This particular data set, denoted in the original ascii files as comb-ot-m1m3m5 includes combined IBEX-Lo heavy neutral pixel odd maps data (map1 + map3 + map5) from all directions 

IBEX Data Release-9, Park et al. (2015) IBEX-Lo combined odd six-month maps in ascii list and image formats

IBEX-Lo Release-09; Park Oxygen Map Counting Rate 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Park et al. (2015) subset of the Release 9 The IBEX-Lo Heavy Neutral Maps (6 months-cadence) data in the form of direct event counts, counting rates and other supporting data3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles from the measured direct events identified as 'Oxygen', which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns (Park et al. 2015). Because there are no sputtering corrections, the 'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps are produced by Pipeline code. There are energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 9 are given in the following journal publication: 4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October. http://dx.doi.org/10.1088/0067-0049/220/2/34 5. The following list associates Release 9 map numbers (1-6) with mission year (1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20118: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV6: This particular data set, denoted in the original ascii files as lvset_o_mapN for N=1,6, includes pixel map data from all directions at 6 month cadence. 

IBEX Data Release-9, IBEX-Lo six-month maps in ascii list and image formats

O ENA Total Counts at IBEX-Lo Energy Channel 5 ~0.209 keV - mapped

O ENA Total Counts at IBEX-Lo Energy Channel 6 ~0.439 keV - mapped

O ENA Total Counts at IBEX-Lo Energy Channel 7 ~0.872 keV - mapped

O ENA Total Counts (#) at IBEX-Lo Energy Channel 8, Center Energy 1.821 keV; the energy resolution is delta-E/E = 0.8 for all channels.  - mapped

IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral maps: m1-to-m6 (map1 + map2 + map3 + map4 + map5 + map6) with statistical filtering

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2008-2017. 2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo Heavy Neutral Maps, mostly of oxygen, averaged over three years, 2008-2011, from IBEX-Lo maps 1 ... 6. There are four types of maps derived from different statistical filtering approaches: signal/noise filtering, confidence limit method (CLM), cluster analysis method (CLM), and CLUSTER with signal/noise filtering, all as described in Park et al. (2015). Map data for the first two approaches are in counts/second and for the last two in counts/hour (Cluster ID). 3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles from the measured direct events identified as 'Oxygen', which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns (Park et al. 2015). Because there are no sputtering, corrections, the 'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps are produced by Pipeline code. There are energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from this part of Release 9 are given in the following journal publication:4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October. http://dx.doi.org/10.1088/0067-0049/220/2/34 5. The following list associates Release 9 map numbers (1-6) with mission year (1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/20116: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV7: This particular data set, denoted in the original ascii files as comb-ot-m1m6 includes combined IBEX-Lo heavy neutral pixel maps data (map1 + map2 + map3 + map4 + map5 + map6)  for counting rates from all directions 

IBEX Data Release-9, Park et al. (2015) IBEX-Lo combined maps in ascii list and image formats

O ENA Total CLM-filtered count rate, Lo Energy Ch.5 ~0.209 keV - mapped

O ENA Total CLM-filtered count rate, Energy Ch.7 ~0.872 keV - mapped

O ENA Total CLM-filtered count rate, Energy Ch.8 ~1.821 keV - mapped

O ENA Signal/Noise-filtered count rate, Lo Energy Ch.5 ~0.209 keV - mapped

O ENA Signal/Noise-filtered Count Rate, Lo Energy Ch.6 ~0.439 keV - mapped

O ENA Signal/Noise-filtered Count Rate, Lo Energy Ch.7 ~0.872 keV - mapped

O ENA Signal/Noise-filtered Count Rate, Lo Energy Ch.8 ~1.821 keV - mapped

O ENA count rate filtered by s/n ratio and confidence level method, Lo Energy Ch.5 ~0.209 keV - mapped

O ENA count rate filtered by s/n ratio and confidence level method, Energy Ch.6 ~0.439 keV - mapped

O ENA count rate filtered by s/n ratio and confidence level method, Energy Ch.7 ~0.872 keV - mapped

O ENA count rate filtered by s/n ratio and confidence level method, Lo Energy Ch.8 ~1.821 - mapped

Cluster-filtered count rate at Lo Energy Ch.5 ~0.209 keV - mapped

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the IBEX Release 9: Interstellar He Parameters. 3: Reference: Schwadron et al. Schwadron et al. 2015, ApJS Special Issue, Determination of Interstellar He Parameters using 5 years of data from the Interstellar Boundary Explorer beyond closed form approximations. 4: Data Location: http://ibex.swri.edu/ibexpublicdata/Data_Release_9/schwadronData.html5: Contact: Nathan Schwadron, University of New Hampshire, Durham, NH nschwadron@unh.edu6: Orbit Start and End Times: 7: 23: 2009-03-26 21:09:00.318 to 2009-04-03 16:07:51.743 8:  24: 2009-04-03 12:10:21.253 to 2009-04-11 08:15:09.669 9:  25: 2009-04-11 05:06:40.967 to 2009-04-18 22:05:11.125 10:  27: 2009-04-26 08:27:40.916 to 2009-05-04 05:31:06.519 11:  28: 2009-05-04 02:02:57.673 to 2009-05-11 21:13:47.596 12:  29: 2009-05-11 17:27:02.484 to 2009-05-19 19:27:18.831 13:  51: 2009-10-26 08:19:34.905 to 2009-11-03 02:38:01.730 14:  52: 2009-11-02 22:34:07.792 to 2009-11-10 19:03:55.230 15:  53: 2009-11-10 15:46:22.161 to 2009-11-18 10:58:17.674 16:  55: 2009-11-25 23:44:19.069 to 2009-12-03 11:26:37.151 17:  56: 2009-12-03 08:22:31.792 to 2009-12-10 22:03:52.604 18:  57: 2009-12-10 18:55:33.969 to 2009-12-18 06:58:47.247  19:  72: 2010-04-04 11:17:28.386 to 2010-04-12 09:13:51.008 20:  74: 2010-04-19 14:09:01.851 to 2010-04-27 03:44:14.913 21:  77: 2010-05-12 01:33:51.796 to 2010-05-19 20:43:01.583 22:  78: 2010-05-19 17:33:48.047 to 2010-05-27 13:02:03.396 23:  103: 2010-11-26 07:56:05.324 to 2010-12-04 04:11:44.879 24:  187a: 2012-11-21 00:17:13.430 to 2012-11-25 00:40:26.707 25:  188b: 2012-12-03 12:46:18.859 to 2012-12-08 00:44:50.846 26:  206a: 2013-05-13 23:15:27.433 to 2013-05-17 12:19:58.215 27:  207b: 2013-05-26 12:21:08.868 to 2013-05-30 23:14:44.98928: For the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~9.1 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 9.1 degree apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b.' Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV). 29: Interstellar He represents a key sample of interstellar matter that, due to its high first ionization potential, survives the journey from beyond our solar system's heliospheric boundaries to Earth. Ongoing analysis of interstellar neutral (ISN) He atoms by the Interstellar Boundary Explorer (IBEX) has resulted in a growing sophistication in our understanding of local interstellar flow. A key feature of the IBEX observations near perihelion of the ISN trajectories is a narrow 'tube' of approximately degenerate interstellar parameters. These degenerate solutions provide a tightly coupled relationship between interstellar flow longitude and latitude, speed, and temperature. However, IBEX analysis resulting in a specific solution for inflow longitude, inflow speed, temperature and inflow latitude was accompanied with a sizeable uncertainty along the parameter tube. Here, we use the three-step method to find the interstellar parameters: 1) the ISN He peak rate in ecliptic longitude determines uniquely a relation (as part of the tube in parameter space) between the longitude lambda-ISN-8 and the speed VISN-8 of the He ISN flow at infinity; 2) the ISN He peak latitude (on the great circle swept out in each spin) is compared to simulations to derive unique values for lambda-ISN-8 and VISN-8 along the parameter tube; 3) the angular width of the He flow distributions as a function of latitude is used to derive the interstellar He temperature. For simulated peak latitudes, we use a relatively new analytical tool that traces He atoms from beyond the termination shock into the position of IBEX and incorporates the detailed response function of IBEX-Lo. By varying interstellar parameters along the IBEX parameter tube, we find the specific parameters that minimize the chi-square difference between observations and simulations. The new computational tool for simulating neutral atoms through the integrated IBEX-Lo response function makes no assumptions or expansions with respect to spin axis pointing or frame of reference. Thus, we are capable of moving beyond closed form approximations and utilize observations of interstellar He during the complete 5 year period from 2009 to 2013 when the primary component of interstellar He is most prominent. Chi-square minimization of simulations compared to observations results in a He ISN flow longitude 75.6 degrees +-1.40 degrees, latitude -5.12 degrees +-0.27 degrees , speed 25.4 +-1.1 km/s, and temperature 8000 +-1300 K, where the uncertainties are related and apply along the IBEX parameter tube. This paper also provides documentation for a new release of ISN data and associated model runs'IBEX data used in the Schwadron et al. 2015 analysis to compute interstellar He parameters. Data are included for each position along the parameter tube as defined by the inflow speed. The inflow speed is given by the filename (i.e. runex-22.888889.txt means 22.9 km/s inflow speed).

IBEX Release-9; Determination of Interstellar He Parameters using 5 years of data from the Interstellar Boundary Explorer beyond closed form approximations

SPDF/CDAWeb. Please also acknowledge the data producer: David McComas at Princeton University

SPDF/SSCWeb. Please also acknowledge the data producer: David McComas at Princeton University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David McComas at Princeton University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release09/ena_lo_schwadron-interstellar-he_1yr/ibex_h3_ena_lo_r09_schwadron-interstellar-he_1yr_20090120_v01.cdf. The most common cadence, 31224000 [ms] = PT8H40M24S, occurred for 10.7143% of the 3 timesteps. 

IBEX-Lo Release-10; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (6 months-cadence) IBEX-Lo map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes without any corrections (nocg) for spacecraft motion (Compton-Getting) and ENA survival probability (nosp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_mapN for N=1,14, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence. 

IBEX-Lo Release-10; no Compton-Getting, no Survival-Probability, Omnidirectional 7-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (7-year-average of 6-month-cadence maps) IBEX-Lo map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes without any corrections for spacecraft motion (nocg) (Compton-Getting) and with no applied ENA survival probability correction (nosp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_single, includes pixel map data from all directions (omnidirectional), no CG, SP, 7 year cadence. 

IBEX-Lo Release-10; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (6 months-cadence) IBEX-Lo map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes without any corrections for spacecraft motion (nocg) (Compton-Getting) but with the applied ENA survival probability correction (sp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_tabular_mapN for N=1,14, includes pixel map data from all directions (omnidirectional), no CG, SP, 6 month cadence. 

IBEX-Lo Release-10; no Compton-Getting, Survival-Probability, Omnidirectional 7-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 15 releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 2: This data set is from the Release 10 (7-year-average of 6-month-cadence maps) IBEX-Lo map data for the first seven years, 2009-2015, in the form of omnidirectional fluxes without any corrections for spacecraft motion (nocg) (Compton-Getting) but with the applied ENA survival probability correction (sp) between 1 and 100 AU.3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in numerical data form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled science from Release 10 are given in the following journal publication:4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146: 117...147; DOI 10.1007/s11214-009-9495-85: https://link.springer.com/article/10.1007/s11214-009-9495-86. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 10 map numbers (1-14) with mission year (1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/20158: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_tabular_single, includes pixel map data from all directions (omnidirectional), no CG, SP, 7 year cadence. 

IBEX Release-11; Oxygen count rates for different spin phase bins organized by orbit

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the IBEX Release 11: Oxygen count rates for different spin phase bins organized by selected orbits in years 2009 and 2010.3: Reference: Schwadron et al. 2016, ApJ, 828:81, Determination of Interstellar O Parameters Using the First Two Years of Data from the Interstellar Boundary Explorer. 4: Data Location: http://ibex.swri.edu/ibexpublicdata/Data_Release_11/schwadronData.html5: Contact: Nathan Schwadron, University of New Hampshire, Durham, NH (nschwadron@unh.edu)6: Orbit Start and End Times: 7: 23: 2009-03-26 21:09:00.318 to 2009-04-03 16:07:51.743 8:  24: 2009-04-03 12:10:21.253 to 2009-04-11 08:15:09.669 9:  25: 2009-04-11 05:06:40.967 to 2009-04-18 22:05:11.125 10:  27: 2009-04-26 08:27:40.916 to 2009-05-04 05:31:06.519 11:  28: 2009-05-04 02:02:57.673 to 2009-05-11 21:13:47.596 12:  29: 2009-05-11 17:27:02.484 to 2009-05-19 19:27:18.831 13:  51: 2009-10-26 08:19:34.905 to 2009-11-03 02:38:01.730 14:  52: 2009-11-02 22:34:07.792 to 2009-11-10 19:03:55.230 15:  53: 2009-11-10 15:46:22.161 to 2009-11-18 10:58:17.674 16:  55: 2009-11-25 23:44:19.069 to 2009-12-03 11:26:37.151 17:  56: 2009-12-03 08:22:31.792 to 2009-12-10 22:03:52.604 18:  57: 2009-12-10 18:55:33.969 to 2009-12-18 06:58:47.247  19:  72: 2010-04-04 11:17:28.386 to 2010-04-12 09:13:51.008 20:  74: 2010-04-19 14:09:01.851 to 2010-04-27 03:44:14.913 21:  77: 2010-05-12 01:33:51.796 to 2010-05-19 20:43:01.583 22:  78: 2010-05-19 17:33:48.047 to 2010-05-27 13:02:03.396 23:  103: 2010-11-26 07:56:05.324 to 2010-12-04 04:11:44.879 24:  187a: 2012-11-21 00:17:13.430 to 2012-11-25 00:40:26.707 25:  188b: 2012-12-03 12:46:18.859 to 2012-12-08 00:44:50.846 26:  206a: 2013-05-13 23:15:27.433 to 2013-05-17 12:19:58.215 27:  207b: 2013-05-26 12:21:08.868 to 2013-05-30 23:14:44.98928: For the first two and a half years of science operations (through Orbit 127), IBEX's orbital period was ~7.5 days and the spin axis was repointed once each orbit (around perigee), leading to bands of sky viewing centered 7.5 degree apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE (McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days (one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130 onward are split into two segments, 'a' and 'b.' Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step (ESA1) in exchange for doubling the statistical sampling of ESA3 (center energy ~1.1 keV). 

Please acknowledge the IBEX Mission Principal Investigator Dr. David J McComas of Southwest Research Institute, San Antonio, TX, and Dr. Nathan Schwadron, University of New Hampshire, Durham, NH

Determination of Interstellar O Parameters Using the First Two Years of Data from the Interstellar Boundary Explorer

The IBEX Release 11 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

SPDF/CDAWeb. Please also acknowledge the data producer: David McComas at Southwest Research Institute, San Antonio, TX

SPDF/SSCWeb. Please also acknowledge the data producer: David McComas at Southwest Research Institute, San Antonio, TX

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David McComas at Southwest Research Institute, San Antonio, TX

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release11/ena_lo_schwadron-interstellar-o/ibex_h3_ena_lo_r11_schwadron-interstellar-o_20090121_v01.cdf. The most common cadence, 239075328 [ms] = P2DT18H24M35.328S, occurred for 1.6949% of the 1 timesteps. 

IBEX-lo Release 17; Compton-Getting, no Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_noSP_antiram_cg_hb_N for N=2009-2019, includes pixel map data from antiram direction,  CG, no SP, 1 year cadence. 

The IBEX Release 17 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

IBEX-lo Release 17; Compton-Getting, no Survival-Probability, OMNIdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of omni-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_cg_hb_N for N=2009-2019, includes pixel map data from all directions (omnidirectional), CG, no SP, 1 year cadence. 

IBEX-lo Release 17; Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_noSP_ram_cg_hb_N for N=2009-2019, includes pixel map data from ram direction,  CG, no SP, 1 year cadence. 

IBEX-lo Release 17; Compton-Getting, Survival-Probability, ANTIRAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of antiram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and with correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_tabular_antiram_cg_hb_N for N=2009-2019, includes pixel map data from antiram direction,  CG, SP, 1 year cadence. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of omni-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and with correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_tabular_cg_hb_N for N=2009-2019, includes pixel map data from all directions (omnidirectional), CG, SP, 1 year cadence. 

IBEX-lo Release 17; Compton-Getting, Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and with correction for ENA survival probability (sp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_tabular_cg_hb_N for N=2009-2019, includes pixel map data from ram direction,  CG, SP, 1 year cadence. 

IBEX-lo Release 17; no Compton-Getting, no Survival-Probability, RAMdirectional 1-Year-Average West Ecliptic Maps

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2019. 2: This data set is from the Release 17 (1 year-cadence) IBEX-Lo map data for the years 2009-2019 in the form of ram-directional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 1-8 in numerical data form. Energy channels 1-8 have FWHM center-point energies at 0.015, 0.029, 0.055, 0.11, 0.209, 0.439, 0.872, 1.821 keV, respectively. 4: Details of the data and enabled science from Release 10 are given in the following journal publication:  McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 5: http://doi.org/10.3847/1538-4365/aa66d8 6. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. noSP - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. 7. The following list associates Release 17 map numbers (1-22) with mission year (1-9), orbits (11-471b), and dates (12/25/2008-12/26/2019): Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: Map2012A, year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: Map2012B, year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: Map2013A, year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: Map2013B, year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: Map2014A, year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: Map2014B, year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: Map2015A, year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: Map2015B, year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: Map2016A, year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: Map2016B, year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: Map2017A, year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: Map2017B, year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: Map2018A, year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: Map2018B, year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: Map2019A, year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: Map2019B, year 11, orbits 452a-471b, dates 06/28/2019 . 12/26/20198: The energy resolution is delta-E/E = 0.8 for all channels:Energy channel 1: center energy = 0.015 keVEnergy channel 2: center energy = 0.029 keVEnergy channel 3: center energy = 0.055 keVEnergy channel 4: center energy = 0.11 keVEnergy channel 5: center energy = 0.209 keVEnergy channel 6: center energy = 0.439 keVEnergy channel 7: center energy = 0.872 keVEnergy channel 8: center energy = 1.821 keV9: This particular data set, denoted in the original ascii files as lvset_h_noSP_ram_nocg_hb_N for N=2009-2019, includes pixel map data from ram direction,  no CG, no SP, 1 year cadence. 

IBEX Data Release 5 - Mariner 10 Hydrogen Ly-alpha backscattered emision and Helium 584A backscattered solar emission from Roll Control Maneuver #7 of Mariner 10. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 16 releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 2: This data set is from the IBEX Data Release 5 - Mariner 10 Hydrogen Ly-alpha backscattered emision and Helium 584A backscattered solar emission from Roll Control Maneuver #7 of Mariner 10. Source of data:  Wayne Pryor <Wayne.Pryor@centralaz.edu> and Joe Ajello <joseph.m.ajello@jpl.nasa.gov> Main papers describing scientific results of data: a) Ajello, J.~M., An interpretation of Mariner 10 helium (584 A) and hydrogen (1216 A) interplanetary emission observations, Astrophysical Journal, vol. 222, pp 1068-1079, 1978 doi=10.1086/156224 b) Ajello, J.~M. and Witt, N. and Blum, P.~W., Four UV observations of the interstellar wind by Mariner 10 - Analysis with spherically symmetric solar radiation models, Astrophysical Journal, volume 73, pp260-271, 1979 

IBEX Data Release 5: Hydrogen Ly-alpha backscattered emission and Helium 584A backscattered solar emision from Roll Control Maneuver #7 of Mariner 10. XYZ location of spacecraft during observations in ecliptic coordinates and for the epoch of observation are: -0.500; 0.560; 0.030. See science papers above, and others by same authors

The IBEX Release 5 data are archived as fully citable data. Please consult IBEX team publications and personnel for further details on production, processing, and usage of these data. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release05/ena_r05_mariner-h-he/ibex_h3_ena_r05_mariner-h-he_19740128_v01.cdf. The most common cadence, 21000 [ms] = PT21S, occurred for all 663 timesteps. 

1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 18 releases of IBEX-HI and IBEX-LO data covering 2009-2022. 2: This data set is from the Release 18 (1 year-cadence) IBEX-Hi map data for the years 2009-2022 in the form of antiramdirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft  motion and no correction for ENA survival probability (nosp) between 1 and 100 AU. 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), http://doi.org/10.3847/1538-4365/aa66d8 5. The following codes are used to define dataset types:cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs. nocg = no Compton-Getting corrections sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular. nosp - no survival probability corrections have been applied to the data. omni = data from all directions. ram = data was collected when the spacecraft was ramming into the incoming ENAs. antiram = data was collected when the spacecraft was moving away from the incoming ENAs. mono = mono-energy Compton-Getting corrected maps. 6. The following list associates Release 18 map numbers (1-28) with mission year (1-14), orbits (11-592B), and dates (12/25/2008-12/26/2022): Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015Map 15: year 8, orbits 311a-330b, dates 12/24/2015 . 06/23/2016Map 16: year 8, orbits 331a-351a, dates 06/24/2016 . 12/26/2016Map 17: year 9, orbits 351b-371a, dates 12/26/2016 . 06/24/2017Map 18: year 9, orbits 371b-391a, dates 06/25/2017 . 12/25/2017Map 19: year 10, orbits 391b-411b, dates 12/25/2017 . 06/28/2018Map 20: year 10, orbits 412a-431b, dates 06/29/2018 . 12/26/2018Map 21: year 11, orbits 432a-451b, dates 12/27/2018 . 06/27/2019Map 22: year 11, orbits 452a-471b, dates 06/27/2019 . 12/26/2019Map 23: year 12, orbits 472a-491b, dates 12/26/2019 . 06/24/2020Map 24: year 12, orbits 492a-511b, dates 06/25/2020 . 12/24/2020Map 25: year 13, orbits 512a-531b, dates 12/24/2020 . 06/24/2021Map 26: year 13, orbits 532a-552b, dates 06/25/2021 . 12/27/2021Map 27: year 14, orbits 552a-572b, dates 12/27/2021 . 06/26/2022Map 28: year 14, orbits 572a-592b, dates 06/26/2022 . 12/26/20227: This particular data set, denoted in the original ascii files as stateinfo/oNNNNX.ibex_state_GSE.txt , where NNNN is an orbit number from 0011 to 0592 and X = 'a' or 'b' denotes the first or second half of the orbit for orbits, which number is bigger than 129, represents state vector, i.e. both position and velocity X, Y, and Z components. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/h3/release18/ena_r18_state_vector/ibex_h3_ena_r18_state_vector_20081225_orb0011_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 190 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ibex/ephemeris/ssc/2008/ibex_or_ssc_20080101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.9999% of the 1155896 timesteps. 

Michelson Interferometer for Global High-resolution Thermospheric Imaging (MIGHTI) Sensor A: Line-of-sight Wind Profiles

ICON explores the boundary between Earth and space - the ionosphere - to understand the physical connection between our world and the immediate space environment around us. Visit 'http://icon.ssl.berkeley.edu' for more details.

This is a data product from the NASA Ionospheric Connection Explorer mission, an Explorer launched at 21:59:45 EDT on October 10, 2019, from Cape Canaveral AFB in the USA. Guidelines for the use of this product are described in the ICON Rules of the Road  (http://icon.ssl.berkeley.edu/Data).  Responsibility for the mission science falls to the Principal Investigator, Dr. Thomas Immel at UC Berkeley:  Immel, T.J., England, S.L., Mende, S.B. et al. Space Sci Rev (2018) 214: 13. https://doi.org/10.1007/s11214-017-0449-2  Responsibility for the validation of the L1 data products falls to the instrument lead investigators/scientists.  * EUV: Dr. Eric Korpela :  https://doi.org/10.1007/s11214-017-0384-2  * FUV: Dr. Harald Frey : https://doi.org/10.1007/s11214-017-0386-0  * MIGHTI: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0358-4, and https://doi.org/10.1007/s11214-017-0374-4  * IVM: Dr. Roderick Heelis : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for the validation of the L2 data products falls to those scientists responsible for those products.  * Daytime O and N2 profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-018-0477-6  * Daytime (EUV) O+ profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-017-0385-1  * Nighttime (FUV) O+ profiles: Dr. Farzad Kamalabadi : https://doi.org/10.1007/s11214-018-0502-9  * Neutral Wind profiles: Dr. Jonathan Makela : https://doi.org/10.1007/s11214-017-0359-3  * Neutral Temperature profiles: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0434-9  * Ion Velocity Measurements : Dr. Russell Stoneback : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for Level 4 products falls to those scientists responsible for those products.  * Hough Modes : Dr. Chihoko Yamashita :  https://doi.org/10.1007/s11214-017-0401-5  * TIEGCM : Dr. Astrid Maute : https://doi.org/10.1007/s11214-017-0330-3  * SAMI3 : Dr. Joseph Huba : https://doi.org/10.1007/s11214-017-0415-z  Pre-production versions of all above papers are available on the ICON website.  http://icon.ssl.berkeley.edu/Publications  Overall validation of the products is overseen by the ICON Project Scientist, Dr. Scott England.  NASA oversight for all products is provided by the Mission Scientist, Dr. Jeffrey Klenzing.  Users of these data should contact and acknowledge the Principal Investigator Dr. Immel and the party directly responsible for the data product (noted above) and acknowledge NASA funding for the collection of the data used in the research with the following statement :  'ICON is supported by NASA's Explorers Program through contracts NNG12FA45C and NNG12FA42I'.  These data are openly available as described in the ICON Data Management Plan available on the ICON website (http://icon.ssl.berkeley.edu/Data). 

Michelson Interferometer for Global High-resolution Thermospheric Imaging (MIGHTI): instrument design and calibration

Space Science Reviews, 212(1-2), pp.553-584. DOI: 10.1007/s11214-017-0358-4

SPDF/CDAWeb. Please also acknowledge the data producer: T. J. Immel at UC Berkeley>SSL

SPDF/SSCWeb. Please also acknowledge the data producer: T. J. Immel at UC Berkeley>SSL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. J. Immel at UC Berkeley>SSL

Ionospheric Connection Explorer (from all.xml/observatory/description/@short)

Michelson Interferometer for Global High-resolution Thermospheric Imaging, Sensor A (from all.xml/instrument/description/@short)

Ionospheric Connection Explorer (from Master/CDFglobalAttributes/Source_name)

Data Product 2.1: Line-of-sight Wind Profiles (from Master/CDFglobalAttributes/Data_type)

Line-of-sight horizontal wind profile. A positive wind is towards MIGHTI.

A quantification of the volume emission rate (VER) quality, from 0 (Bad) to 1 (Good)

Michelson Interferometer for Global High-resolution Thermospheric Imaging (MIGHTI) Sensor B - Line-of-sight Wind Profiles

Michelson Interferometer for Global High-resolution Thermospheric Imaging, Sensor B (from all.xml/instrument/description/@short)

ICON explores the boundary between Earth and space - the ionosphere - to understand the physical connection between our world and the immediate space environment around us. Visit http://icon.ssl.berkeley.edu for more details.

Michelson Interferometer for Global High-resolution Thermospheric Imaging (from all.xml/instrument/description/@short)

Data Product 2.2: Cardinal Vector Winds (from Master/CDFglobalAttributes/Data_type)

Meridional component of the horizontal wind. Positive Northward.

A quantification of the VER data quality, from 0 (Bad) to 1 (Good)

A quantification of the wind data quality, from 0 (Bad) to 1 (Good)

This is a data product from the NASA Ionospheric Connection Explorer mission, an Explorer launched at 21:59:45 EDT on October 10, 2019, from Cape Canaveral AFB in the USA. Guidelines for the use of this product are described in the ICON Rules of the Road  (http://icon.ssl.berkeley.edu/Data).  Responsibility for the mission science falls to the Principal Investigator, Dr. Thomas Immel at UC Berkeley:  Immel, T.J., England, S.L., Mende, S.B. et al. Space Sci Rev (2018) 214: 13. https://doi.org/10.1007/s11214-017-0449-2  Responsibility for the validation of the L1 data products falls to the instrument lead investigators/scientists.  * EUV: Dr. Eric Korpela :  https://doi.org/10.1007/s11214-017-0384-2  * FUV: Dr. Harald Frey : https://doi.org/10.1007/s11214-017-0386-0  * MIGHTI: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0358-4, and https://doi.org/10.1007/s11214-017-0374-4  * IVM: Dr. Roderick Heelis : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for the validation of the L2 data products falls to those scientists responsible for those products.  * Daytime O and N2 profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-018-0477-6  * Daytime (EUV) O+ profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-017-0385-1  * Nighttime (FUV) O+ profiles: Dr. Farzad Kamalabadi : https://doi.org/10.1007/s11214-018-0502-9  * Neutral Wind profiles: Dr. Jonathan Makela : https://doi.org/10.1007/s11214-017-0359-3  * Neutral Temperature profiles: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0434-9  * Ion Velocity Measurements : Dr. Russell Stoneback : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for Level 4 products falls to those scientists responsible for those products.  * Hough Modes : Dr. Chihoko Yamashita :  https://doi.org/10.1007/s11214-017-0401-5  * TIEGCM : Dr. Astrid Maute : https://doi.org/10.1007/s11214-017-0330-3  * SAMI3 : Dr. Joseph Huba : https://doi.org/10.1007/s11214-017-0415-z  Pre-production versions of all above papers are available on the ICON website.  http://icon.ssl.berkeley.edu/Publications  Overall validation of the products is overseen by the ICON Project Scientist, Dr. Scott England.  NASA oversight for all products is provided by the Mission Scientist, Dr. Jeffrey Klenzing.  Users of these data should contact and acknowledge the Principal Investigator Dr. Immel and the party directly responsible for the data product (noted above) and acknowledge NASA funding for the collection of the data used in the research with the following statement : "ICON is supported by NASA's Explorers Program through contracts NNG12FA45C and NNG12FA42I".  These data are openly available as described in the ICON Data Management Plan available on the ICON website (http://icon.ssl.berkeley.edu/Data). 

Michelson Interferometer for Global High resolution imaging of the Thermosphere and Ionosphere (from all.xml/instrument/description/@short)

Data Product 2.3: MIGHTI Retrieved Temperatures and Brightnesses (from Master/CDFglobalAttributes/Data_type)

Bias (systematic) uncertainties in derived temperatures by altitude.

Statistical (1-sigma) uncertainties in derived temperature by altitude.

Background Signal by filter by altitude and filter. This has been corrected for flatfield effects across the detector.

Common shift of all filter center wavenumbers due to temperature by altitude

Uncertainty (1-sigma) in the shift of all filter center wavenumbers by altitude.

ICON FUV Daytime: column density ratio of thermospheric atomic oxygen to molecular nitrogen. 

ICON explores the boundary between Earth and space (the ionosphere) to understand  the physical connection between our world and the immediate space environment around us. Visit http://icon.ssl.berkeley.edu  for more details.

This is a data product from the NASA Ionospheric Connection Explorer mission, an Explorer launched in 2019.  Guidelines for the use of this product are described in the ICON Rules of the Road  (https://http://icon.ssl.berkeley.edu/Data).  Responsibility for the mission science falls to the Principal Investigator, Dr. Thomas Immel at UC Berkeley: Immel, T.J., England, S.L., Mende, S.B. et al. Space Sci Rev (2018) 214: 13. https://doi.org/10.1007/s11214-017-0449-2  Responsibility for the validation of the L1 data products falls to the instrument lead investigators/scientists. * EUV: Dr. Eric Korpela :  https://doi.org/10.1007/s11214-017-0384-2  * FUV: Dr. Harald Frey : https://doi.org/10.1007/s11214-017-0386-0 * MIGHTI: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0358-4, and https://doi.org/10.1007/s11214-017-0374-4 * IVM: Dr. Roderick Heelis : https://doi.org/10.1007/s11214-017-0383-3   Responsibility for the validation of the L2 data products falls to those scientists responsible for those products.  * Daytime O and N2 profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-018-0477-6 * Daytime (EUV) O+ profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-017-0385-1 * Nighttime (FUV) O+ profiles: Dr. Farzad Kamalabadi : https://doi.org/10.1007/s11214-018-0502-9 * Neutral Wind profiles: Dr. Jonathan Makela : https://doi.org/10.1007/s11214-017-0359-3 * Neutral Temperature profiles: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0434-9 * Ion Velocity Measurements : Dr. Russell Stoneback : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for Level 4 products falls to those scientists responsible for those products. * Hough Modes : Dr. Chihoko Yamashita :  https://doi.org/10.1007/s11214-017-0401-5 * TIEGCM : Dr. Astrid Maute : https://doi.org/10.1007/s11214-017-0330-3 * SAMI3 : Dr. Joseph Huba : https://doi.org/10.1007/s11214-017-0415-z  Pre-production versions of all above papers are available on the ICON website.  Overall validation of the products is overseen by the ICON Project Scientist, Dr. Scott England.  NASA oversight for all products is provided by the Mission Scientist, Dr. Jeffrey Klenzing.  Users of these data should contact and acknowledge the Principal Investigator Dr. Immel and the party directly responsible for the data product (noted above) and acknowledge NASA funding for the collection of the data used in the research with the following statement : "ICON is supported by NASA’s Explorers Program through contracts NNG12FA45C and NNG12FA42I".  These data are openly available as described in the ICON Data Management Plan available on the ICON website (http://icon.ssl.berkeley.edu/Data).

Space Science Reviews, 212(1-2), pp.655-696. DOI: 10.1007/s11214-017-0386-0

Iconospheric Connection Explorer (from all.xml/observatory/description/@short)

Iconospheric Connection Explorer (from Master/CDFglobalAttributes/Source_name)

Data Product 2.4: FUV Daytime (from Master/CDFglobalAttributes/Data_type)

This is a data product from the NASA Ionospheric Connection Explorer mission, an Explorer launched in 2019.  Guidelines for the use of this product are described in the ICON Rules of the Road  (https://http://icon.ssl.berkeley.edu/Data).  Responsibility for the mission science falls to the Principal Investigator, Dr. Thomas Immel at UC Berkeley: Immel, T.J., England, S.L., Mende, S.B. et al. Space Sci Rev (2018) 214: 13. https://doi.org/10.1007/s11214-017-0449-2  Responsibility for the validation of the L1 data products falls to the instrument lead investigators/scientists. * EUV: Dr. Eric Korpela :  https://doi.org/10.1007/s11214-017-0384-2  * FUV: Dr. Harald Frey : https://doi.org/10.1007/s11214-017-0386-0 * MIGHTI: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0358-4, and https://doi.org/10.1007/s11214-017-0374-4 * IVM: Dr. Roderick Heelis : https://doi.org/10.1007/s11214-017-0383-3   Responsibility for the validation of the L2 data products falls to those scientists responsible for those products.  * Daytime O and N2 profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-018-0477-6 * Daytime (EUV) O+ profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-017-0385-1 * Nighttime (FUV) O+ profiles: Dr. Farzad Kamalabadi : https://doi.org/10.1007/s11214-018-0502-9 * Neutral Wind profiles: Dr. Jonathan Makela : https://doi.org/10.1007/s11214-017-0359-3 * Neutral Temperature profiles: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0434-9 * Ion Velocity Measurements : Dr. Russell Stoneback : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for Level 4 products falls to those scientists responsible for those products. * Hough Modes : Dr. Chihoko Yamashita :  https://doi.org/10.1007/s11214-017-0401-5 * TIEGCM : Dr. Astrid Maute : https://doi.org/10.1007/s11214-017-0330-3 * SAMI3 : Dr. Joseph Huba : https://doi.org/10.1007/s11214-017-0415-z  Pre-production versions of all above papers are available on the ICON website.  Overall validation of the products is overseen by the ICON Project Scientist, Dr. Scott England.  NASA oversight for all products is provided by the Mission Scientist, Dr. Ruth Lieberman.  Users of these data should contact and acknowledge the Principal Investigator Dr. Immel and the party directly responsible for the data product (noted above) and acknowledge NASA funding for the collection of the data used in the research with the following statement : "ICON is supported by NASA’s Explorers Program through contracts NNG12FA45C and NNG12FA42I".  These data are openly available as described in the ICON Data Management Plan available on the ICON website (http://icon.ssl.berkeley.edu/Data).

Daytime O/N2 Retrieval Algorithm for the Ionospheric Connection Explorer (ICON)

SPDF/CDAWeb. Please also acknowledge the data producer: T. J. Immel at UC Berkeley > SSL

SPDF/SSCWeb. Please also acknowledge the data producer: T. J. Immel at UC Berkeley > SSL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. J. Immel at UC Berkeley > SSL

Data Product 2.4: FUV Limb Daytime (from Master/CDFglobalAttributes/Data_type)

This is a data product from the NASA Ionospheric Connection Explorer mission, an Explorer launched at 21:59:45 EDT on October 10, 2019, from Cape Canaveral AFB in the USA. Guidelines for the use of this product are described in the ICON Rules of the Road  (http://icon.ssl.berkeley.edu/Data).  Responsibility for the mission science falls to the Principal Investigator, Dr. Thomas Immel at UC Berkeley:  Immel, T.J., England, S.L., Mende, S.B. et al. Space Sci Rev (2018) 214: 13. https://doi.org/10.1007/s11214-017-0449-2  Responsibility for the validation of the L1 data products falls to the instrument lead investigators/scientists.  * EUV: Dr. Eric Korpela :  https://doi.org/10.1007/s11214-017-0384-2  * FUV: Dr. Harald Frey : https://doi.org/10.1007/s11214-017-0386-0  * MIGHTI: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0358-4, and https://doi.org/10.1007/s11214-017-0374-4  * IVM: Dr. Roderick Heelis : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for the validation of the L2 data products falls to those scientists responsible for those products.  * Daytime O and N2 profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-018-0477-6  * Daytime (EUV) O+ profiles: Dr. Andrew Stephan : https://doi.org/10.1007/s11214-017-0385-1  * Nighttime (FUV) O+ profiles: Dr. Farzad Kamalabadi : https://doi.org/10.1007/s11214-018-0502-9  * Neutral Wind profiles: Dr. Jonathan Makela : https://doi.org/10.1007/s11214-017-0359-3  * Neutral Temperature profiles: Dr. Christoph Englert : https://doi.org/10.1007/s11214-017-0434-9  * Ion Velocity Measurements : Dr. Russell Stoneback : https://doi.org/10.1007/s11214-017-0383-3  Responsibility for Level 4 products falls to those scientists responsible for those products.  * Hough Modes : Dr. Chihoko Yamashita :  https://doi.org/10.1007/s11214-017-0401-5  * TIEGCM : Dr. Astrid Maute : https://doi.org/10.1007/s11214-017-0330-3  * SAMI3 : Dr. Joseph Huba : https://doi.org/10.1007/s11214-017-0415-z  Pre-production versions of all above papers are available on the ICON website.  http://icon.ssl.berkeley.edu/Publications  Overall validation of the products is overseen by the ICON Project Scientist, Dr. Scott England.  NASA oversight for all products is provided by the Mission Scientist, Dr. Jeffrey Klenzing.  Users of these data should contact and acknowledge the Principal Investigator Dr. Immel and the party directly responsible for the data product (noted above) and acknowledge NASA funding for the collection of the data used in the research with the following statement :  'ICON is supported by' NASA's Explorers Program through contracts NNG12FA45C and NNG12FA42I.  These data are openly available as described in the ICON Data Management Plan available on the ICON website (http://icon.ssl.berkeley.edu/Data). 

Intensified Far Ultraviolet Imager (from all.xml/instrument/description/@short)

Data Product 2.5: FUV Nighttime O+ profile (from Master/CDFglobalAttributes/Data_type)

A quantification of the inversion quality, from 0 (Bad) to 1 (Good)

Volume Emission Rate (VER) of 135.6-nm emission (non-smoothed, whole earth view)

ICON explores the boundary between Earth and space (the ionosphere) to understand the physical connection between our world and the immediate space environment around us. Visit https://icon.ssl.berkeley.edu for more details.

Space Science Reviews, 212(1-2), pp.631-643. DOI: 10.1007/s11214-017-0384-2

Extreme Ultraviolet Imager (from all.xml/instrument/description/@short)

Data Product 2.6: EUV Daytime Ionosphere (from Master/CDFglobalAttributes/Data_type)

1-Sigma in O+ Density Profile from Retrieval - stacked time_series

ICON explores the boundary between Earth and space (the ionosphere) to understand the physical connection between our world and the immediate space environment around us. Visit http://icon.ssl.berkeley.edu for more details.

Ion Velocity Measurements for the Ionospheric Connections Explorer

Space Science Reviews, 212(1-2), pp.615-629. DOI: 10.1007/s11214-017-0383-3

Ion temperature determined using a best fit of RPA measurements to Whipple equation.

Raw ion velocity determined using a best fit of RPA measurements to the Whipple equation.

Plasma potential relative to instrument aperture plane - determined using a best fit to RPA measurements.

Altitude of North Footpoint of Geomagnetic Line at 150 km from IGRF

ECEF X-Component of Field Aligned Drift Direction at Northern Footpoint

ECEF Y-Component of Field Aligned Drift Direction at Northern Footpoint

ECEF Z-Component of Field Aligned Drift Direction at Northern Footpoint

Latitude of North Footpoint of Geomagnetic Line at 150 km from IGRF

Longitude of North Footpoint of Geomagnetic Line at 150 km from IGRF

ECEF X-Component of Meridional Drift Direction at Northern Footpoint

ECEF Y-Component of Meridional Drift Direction at Northern Footpoint

ECEF Z-Component of Meridional Drift Direction at Northern Footpoint

ECEF X-Component of Zonal Drift Directrion at Northern Footpoint

ECEF Y-Component of Zonal Drift Directrion at Northern Footpoint

Altitude of South Footpoint of Geomagnetic Line at 150 km from IGRF

ECEF X-Component of Field Aligned Drift Direction at Southern Footpoint

ECEF Y-Component of Field Aligned Drift Direction at Southern Footpoint

ECEF Z-Component of Field Aligned Drift Direction at Southern Footpoint

Latitude of South Footpoint of Geomagnetic Line at 150 km from IGRF

Longitude of South Footpoint of Geomagnetic Line at 150 km from IGRF

ECEF X-Component of Meridional Drift Direction at Southern Footpoint

ECEF Y-Component of Meridional Drift Direction at Southern Footpoint

ECEF Z-Component of Meridional Drift Direction at Southern Footpoint

Data Product 2.7: IVM Ionospheric Parameters (from Master/CDFglobalAttributes/Data_type)

Binary Coded Integer Describing Space Environment Region of Space Craft

References:     1.Troshichev O.A. et al, Planet.Space Sci.,   36, 1095, 1988. 2.Vennerstrom S. et al,  Report UAG-103, World Data Center A for STP, Boulder, April 1994 

SPDF/CDAWeb. Please also acknowledge the data producer: V.Sergeev at Institute of physics Univ. of St.-Peterburg St.-Peterburg, Russia

SPDF/SSCWeb. Please also acknowledge the data producer: V.Sergeev at Institute of physics Univ. of St.-Peterburg St.-Peterburg, Russia

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V.Sergeev at Institute of physics Univ. of St.-Peterburg St.-Peterburg, Russia

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/ground/geo_index/1995/ig_k0_pci_19950807_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

PC Geomagnetic Index (from all.xml/instrument/description/@short)

Imager for Magnetospause-to-Aurora Global Extreme Ultraviolet Imager Modified Data 2

Katus, R. M., D. L. Gallagher, M. W. Liemohn,A. M. Keesee, and L. K. Sarno?Smith (2015), Statistical storm time examination of MLT dependent plasmapause location derived from IMAGE EUV,J. Geophys. Res. Space Physics, 120, 5545?5559, doi:10.1002/2015JA021225.

IMAGE Extreme Ultraviolet Imager web site, hosted by LPL, Univ. of Arizona

Imager for Magnetopause-to-Aurora Global Exploration, IMAGE, satellite Extreme Ultraviolet Imager, instrument information web site, hosted by the Lunar and Planetary Laboratory, University of Arizona

General information concerning the Imager for Magnetopause-to-Aurora Global Exploration, IMAGE, Extreme Ultraviolet, EUV, instrument

Katus et al. (2015) IMAGE EUV storm time plasmapause position, Journal of Geophysical Research Space Physics publication

Katus, R.M., D.L. Gallagher, M.W. Liemohn, A.M. Keesee, and L.K. Sarno-Smith, Statistical Storm Time Examination of MLT dependent Plasmapause Location derived from IMAGE EUV, J. Geophys. Res. Space Phys., 120, 5545-5559, 2015, DOI: 10.1002/2015JA021225

SPDF/CDAWeb. Please also acknowledge the data producer: R. M. Katus at Eastern Michigan University

SPDF/SSCWeb. Please also acknowledge the data producer: R. M. Katus at Eastern Michigan University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. M. Katus at Eastern Michigan University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/fuv/euv_m2/2000/image_m2_euv_20000504_v02.cdf. The most common cadence, 599999994412 [ns] = PT9M59.999994S, occurred for 41.6667% of the 10 timesteps. 

Imager for Magnetospause-to-Aurora Global Exploration (from all.xml/observatory/description/@short)

Imager for Magnetospause-to-Aurora Global Exploration (from Master/CDFglobalAttributes/Source_name)

Sharpest gradient from equatorial IMAGE EUV Ion Images, at 48 MLT 0:0.5:23.5 MLT hours (spectrogram)

Sharpest gradient from equatorial IMAGE EUV !CIon Images. 12MLT=down, 6MLT=right

Sharpest gradient from equatorial IMAGE EUV !CIon Images. 12MLT=down, 6MLT=left

Sharpest gradient from equatorial IMAGE EUV Ion Images. Images flipped so 6MLT is to the left

---> (MOVIE) Sharpest gradient from equatorial IMAGE EUV Ion Images.

Integer quality rating 1:3 of the plasmapause data with 3 being the best

IMAGE EUV Images mapped to the !Cequatorial plane. 12MLT=down, 6MLT=right

IMAGE EUV Images mapped to the !Cequatorial plane. 12MLT=down, 6MLT=left

IMAGE EUV Images mapped to the equatorial plane. Images flipped so 6MLT is to the left

---> (MOVIE) IMAGE EUV Images mapped to the equatorial plane, log10 scale.

IMAGE RPI electron density along the spacecraft orbit, IMAGE Radio Plasma Imager (RPI)

The electron density values listed in this file are derived from the IMAGE Radio Plasma Imager (B.W. Reinisch, PI) data using an automatic fitting program written by Phillip Webb with manual correction.The electron number densities were produced using an automated procedure (with manual correction when necessary) which attempted to self-consistently fit an enhancement in the IMAGE RPI Dynamic Spectra to either 1) the Upper Hybrid Resonance band, 2) the Z-mode or 3) the continuum edge. The automatic algorithm works by rules determined by comparison of the active and passive RPI data [Benson et al., GRL, vol. 31, L20803, doi:10.1029/2004GL020847, 2004].The manual data points are not from frequencies chosen freely by a human. Rather the human specifies that the computer should search for a peak or continuum edge in a certain frequency region. Thus even the manual points are determined, in part, by the automatic algorithms. Of course that does not guarantee that the data points are right, but it does eliminate some human bias.For a more detailed description see http://ulcar.uml.edu/rpi.html.

Please acknowledge CDAWeb/SPDF, Phillip Webb, Yongli Wang, Bodo Reinisch and Richard Denton.

IMAGE RPI Instrument page maintained by NASA GSFC with RPI facts, description, team, data, documents, discoveries, and related links sections

IMAGE RPI Instrument page maintained by University of Massachusetts Lowell with RPI description, team, software downloads, software user guides, access to CORPRAL automated prospecting results, mission planning tools and commanding guide, data model descriptions for Level 0 and 1, sonification files of 2003 Halloween storm, and useful links

RPIAnywhere software download page, including BinBrowser (RPI data analysis tool) and EdRPI (RPI mission planning tool)

This data file is a work in progress, and may be modified later. Be warned that the electron density values inferred from the continuum edge are especially tentative.

SPDF/CDAWeb. Please also acknowledge the data producer: R. E. Denton & B.W. Reinisch at Dartmouth, UMLCAR

SPDF/SSCWeb. Please also acknowledge the data producer: R. E. Denton & B.W. Reinisch at Dartmouth, UMLCAR

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. E. Denton & B.W. Reinisch at Dartmouth, UMLCAR

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/rpi/rpi_Ne_fp_along_orbit/rpi_electron_density_CDF/2001/im_electron_density_rpi_20010101_v01.cdf. The most common cadence, 117995 [ms] = PT1M57.995S, occurred for 4.1527% of the 124 timesteps. 

Imager for Magnetopause to Aurora Global Exploration (from all.xml/observatory/description/@short)

Radio Plasma Imager (from all.xml/instrument/description/@short)

Imager for Magnetopause to Aurora Global Exploration (from Master/CDFglobalAttributes/Source_name)

Electron Plasma Parameters (from Master/CDFglobalAttributes/Data_type)

L_dip - L-shell calculated from R and MLAT assuming a dipole magnetic field

Spectral feature for auto-fit, 1:Upper Hybrid, 2:Z-Mode, 3:Continuum Edge

electron cyclotron frequency from the spacing of n+1/2 harmonics

standard deviation (kHz) of fce_n+1/2 based on individual frequencies

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Jim Burch at Southwest Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Jim Burch at Southwest Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Jim Burch at Southwest Research Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hk/ads_k0/2000/im_hk_ads_20000325_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for all 176 timesteps. 

Imager for Magnetopause to Auroral Global Exploration (from all.xml/observatory/description/@short)

Attitude Determination System (from all.xml/instrument/description/@short)

Imager for Magnetopause to Auroral Global Exploration (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hk/ast_k0/2000/im_hk_ast_20000325_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for all 176 timesteps. 

Autonomous Star Tracker (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hk/com_k0/2000/im_hk_com_20000325_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for all 176 timesteps. 

Communication Systems (from all.xml/instrument/description/@short)

Filtered Spinrate valid flag given to CIDP (0=not valid,1=valid)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hk/fsw_k0/2000/im_hk_fsw_20000325_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for all 176 timesteps. 

Schedulers 1 Hz counter. Note: CDF_UINT4 data was converted to HAPI double.

DRAM multibit error counter. Note: CDF_UINT4 data was converted to HAPI double.

DRAM singlebit error counter. Note: CDF_UINT4 data was converted to HAPI double.

CMM multibit error counter. Note: CDF_UINT4 data was converted to HAPI double.

CMM singlebit error counter. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hk/pwr_k0/2000/im_hk_pwr_20000325_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for all 176 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hk/tml_k0/2000/im_hk_tml_20000325_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for all 176 timesteps. 

Ion Images, Key Parameters, IMAGE Extreme UltraViolet (EUV) experiment

SPDF/CDAWeb. Please also acknowledge the data producer: Bill Sandel at U/Arizona

SPDF/SSCWeb. Please also acknowledge the data producer: Bill Sandel at U/Arizona

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Bill Sandel at U/Arizona

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/euv/euv_k0/2000/im_k0_euv_20000328_v01.cdf. The most common cadence, 600180 [ms] = PT10M0.18S, occurred for 5.2632% of the 2 timesteps. 

EUV ion (He+) images of earth and surrounding plasmasphere (no grid, small format, linear scale)

 ---> EUV ion images, as above (mapped, large format, log10 scale)

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Don Mitchell at APL

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Don Mitchell at APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Don Mitchell at APL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/hena/hena_k0/2000/im_k0_hena_20000421_v01.cdf. The most common cadence, 119997 [ms] = PT1M59.997S, occurred for 15.9879% of the 106 timesteps. 

High Energy Neutral Atom Imager (from all.xml/instrument/description/@short)

ENA H Images @ 50-60 keV (no grid, small format, linear scale) - Image0

ENA H Images @ 39-50 keV (no grid, small format, linear scale) - Image1

ENA H Images @ 27-39 kev (no grid, small format, linear scale) - Image2

ENA H Images @ 16-27 keV (no grid, small format, linear scale) - Image3

ENA H Images @ 10-16 keV (no grid, small format, linear scale) - Image4

ENA H Images @ <10 keV (no grid, small format, linear scale) - Image5

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Tom Moore at GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Tom Moore at GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Tom Moore at GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/lena/lena_k0/2000/im_k0_lena_20000524_v01.cdf. The most common cadence, 120299 [ms] = PT2M0.299S, occurred for 2.3743% of the 17 timesteps. 

LOW ENERGY NEUTRAL ATOM IMAGER (from all.xml/instrument/description/@short)

ENA H Images @ 20 eV (no grid, small format, linear scale) - Image0

ENA H Images @ 70 eV (no grid, small format, linear scale) - Image1

ENA H Images @ 200 eV (no grid, small format, linear scale) - Image2

Medium Energy Neutral Atom (MENA) H Images, Key Parameters, IMAGE

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Craig Pollock at SwRI

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Craig Pollock at SwRI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Craig Pollock at SwRI

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/mena/mena_k0/2000/im_k0_mena_20000404_v01.cdf. The most common cadence, 119998 [ms] = PT1M59.998S, occurred for 3.0488% of the 10 timesteps. 

Medium Energy Neutral Atom Imager (from all.xml/instrument/description/@short)

ENA H Images @ 1.0-2.2 keV/n (no grid, small format, linear scale) - Image0

ENA H Images @ 2.2-5.3 keV/n (no grid, small format, linear scale) - Image1

ENA H Images @ 5.3-12 keV/n (no grid, small format, linear scale) - Image2

ENA H Images @ 12-27 keV/n (no grid, small format, linear scale) - Image3

ENA H Images @ 27-70 keV/n (no grid, small format, linear scale) - Image4

RPI Plasmagram/Echomap, Key Parameters, IMAGE Radio Plasma Imager (RPI)

SPDF/CDAWeb. Please also acknowledge the data producer: B.W. Reinisch at UMLCAR

SPDF/SSCWeb. Please also acknowledge the data producer: B.W. Reinisch at UMLCAR

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: B.W. Reinisch at UMLCAR

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/rpi/rpi_k0/2000/im_k0_rpi_20000326_v01.cdf. The most common cadence, 119997 [ms] = PT1M59.997S, occurred for 22.9814% of the 111 timesteps. 

Echo Amplitude Image [nV] - Plasmagram - linear (frequency vs. range, standard display/orientation)

Program Specifications (25 values/epoch) [NO PLOT - LISTING ONLY]

Electron Auroral Images @ 1356A, Key Parameters, IMAGE Far UltraViolet (FUV) Spectrographic Imaging camera Electrons (SIE) 

SPDF/CDAWeb. Please also acknowledge the data producer: S. Mende at UC/Berkeley/SSL

SPDF/SSCWeb. Please also acknowledge the data producer: S. Mende at UC/Berkeley/SSL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: S. Mende at UC/Berkeley/SSL

Magnetopause to Aurora (from all.xml/observatory/description/@short)

Electron Auroral Images at 1356 A (from all.xml/instrument/description/@short)

Magnetopause to Aurora (from Master/CDFglobalAttributes/Source_name)

FUV/SIE Electron Images @ 1356A (raw cnts, no grid, small format, linear scaling) - use CDAWeb noise filter

FUV/SIE Electron Images @ 1356A (no grid, small format, log10 scaling)

orientation direction cosine X (direction of true spin axis at SIE Snapshot Time)

oriention direction cosine Y (direction of true spin axis at SIE Snapshot Time)

SIE spin axis orientation direction cosine X-direction, s/c frame

SIE spin axis orientation direction cosine Y-direction, s/c frame

SIE spin axis orientation direction cosine Z-direction, s/c frame

Proton Auroral Images @ 1218A, Key Parameters, IMAGE Far UltraViolet (FUV) Spectrographic Imaging camera Protons (SIP)

Proton Auroral Images at 1218 A (from all.xml/instrument/description/@short)

FUV/SIP Proton Images @1218A (raw cnts, no grid, small format, linear scale) - use CDAWeb noise filter

FUV/SIP Proton Images @ 1218A, (no grid, small format, log10 scaling)

[DO NOT USE] FUV/SIP Proton Images @1218A (raw cnts, mapped, large format, log10 scaling) 

orientation direction cosine X (direction of true spin axis at SIP Snapshot Time)

orientation direction cosine Y (direction of true spin axis at SIP Snapshot Time)

Auroral Images, Key Parameters, IMAGE Far UltraViolet (FUV) Wide-band Imaging Camera (WIC)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/fuv/wic_k0/2000/im_k0_wic_20000425_v01.cdf. The most common cadence, 248393 [ms] = PT4M8.393S, occurred for 6.2500% of the 1 timesteps. 

Auroral Images, Wide-Band Imaging Camera (from all.xml/instrument/description/@short)

FUV/WIC LBH Auroral Images (raw cnts/14 bits, no grid, small format, linear scale)

 ---> FUV/WIC LBH Auroral Images, as above (small format, log10 scaling)

 ---> FUV/WIC LBH Auroral Images, as above (large format, log10 scaling)

 ---> [DO NOT USE] FUV/WIC LBH Auroral Mapped Images, as above (log10 scaling)

 ---> [DO NOT USE] FUV/WIC LBH Auroral Mapped Images, as above (movie format, log10 scaling)

orientation direction cosine X (direction of true spin axis at WIC Snapshot Time)

oriention direction cosine Y (direction of true spin axis at WIC Snapshot Time)

WIC spin axis orientation direction cosine X-direction, s/c frame

WIC spin axis orientation direction cosine Y-direction, s/c frame

WIC spin axis orientation direction cosine Z-direction, s/c frame

RPI Dynamic Spectrogram, Key Parameters, IMAGE Radio Plasma Imager (RPI)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/rpi/rpi_k1/2000/im_k1_rpi_20000412_v01.cdf. The most common cadence, 299791 [ms] = PT4M59.791S, occurred for 35.2941% of the 6 timesteps. 

IMAGE GSE and GSM coordinates for the full mission, as plots and listings, are also available from

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/orbit/def_or/2000/im_or_def_20000327_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for all 719 timesteps. 

[All values have been corrected 7/9/2001] GSM Cartesian Position, time-series

[All values have been corrected 7/9/2001] GSE Cartesian Position, time-series

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/image/orbit/pre_or/2001/im_or_pre_20010221_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for all 719 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee3/helio1day/isee-3_helio1day_position_19840101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 99.9829% of the 5843 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee3/helio1hr/isee-3_helio1hr_position_20140101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 17519 timesteps. 

These files provides access to a field/plasma-merged 2-min ISEE3 data setcreated at NSSDC as part of preparing ISEE3 data for new OMNI. Input to the data set were 1-min MAG magnetic field data, 24-splasma data, and daily spacecraft position data, all obtained from https://spdf.gsfc.nasa.gov/pub/data/isee/isee3/ from which needed documentation may be found. The annual files of this ASCII data set may be accessed at this site https://spdf.gsfc.nasa.gov/pub/data/isee/isee3/2_min_merged_mag_plasma/ as well.Time span: Mag field: 1978-09-11 - 1982-10-12           Plasma: 1978-09-11 - 1980-02-19Note that Magntic Field is given in SE- Spacecraft-centered Solar-Ecliptic coordinate system. 

ISEE-3 Merged Magnetic Field and Solar Wind Plasma 2 min Average ASCII Data

Description of the Format of the ISEE-3 Merged Magnetic Field and Solar Wind Plasma 2 min Average ASCII Data

SPDF/CDAWeb. Please also acknowledge the data producer: Edward Smith at JPL NASA

SPDF/SSCWeb. Please also acknowledge the data producer: Edward Smith at JPL NASA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Edward Smith at JPL NASA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee3/isee3_cdaweb/2min_magnetic_field_plasma/1978/isee-3_magplasma_2min_magnetic_field_plasma_19780813_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for all 101519 timesteps. 

Vector Helium Magnetometer and Plasma (from all.xml/instrument/description/@short)

ISEE-3 2-min averaged Magnetic Field and Plasma (from Master/CDFglobalAttributes/Data_type)

magnetic field vector in s/c-centered Solar-Ecliptic coordinates

This data set contains averaged 1-minute magnetic field data converted from simple ASCII records. It was created at NSSDC from a more complex, multi-resolution data set (NSSDC ID = SPHE-00673; Old ID = 78-079A-02D) provided by the Principal Investigator team and now available from https://spdf.gsfc.nasa.gov/pub/data/isee/isee3/magnetic_fields/The coordinate system for the B-field components is the JPL-defined I,S coordinate system (origin at the spacecraft): I is the unit vector in the direction of the ISEE-3 spin axis (positive in the northward direction), and S is the unit vector from the spacecraft to the sun. The z-axis is parallel to to I, the y-axis to the cross-product I x S, and the x-axis to Y x Z. The I,S coordinate system is approximately the same as the Solar Ecliptic (SE) system since the spacecraft z-axis (the spin axis) is maintained within 0.5 degree of perpendicular to the ecliptic plane. (SE is defined the same way as GSE, but with the spacecraft [point of observation] substituted for Earth).  For years 1984-1990 we added spacecraft position in HGI coordinateThe HGI coordinates are Sun-centered and inertially fixed with respect to an  X-axis directed along the intersection line of theecliptic and solar equatorial  planes, and defines zero of the longitude, HGI_LONG. The solar equator plane  is inclined at 7.25degrees from the ecliptic. This direction was towards ecliptic  longitude of 74.367 deg on 1 January 1900 at 12:00 UT; because of the precession of the Earth"s equator, this longitude increases by 1.4 deg/century.  The Z-axis is directed perpendicular to and northward of the solar equator, and the Y-axis completes the right-handed set.  The longitude, HGI_LONG increase from zero in the X-direction towards Y-direction.The latitude HG_LAT increases to +90 deg towards  the north pole, and to -90 deg towardsm south pole. Note that here present values averaged in 1-minute, e.g. <B>^2 may be not equal <B^2)>.

ISEE-3 Magnetic Field 1 min Average ASCII Data, 1978-1983, Magnetospheric Phase of the ISEE 3 Mission

Description of the Format of the ISEE-3 Magnetic Field 1 min Average ASCII Data, 1978-1983, covering the Magnetospheric Phase of the ISEE 3 Mission

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee3/isee3_cdaweb/1min_magnetic_field/isee-3_mag_1min_magnetic_field_19780801_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 220319 timesteps. 

MAG - Vector Helium Magnetometer (from all.xml/instrument/description/@short)

ISEE-3 1-min averaged Magnetic Field (from Master/CDFglobalAttributes/Data_type)

C. T. Russell (IEEE Trans. Geoscience Electronics, GE-16, 239-242, 1978). This publication is available online at http://www-ssc.igpp.ucla.edu/personnel/russell/papers/ISEE_fluxgate/.

SPDF/CDAWeb. Please also acknowledge the data producer: C. T. Russell at UCLA

SPDF/SSCWeb. Please also acknowledge the data producer: C. T. Russell at UCLA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C. T. Russell at UCLA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/isee1_cdaweb/4sec_mfi/1977/isee1_4sec_mfi_19771022_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 87.3545% of the 2252 timesteps. 

International Sun-Earth Explorer 1 (from all.xml/observatory/description/@short)

3-axis fluxgate magnetometer (from all.xml/instrument/description/@short)

International Sun-Earth Explorer 1 (from Master/CDFglobalAttributes/Source_name)

Magnetic Field X Comp. - Spacecraft axes (near GSE): 12-sec avg at 4-sec intervals

Magnetic Field Y Comp. - Spacecraft axes (near GSE): 12-sec avg at 4-sec intervals

Magnetic Field Z Comp. - Spacecraft axes (near GSE): 12-sec avg at 4-sec intervals

Data at 60-s and 4-s resolution also available through IGPP at UCLA for entire ISEE mission (Oct.22, 1977 through Sept. 25, 1987).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/isee1_cdaweb/60sec_mfi/1977/isee1_60sec_mfi_19771022_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 3444 timesteps. 

60-sec vector magnetic field (from Master/CDFglobalAttributes/Data_type)

NMP_Sep:  Separation vector <ISEE 1> - <ISEE 2> component along the model normal to the magnetopause

NBS_Sep:  Separation vector <ISEE 1> - <ISEE 2> component along bow shock normal. 

This enhanced CDF master was generated by NSSDC, with input from R. Fitzenreiter and A. F.-Vinas, to make useable a bare-bones CDF data set provided earlier to NSSDC. This current CDF master version, Oct. 5, 2007, is used for making a new CDF by selecting only certain variables from those available in the original bare-bones CDF (SPHE-00414).

SPDF/CDAWeb. Please also acknowledge the data producer: K. Ogilvie, R. Fitzenreiter, & A. Vinas at GSFC Code 690

SPDF/SSCWeb. Please also acknowledge the data producer: K. Ogilvie, R. Fitzenreiter, & A. Vinas at GSFC Code 690

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Ogilvie, R. Fitzenreiter, & A. Vinas at GSFC Code 690

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/isee1_cdaweb/h0/fe/1977/isee1_h0_fe_19771029_v01.cdf. The most common cadence, 18245 [ms] = PT18.245S, occurred for 13.4518% of the 106 timesteps. 

International Sun Earth Explorer 1 (from all.xml/observatory/description/@short)

International Sun Earth Explorer 1 (from Master/CDFglobalAttributes/Source_name)

Fast Electron Moments (from Master/CDFglobalAttributes/Data_type)

Electron density at 0.5 sec resolution (60-deg sector) taken during one spin. 

Electron Temperature = 1/3 trace of the diagonalized pressure tensor.

Normalized difference between perp. eigenvalues of pressure tensor 

Cosine of the angle between pressure tensor principal axis and magnetic field

Eigenvalues of diagonalized pressure tensor divided by (density * Boltzmann constant)

Highest, mid, and lowest energy electron channels above SC potential

Hi, mid, & lowest energy electron channels > SC potential, used in moments.

Data coverage includes the region from 6 earth radii out to (but excluding) the bow shock. The reasons for selecting this area of coverage are that the solar wind ion distributions are too cold to be adequately resolved by this instrument, and inside the region of 6 earth radii the fast plasma data would be contaminated by the energetic particle background. The data are provided at a temporal resolution of approximately 60 seconds. They represent moments of individual two-dimensional (2D) distributions obtained in approximately 3 or approximately 6 seconds (see below). No time averaging over longer intervals is involved; instead, the temporal resolution of the full data set (approximately 3 / 6 / 12 s) was reduced to approximately 60 s. The UT given indicates the start of the respective sampling interval. For a description of the instrument see Bame et al., 1978 (IEEE Transact. Geosci. Electron. GE-16, 216) and Bame et al., 1993 (Rev. Sci. Inst., 64, 1026). Remarks about the computation of the moments may be found in Paschmann et al., 1978 (Space Sci. Rev. 22, 717). The moments were computed for three 'species', but only the ion moments are included here: lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV). The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined.  Tperp and Tpara are obtained from diagonalization of the  3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of  the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by a 'SCALETYP' value of 'linear' in this file. A quality Flag value of 1 indicates that the values are suspect because of unreliable location info. 

SPDF/CDAWeb. Please also acknowledge the data producer: S. Bame & J. Gosling at LANL

SPDF/SSCWeb. Please also acknowledge the data producer: S. Bame & J. Gosling at LANL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: S. Bame & J. Gosling at LANL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/isee1_cdaweb/1min_fpe/1977/isee1_h1_fpe_19771029_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 71.0145% of the 49 timesteps. 

Fast Plasma Experiment (from all.xml/instrument/description/@short)

60-s Fluid Parameters (from Master/CDFglobalAttributes/Data_type)

Energy range covered, 0: 50 eV to 20 KeV per charge; 1: 70 eV to 40 KeV per charge

IFLAG  0: Den >= 0.1 per cm3, 1: Den < 0.1 per cm3 (see VAR_NOTES if = 1)

X-component of 2D bulk velocity (s/c coordinates). See VAR_NOTES.

Y-component of 2D bulk velocity (s/c coordinates). See VAR_NOTES.

These data are high temporal resolution solar wind ion moments derived from measurements obtained by the Los Alamos X-Fan Solar Wind Ion Experiment (SWE) on ISEE-1. The data cover the solar wind seasons for the spacecraft (roughly July through December) from 1977 through 1983. The temporal resolution is 24 seconds at high data rate and 48 seconds at low data rate. Among the parameters, the flow azimuth is given in degrees, with 0 degrees corresponding to flow from the sun [corrected for aberration] and positive azimuths corresponding to flow toward dawn; flow latitude is in degrees, with positive latitudes corresponding to flow toward the south; an alpha/proton fraction of 0.00 means no determination was made. The data providers did not attempt to cross-calibrate density values with those from other experiments. However, they expected that density values will tend to be too low in later years because of detector degradation. Cross-calibration using, for example, IMP-derived values would be a useful exercise. Please note also that many of these measurements were obtained within the foreshock region where the solar wind flow is affected by waves in the foreshock. References: Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., ISEE-1 and ISEE-2 fast plasma experiment and the ISEE-1 solar wind experiment, IEEE Trans. Geosci. Electron., GE-16, 216, 1978];  Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., Magnetospheric plasma analyzer for spacecraft with constrained resources, Rev. Sci. Instrum., 64, 1026 (1993)].The moments are presented in s/c coordinates: the z-axis is aligned with the spin axis, which points radially toward the center of the Earth; the x-axis is in the plane containing the spacecraft spin axis and the spin axis of the Earth, with +X generally northward; and the y-axis points generally eastward. Polar angles are measured relative to the spin axis (+Z), and azimuthal angles are measured around the z-axis, with zero along the +X direction. The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined  spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/isee1_cdaweb/24or48s_fpe/1977/isee1_h2_fpe_19771030_v01.cdf. The most common cadence, 49000 [ms] = PT49S, occurred for 53.1373% of the 542 timesteps. 

International Sun-Earth Explorer (from all.xml/observatory/description/@short)

Fast Plasma & Solar Wind Ion Experiment (from all.xml/instrument/description/@short)

International Sun-Earth Explorer (from Master/CDFglobalAttributes/Source_name)

'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978.

More information on ISEE-1 Plasma Wave Investigation is available at the University of Iowa ISEE Page

ISEE-1 PWI SA data are open to everyone. However, users of these data are encouraged to contact the PI institute and the U of I ISEE website should questions arise.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/waves_pwi/sa_pwi/1977/isee1_pwi_sa_19771022_v01.cdf. The most common cadence, 249880000 [ns] = PT0.24988S, occurred for 37.8640% of the 14447 timesteps. 

Users of the ISEE-1 PWI SA Rapid Sample data are encouraged to acknowledge NASA CDAWeb and The University of Iowa as the source of the data in any publication.

More information on ISEE-1 Plasma Wave Investigation is available at the University of Iowa ISEE PWI Page

ISEE-1 PWI SA Rapid Sample data are open to everyone. However, users of these data are encouraged to contact the PI institute and the ISEE-1 PWI website should questions arise.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/waves_pwi/sa-rapid-e_pwi/1977/isee1_pwi_sa-rapid-e_19771022_v01.cdf. The most common cadence, 31235000 [ns] = PT0.031235S, occurred for 47.3145% of the 119357 timesteps. 

Spectrum Analyzer Rapid Sample (from Master/CDFglobalAttributes/Data_type)

ISEE-1 PWI SFR data are open to everyone. However, users of these data are encouraged to contact the PI institute and the U of I ISEE website should questions arise.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee1/waves_pwi/sfr-e_pwi/1977/isee1_pwi_sfr-e_19771022_v01.cdf. The most common cadence, 31985000000 [ns] = PT31.985S, occurred for 36.3636% of the 24 timesteps. 

Sweep Frequency Receiver (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee2/isee2_cdaweb/4sec_mfi/1977/isee2_4sec_mfi_19771022_v01.cdf. The most common cadence, 4000 [ms] = PT4S, occurred for 90.1471% of the 3248 timesteps. 

International Sun-Earth Explorer 2 (from all.xml/observatory/description/@short)

3-axis fluxgate magnetometer averages (from all.xml/instrument/description/@short)

International Sun-Earth Explorer 2 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee2/isee2_cdaweb/60sec_mfi/1977/isee2_60sec_mfi_19771022_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 3451 timesteps. 

Data coverage includes the region from 6 earth radii out to (but excluding) the bow shock. The reasons for selecting this area of coverage are that the solar wind ion distributions are too cold to be adequately resolved by this instrument, and inside the region of 6 earth radii the fast plasma data would be contaminated by the energetic particle background. The data are provided at a temporal resolution of approximately 60 seconds. They represent moments of individual two-dimensional (2D) distributions obtained in approximately 3 or approximately 6 seconds (see below). No time averaging over longer intervals is involved; instead, the temporal resolution of the full data set (approximately 3 / 6 / 12 s) was reduced to approximately 60 s. The UT given indicates the start of the respective sampling interval. For a description of the instrument see Bame et al., 1978 (IEEE Transact. Geosci. Electron. GE-16, 216) and Bame et al., 1993 (Rev. Sci. Inst., 64, 1026). Remarks about the computation of the moments may be found in Paschmann et al., 1978 (Space Sci. Rev. 22, 717). The moments were computed for three 'species', but only the ion moments are included here: lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV). The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined.  Tperp and Tpara are obtained from diagonalization of the  3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of  the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by a 'SCALETYP' value of 'log' in this file. A quality Flag value of 1 indicates that the values are suspect because of unreliable location info. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/isee/isee2/isee2_cdaweb/1min_fpe/1977/isee2_h1_fpe_19771027_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 92.9134% of the 236 timesteps. 

AMS-02 proton flux (p), helium flux (He), p/He flux ratio, electron flux (e-), positron flux (e+) and e+/e- flux ratio at Bartels rotation time resolution

NASA Web Page for the Alpha Mass Spectrometer-02 (AMS-02) onboard the International Space Station

SPDF/CDAWeb. Please also acknowledge the data producer: Prof. V. Bindi at University of Hawaii at Manoa

SPDF/SSCWeb. Please also acknowledge the data producer: Prof. V. Bindi at University of Hawaii at Manoa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Prof. V. Bindi at University of Hawaii at Manoa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/iss/ams-02/27day_averages/2011/iss_27day-averages_ams-02_20110520_v01.cdf. The most common cadence, 2332800000000000 [ns] = P27D, occurred for 93.5897% of the 73 timesteps. 

International Space Station (from all.xml/observatory/description/@short)

Alpha Magnetic Spectrometer (from all.xml/instrument/description/@short)

International Space Station (from Master/CDFglobalAttributes/Source_name)

Bartels rotation number. Note: CDF_UINT4 data was converted to HAPI double.

Proton flux total error: statistical and systematic added in quadrature.

Proton fluxtime-dependent error: trigger and reconstruction efficiency errors added in quadrature.

Proton Flux systematic error: acceptance, background contamination, geomagnetic cutoff, event selection, rigidity resolution, unfolding, absolute rigidity scale and time-dependent errors added in quadrature.

Helium flux total error: statistical and systematic added in quadrature.

Helium flux time-dependent error: trigger and reconstruction efficiency errors added in quadrature.

Helium flux systematic error: acceptance, background contamination, geomagnetic cutoff, event selection, rigidity resolution, unfolding, absolute rigidity scale and time-dependent errors added in quadrature.

Proton to Helium differential flux ratio, at 40 bins 1.92-60.30 GV.

p/He ratio total error: statistical and systematic added in quadrature.

p/He ratio statistical error: p and He statistical errors added in quadrature.

p/He ratio time-dependent error: p and He time-dependent errors added in quadrature.

p/He ratio systematic error: p and He systematic errors added in quadrature, with correlations in rigidity resolution, unfolding, absolute rigidity scale errors taken into account.

Electron flux total error: statistical and systematic added in quadrature.

Electron flux systematic error: acceptance and background contamination errors added in quadrature.

Positron flux total error: statistical and systematic added in quadrature.

Positron flux systematic error: acceptance and background contamination errors added in quadrature.

Positron to electron differential flux ratio, at 49 bins 1.01-49.3 GeV.

e+/e- ratio total error: statistical and systematic added in quadrature.

e+/e- ratio systematic error: acceptance and background contamination errors added in quadrature.

TEPC serrial number = 1003TEPC Analysis SoftwareVersion Number = 3.1 

Establishment of the Dosimetric Technique in the International Space Station, ISS, with a Position Sensitive-Tissue Equivalent Proportional Chamber, PS-TEPC, 20170802

SPDF/CDAWeb. Please also acknowledge the data producer: Edward Semones at NASA Space Radiation Analysis Group/Johnson Space Center

SPDF/SSCWeb. Please also acknowledge the data producer: Edward Semones at NASA Space Radiation Analysis Group/Johnson Space Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Edward Semones at NASA Space Radiation Analysis Group/Johnson Space Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/iss/dos_tepc/iss_dosanl_tepc_201004290327_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 97.0591% of the 188445 timesteps. 

ISS FPMU 1-sec Summary Plasma Densities, Temperatures, Spacecraft Potentials.

ISS FPMU Summary Ionosphere Wide Langmuir Probe (WLP) density and temperature records, Floating Potential Probe (FPP) spacecraft potential records.

Floating Potential Measurement Unit, FPMU, Home Page, Space Dynamics Laboratory, Utah State University, per NASA Policy Directive 2200.1B, Section 1.a.5

Contact Emily Willis for support and use.  Emily.Willis@nasa.gov

SPDF/CDAWeb. Please also acknowledge the data producer: E. Willis at NASA Marshall Space Flight Center

SPDF/SSCWeb. Please also acknowledge the data producer: E. Willis at NASA Marshall Space Flight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: E. Willis at NASA Marshall Space Flight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/iss/sp_fpmu/2006/iss_sp_fpmu_20060803_v02.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 65.0054% of the 2387 timesteps. 

Floating Potential Measurement Unit (from all.xml/instrument/description/@short)

               Magnetic field measurements on the  Interball- Tail  satellites are carried out by IZMIRAN and Space Research Institute RAS  (SRI)          since 1995.  Satellite has  the orbits  with  apogee 200000 (30 Re)  and perigee 500 km. and provides measurements in the solar wind and in the different       regions of the magnetosphere at the same time with Geotail, Polar and Interbal-A working in the magnetosphere and  Wind, ACE in the solar wind.         Magnetic field measurements on-board the Interball  Tail Probe are carried out by the FM-3I and MFI instruments. FM-3I consists of two flux-gate       magnetometers M1 and  M2  covering two  different  ranges:  200  nT  and  1000  nT.  The   M2 instrument is mostly  used to perform the  attitude        control of  the INTERBALL TAIL spacecraft.   M1 magnetometer data are transmitted to the scientific SSNI  telemetry  system at rates  0.125-16 vectors/s       depending on the instrument  operating mode. The magnetic field data from the M2 magnetometer are transmitted at the  rate 1 vectors per 6 sec. to  the       BNS attitude  control  system.  MFI magnetometer has the next parameters: measured range 0.3-37.5 nT, frequency range 0-2  Hz, sampling rate  from 1/4       to 8 measurements per second. FM-3 M2 magnetometer failed in February 1996, FM-3 M1 and MFI are working until now.                   Data presented here are the  combination of the data of all magnetometers. First of all   FM-3 M1 data are used,  if they are absent, used MFI data       and if data of both magnetometer are absent, FM-3 M2 data presented. In case of FM-3 M1 and MFI, data are averaged for 6 seconds intervals. 

SPDF/CDAWeb. Please also acknowledge the data producer: M.Nozdrachev at IKI, Moscow, Russia

SPDF/SSCWeb. Please also acknowledge the data producer: M.Nozdrachev at IKI, Moscow, Russia

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M.Nozdrachev at IKI, Moscow, Russia

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/mfi_h0/1995/it_h0_mfi_19950806_v01.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for 99.9799% of the 4981 timesteps. 

Interball Tail Probe (from all.xml/observatory/description/@short)

Interball Tail Probe (from Master/CDFglobalAttributes/Source_name)

Radioemission flux measured in 100, 252, 500 kHz ranges, the passband 10 kHz. Loop antenna with 1.5 m2 area is used.Full description: http://www.iki.rssi.ru/interball.html

SPDF/CDAWeb. Please also acknowledge the data producer: V.Kurilchik at Sternberg Astronomical Inst.,Moscow State University, 119899, Universitetsky pr., 13 Moscow, Russia

SPDF/SSCWeb. Please also acknowledge the data producer: V.Kurilchik at Sternberg Astronomical Inst.,Moscow State University, 119899, Universitetsky pr., 13 Moscow, Russia

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V.Kurilchik at Sternberg Astronomical Inst.,Moscow State University, 119899, Universitetsky pr., 13 Moscow, Russia

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/akr/1995/it_k0_akr_19950806_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for all 504 timesteps. 

Interball tail probe (from all.xml/observatory/description/@short)

High frequency radioemission flux (from all.xml/instrument/description/@short)

Interball tail probe (from Master/CDFglobalAttributes/Source_name)

SPDF/CDAWeb. Please also acknowledge the data producer: Yu.Yermolaev at Space Research Inst., Russian Acad. Sci., Moscow, Russia

SPDF/SSCWeb. Please also acknowledge the data producer: Yu.Yermolaev at Space Research Inst., Russian Acad. Sci., Moscow, Russia

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Yu.Yermolaev at Space Research Inst., Russian Acad. Sci., Moscow, Russia

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/cor/1995/it_k0_cor_19950902_v02.cdf. The most common cadence, 119000 [ms] = PT1M59S, occurred for all 270 timesteps. 

Ion moments in the range 25 eV -25 keV (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: J.-A. Sauvaud at CESR, BP 4346, 31029, Toulouse, France

SPDF/SSCWeb. Please also acknowledge the data producer: J.-A. Sauvaud at CESR, BP 4346, 31029, Toulouse, France

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.-A. Sauvaud at CESR, BP 4346, 31029, Toulouse, France

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/ele/1995/it_k0_ele_19950815_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 99.6212% of the 526 timesteps. 

Thermal Electron Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/epi/1995/it_k0_epi_19950804_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 99.3750% of the 318 timesteps. 

Tail Probe Energetic Particle Instrument (from all.xml/instrument/description/@short)

Interball Tail Probe Ion Composition Experiment PROMICS, Key Parameters

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/icd/1995/it_k0_icd_19950822_v01.cdf. The most common cadence, 140000 [ms] = PT2M20S, occurred for 45.4545% of the 10 timesteps. 

Tail Probe Ion Composition Data (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: S.Romanov at Space Research Inst., Russian Acad. Sci., Moscow, Russia.

SPDF/SSCWeb. Please also acknowledge the data producer: S.Romanov at Space Research Inst., Russian Acad. Sci., Moscow, Russia.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: S.Romanov at Space Research Inst., Russian Acad. Sci., Moscow, Russia.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/mfi/1995/it_k0_mfi_19950806_v04.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 99.8141% of the 537 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: J.Safrankova at Charles University, Prague, Czech Republic

SPDF/SSCWeb. Please also acknowledge the data producer: J.Safrankova at Charles University, Prague, Czech Republic

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.Safrankova at Charles University, Prague, Czech Republic

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/vdp/1995/it_k0_vdp_19950814_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for 90.9091% of the 60 timesteps. 

Antisunward Ion Flux (from all.xml/instrument/description/@short)

Magnetic field averages and variance are computed from 4 Hz or 1 Hz data Mf1 magnetic field AC amplitudes are measured by fluxgate sensor.Mf2 magnetic field AC amplitudes are measured by search-coil.Mf3 plasma wave AC amplitudesare measured by Langmuir splitprobe.Full description: http://www.iki.rssi.ru/interball.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/wav/1998/it_k0_wav_19980101_v01.cdf. The most common cadence, 120000 [ms] = PT2M, occurred for all 719 timesteps. 

This page maintains the Situation Analysis for the IKI International Space Missions and its coordination with the Inter-Agency multimission campaigns.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/interball/tail/orbit/1995/it_or_def_19950807_v02.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/juno/helio1day/juno_helio1day_position_20110806_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 5189 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/juno/helio1hr/juno_helio1hr_position_20110806_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 124439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/jupiter_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/jupiter_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

This file contains numerical moments computed from measurements of the Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., Rev. Sci. Inst., in press 1993]. The moments are presented in s/c coordinates: the z-axis is aligned with the spin axis, which points radially toward the center of the Earth; the x-axis is in the plane containing the spacecraft spin axis and the spin axis of the Earth, with +X generally northward; and the y-axis points generally eastward. Polar angles are measured relative to the spin axis (+Z), and azimuthal angles are measured around the z-axis, with zero along the +X direction. The moments are computed for three 'species': lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 21.5 secs after the ion measurements. Epoch is the measurement time appropriate for the ions. The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined  spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined.  Tperp and Tpara are obtained from diagonalization of the  3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of  the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by  non-zero 'SCALEMIN' values in this file. A quality flag value of 1  indicates that the values are  preliminary and have not been checked in detail. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/90_mpa/2005/l0_k0_mpa_20051109_v02.cdf. The most common cadence, 86016 [ms] = PT1M26.016S, occurred for 45.8835% of the 457 timesteps. 

Los Alamos National Laboratory 1990-095 (from all.xml/observatory/description/@short)

Los Alamos National Laboratory 1990-095 (from Master/CDFglobalAttributes/Source_name)

[SPECIALIZED USE ONLY] [Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z) (NOT Available prior to 1993/03/15)

[SPECIALIZED USE ONLY] [Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat, Lon) (NOT available prior to 1993/03/15)

     Electron, proton and helium measurements are taken every 160 ms from one of the three telescopes according to the following sequence:  T1, T2, T3, T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes again according to the timing and sequence above and summed for 10.24 secondswhich is approximately one spacecraft rotation.  SOPA Key Parameters are normally averaged over three telescopes for ~ 1 minute (6 - 10.24 seconddata accumulation cycles) giving an average over much of the sky.  The time associated with each set of Key Parameters is determined by using the time (in minutes of the day) at the start of each data collection cycle as an indexinto an array of 1440 time slots dividing the day into 1440 one minute intervals.  The time reported is the midpoint of each interval.       We provide six fluxes:        Low energy Protons:  50 keV to 400 keV        High energy Protons: 1.2 MeV to 5 MeV        Low energy Electrons:  50 keV to 225 keV        High energy Electrons: 315 keV to 1.5 MeV        Helium      : ~0.9 MeV to ~1.3 Mev        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,                       and oxygen     We also compute two electron temperatures and densities and two protontemperatures and densities.  These are based on approximately the same energyranges as the fluxes given in above and are determined for relativisticMaxwellian distributions.   Status of SOPA Instrument 1990-095:  Loss of all ion data as of July 1992All three thin, front, D1 detectors have failed, having become intolerablynoisy.  The net result of this failure is the complete loss of proton, helium, carbon, nitrogen, oxygen and other high Z Key Parameter data fromthe instrument.  Since all three thick, back D2 detectors are still operating normally, the electron measurements remain only insignificantly affected.      Data is flagged with a data quality flag as follows:   +1 Data is Good    0 Data is Suspect   -1 Data is UnusableReferences:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992

Los Alamos Nation Laboratory spacecraft Synchronous Orbit Particle Analyzer (SOPA)

Journal of Geophysical Research Article containing information on the LANL SOPA instrument.

SPDF/CDAWeb. Please also acknowledge the data producer: Reiner Friedel at LANL

SPDF/SSCWeb. Please also acknowledge the data producer: Reiner Friedel at LANL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Reiner Friedel at LANL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/90_spa/1992/l0_k0_spa_19920801_v03.cdf. The most common cadence, 61000 [ms] = PT1M1S, occurred for 38.7344% of the 557 timesteps. 

Los Alamos National Laboratory 1990 (from all.xml/observatory/description/@short)

Synchronous Orbit Particle Analyzer (from all.xml/instrument/description/@short)

Los Alamos National Laboratory 1990 (from Master/CDFglobalAttributes/Source_name)

Spacecraft position, geographic (lat., long. (deg), radius (RE))

Electron temperature in 2 energy bands (50-225 keV, 315-1500 keV)

Partial electron densities in 2 energy bands (50-225 keV, 315-1500 keV)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/91_mpa/1993/l1_k0_mpa_19931027_v01.cdf. The most common cadence, 172034 [ms] = PT2M52.034S, occurred for 59.8361% of the 73 timesteps. 

Los Alamos National Laboratory 1991 (from all.xml/observatory/description/@short)

Los Alamos National Laboratory 1991 (from Master/CDFglobalAttributes/Source_name)

[SPECIALIZED USE ONLY] [Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat, Lon)

     Electron, proton and helium measurements are taken every 160 ms from one of the three telescopes according to the following sequence:  T1, T2, T3, T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes again according to the timing and sequence above and summed for 10.24 secondswhich is approximately one spacecraft rotation.  SOPA Key Parameters are normally averaged over three telescopes for ~ 1 minute (6 - 10.24 seconddata accumulation cycles) giving an average over much of the sky.  The time associated with each set of Key Parameters is determined by using the time (in minutes of the day) at the start of each data collection cycle as an indexinto an array of 1440 time slots dividing the day into 1440 one minute intervals.  The time reported is the midpoint of each interval.       We provide six fluxes:        Low energy Protons:  50 keV to 400 keV        High energy Protons: 1.2 MeV to 5 MeV        Low energy Electrons:  50 keV to 225 keV        High energy Electrons: 315 keV to 1.5 MeV        Helium      : ~0.9 MeV to ~1.3 Mev        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,                       and oxygen     We also compute two electron temperatures and densities and two protontemperatures and densities.  These are based on approximately the same energyranges as the fluxes given in above and are determined for relativisticMaxwellian distributions.   Status of SOPA Instrument 1991-080:  Operating normally as of 01-Feb-1993with the following exception.  Detector D1 on Telescope 2 is becoming noisy.This affects proton and ion data from that telescope.  Bad data is disabled thru software in the ground processing and is NOT averaged into the Key parameter data.  Therefore, the parameters given are good but do not cover the same percentage of the sky.   Data is flagged with a data quality flag as follows:   +1 Data is Good    0 Data is Suspect   -1 Data is UnusableLANL personnel should be contacted before using any data tagged as suspect.References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992

Los Alamos Nation Laboratory spacecraft Geosynchronous Orbit Particle Analyzer (SOPA)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/91_spa/1992/l1_k0_spa_19920801_v03.cdf. The most common cadence, 61000 [ms] = PT1M1S, occurred for 37.7778% of the 272 timesteps. 

Los Alamos National Laboratory 1989 (from all.xml/observatory/description/@short)

Los Alamos National Laboratory 1989 (from Master/CDFglobalAttributes/Source_name)

Spacecraft position, geographic (latitude, longitude (deg), radius (RE))

Partial proton densities in 2 energy bands (50-400 keV, 1.2-5.0 MeV)

Heavy Ion flux at ~5 MeV to ~15 MeV (includes carbon, nitrogen, and oxygen

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/94_mpa/1996/l4_k0_mpa_19960101_v03.cdf. The most common cadence, 86016 [ms] = PT1M26.016S, occurred for 75.1788% of the 736 timesteps. 

Los Alamos National Laboratory 1994 (from all.xml/observatory/description/@short)

Los Alamos National Laboratory 1994 (from Master/CDFglobalAttributes/Source_name)

     Electron, proton and helium measurements are taken every 160 ms from one of the three telescopes according to the following sequence:  T1, T2, T3, T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes again according to the timing and sequence above and summed for 10.24 secondswhich is approximately one spacecraft rotation.  SOPA Key Parameters are normally averaged over three telescopes for ~ 1 minute (6 - 10.24 seconddata accumulation cycles) giving an average over much of the sky.  The time associated with each set of Key Parameters is determined by using the time (in minutes of the day) at the start of each data collection cycle as an indexinto an array of 1440 time slots dividing the day into 1440 one minute intervals.  The time reported is the midpoint of each interval.       We provide six fluxes:        Low energy Protons:  50 keV to 400 keV        High energy Protons: 1.2 MeV to 5 MeV        Low energy Electrons:  50 keV to 225 keV        High energy Electrons: 315 keV to 1.5 MeV        Helium      : ~0.9 MeV to ~1.3 Mev        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,                       and oxygen     We also compute two electron temperatures and densities and two protontemperatures and densities.  These are based on approximately the same energyranges as the fluxes given in above and are determined for relativisticMaxwellian distributions.   Status of SOPA Instrument 1994-084:  Operating normally as of 01-Jan-1996   Data is flagged with a data quality flag as follows:   +1 Data is Good    0 Data is Suspect   -1 Data is UnusableLANL personnel should be contacted before using any data tagged as suspect.References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/94_spa/1996/l4_k0_spa_19960216_v01.cdf. The most common cadence, 61000 [ms] = PT1M1S, occurred for 39.7909% of the 571 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/97_h0_mpa/1998/l7_h0_mpa_19980429_v03.cdf. The most common cadence, 86016 [ms] = PT1M26.016S, occurred for 76.8305% of the 766 timesteps. 

Los Alamos National Laboratory 1997 (from all.xml/observatory/description/@short)

Los Alamos National Laboratory 1997 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/97_mpa/1997/l7_k0_mpa_19970704_v02.cdf. The most common cadence, 86016 [ms] = PT1M26.016S, occurred for 95.0000% of the 38 timesteps. 

     Electron, proton and helium measurements are taken every 160 ms from one of the three telescopes according to the following sequence:  T1, T2, T3, T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes again according to the timing and sequence above and summed for 10.24 secondswhich is approximately one spacecraft rotation.  SOPA Key Parameters are normally averaged over three telescopes for ~ 1 minute (6 - 10.24 seconddata accumulation cycles) giving an average over much of the sky.  The time associated with each set of Key Parameters is determined by using the time (in minutes of the day) at the start of each data collection cycle as an indexinto an array of 1440 time slots dividing the day into 1440 one minute intervals.  The time reported is the midpoint of each interval.       We provide six fluxes:        Low energy Protons:  50 keV to 400 keV        High energy Protons: 1.2 MeV to 5 MeV        Low energy Electrons:  50 keV to 225 keV        High energy Electrons: 315 keV to 1.5 MeV        Helium      : ~0.9 MeV to ~1.3 Mev        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,                       and oxygen     We also compute two electron temperatures and densities and two protontemperatures and densities.  These are based on approximately the same energyranges as the fluxes given in above and are determined for relativisticMaxwellian distributions.   Status of SOPA Instrument LANL-97A:  Operating normally as of 01-Jul-1997   Data is flagged with a data quality flag as follows:   +1 Data is Good    0 Data is Suspect   -1 Data is UnusableLANL personnel should be contacted before using any data tagged as suspect.References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/97_spa/1999/l7_k0_spa_19990101_v01.cdf. The most common cadence, 61000 [ms] = PT1M1S, occurred for 40.2227% of the 578 timesteps. 

LANL 1989-046 Magnetospheric Plasma Analyzer High Resolution data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/89_h0_mpa/1998/l9_h0_mpa_19980503_v03.cdf. The most common cadence, 86018 [ms] = PT1M26.018S, occurred for 70.5036% of the 98 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/89_mpa/1993/l9_k0_mpa_19930315_v01.cdf. The most common cadence, 172036 [ms] = PT2M52.036S, occurred for 36.7615% of the 168 timesteps. 

[SPECIALIZED USE ONLY] [Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat.,Lon.)

     Electron, proton and helium measurements are taken every 160 ms from one of the three telescopes according to the following sequence:  T1, T2, T3, T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes again according to the timing and sequence above and summed for 10.24 secondswhich is approximately one spacecraft rotation.  SOPA Key Parameters are normally averaged over three telescopes for ~ 1 minute (6 - 10.24 seconddata accumulation cycles) giving an average over much of the sky.  The time associated with each set of Key Parameters is determined by using the time (in minutes of the day) at the start of each data collection cycle as an indexinto an array of 1440 time slots dividing the day into 1440 one minute intervals.  The time reported is the midpoint of each interval.       We provide six fluxes:        Low energy Protons:  50 keV to 400 keV        High energy Protons: 1.2 MeV to 5 MeV        Low energy Electrons:  50 keV to 225 keV        High energy Electrons: 315 keV to 1.5 MeV        Helium      : ~0.9 MeV to ~1.3 Mev        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,                       and oxygen     We also compute two electron temperatures and densities and two protontemperatures and densities.  These are based on approximately the same energyranges as the fluxes given in above and are determined for relativisticMaxwellian distributions.   Status of SOPA Instrument 1989-046:  Operating normally as of 01-Feb-1993   Data is flagged with a data quality flag as follows:   +1 Data is Good    0 Data is Suspect   -1 Data is UnusableLANL personnel should be contacted before using any data tagged as suspect.References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/lanl/89_spa/1992/l9_k0_spa_19920801_v03.cdf. The most common cadence, 61000 [ms] = PT1M1S, occurred for 38.1085% of the 548 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/mars_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/mars_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/helio1day/maven_helio1day_position_20131119_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 6251 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/helio1hr/maven_helio1hr_position_20131119_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 97751 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/mercury_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/mercury_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/messenger/helio1day/messenger_helio1day_position_20040805_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 3921 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/messenger/helio1hr/messenger_helio1hr_position_20040804_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 94127 timesteps. 

MESSENGER interplanetary magnetic field (1-second/high resolution) in RTN coordinates

The Mercury Surface, Space Environment, Geochemistry and Ranging (MESSENGER) mission is designed to study the characteristics and environment of Mercury from orbit. Specifically, the scientific objectives of the mission are to characterize the chemical composition of Mercury's surface, the geologic history, the nature of the magnetic field, the size and state of the core, the volatile inventory at the poles, and the nature of Mercurys exosphere and magnetosphere over a nominal orbital mission of one Earth yearMESSENGER launched on 3 August 2004 at 6:15:56 UT (2:15:56 a.m. EDT) on a Delta 7925H (a Delta II Heavy launch vehicle with nine strap-on solid-rocket boosters). The spacecraft was injected into solar orbit 57 minutes later.  The solar panels were then deployed and the spacecraft began sending data on its status. One year after launch, on 2 August 2005, MESSENGER flew by Earth at an altitude of 2347 km. On 12 December 2005 at 11:30 UT, MESSENGER fired its large thruster for 524 seconds, changing the spacecraft velocity by 316 m/s and putting it on course for its 24 October 2006 Venus flyby at an altitude of 2990 km. The second Venus flyby took place on 5 June 2007 at 23:08 UT (7:08 p.m. EDT) at an altitude of approximately 337 km. The first of three Mercury flybys, all at roughly 200 km altitude, occurred on 14 January 2008 at 19:04:39 UT, and the second on 6 October 2008 at 08:40:22 UT.  The third will be on 29 September 2009. There are also five deep space manuevers. Data collected during the Mercury flybys will be used to help plan the scientific campaign during the orbital phase. Mercury orbit insertion will take place on 18 March 2011, requiring a delta-V of 0.867 km/s. The nominal orbit is planned to have a periapsis of 200 km at 60 degrees N latitude, an apoapsis of 15,193 km, a period of 12 hours and an inclination of 80 degrees. The periapsis will slowly rise due to solar perturbations to over 400 km at the end of 88 days (one Mercury year) at which point it will be readjusted to a 200 km, 12 hour orbit via a two burn sequence. Data will be collected from orbit for one Earth year, the nominal end of the primary mission will be in March 2012.  Global stereo image coverage at 250 m/pixel resolution is expected. The mission should also yield global composition maps, a 3-D model of Mercury's magnetosphere, topographic profiles of the northern hemisphere, gravity field to degree and order 16, altitude profiles of elemental species, and a characterization of the volatiles in permanently shadowed craters at the poles.The MESSENGER spacecraft is a squat box (1.27 m x 1.42 m x 1.85 m) with a semi-cylindrical thermal shade (roughly 2.5 meters tall and 2 meters wide) for protection from the Sun and two solar panel wings extending radially about 6 meters from tip to tip.  A 3.6 m magnetometer boom also extends from the craft. The total mass of the spacecraft is 1093 kg, 607.8 kg of this is propellant and helium. The structure is primarily graphite-cyanate-ester (GrCE) composite and consists of two vertical panels which support two large fuel tanks and two vertical panels which support the oxidizer tank and plumbing panel. The four vertical panels make up the center column and are bolted at their aft ends to an aluminum adapter. A single top deck panel mounts the LVA (large velocity adjust) thruster, small thrusters, helium and auxiliary fuel tanks, star trackers and battery.Main propulsion is via the 645-N, 317-s bipropellant LVA thruster, four 22-N monopropellant thrusters provide spacecraft steering during main thruster burns, and ten 4-N monopropellant thrusters are used for attitude control. There is also a reaction-wheel attitude control system. Knowledge for attitude control is provided by star tracking cameras, an inertial measurement unit, and six solar sensors. Power is provided by the solar panels, which extend beyond the sunshade and are rotatable to balance panel temperature and power generation, which provides a nominal 450 W in Mercury orbit. The panels are 70% optical solar reflectors and 30% GaAs/Ge cells. The power is stored in a common-pressure-vessel nickel-hydrogen battery, with 11 vessels and 2 cells per vessel.Communications are in X-band with downlink through two fixed phased-array antenna clusters and uplink and downlink through medium- and low-gain antennas on the forward and aft sides of the spacecraft. Passive thermal control, primarily a fixed opaque ceramic cloth sunshade, is utilized to maintain operating temperatures near the Sun. Radiators are built into the structure and the orbit is optimized to minimize infrared and visible light heating of the spacecraft from the surface of Mercury. Multilayer insulation, low conductivity couplings, and heaters are also used to maintain temperatures within operating limits.Five science instruments are mounted externally on the bottom deck of the main body: the Mercury Dual Imaging System (MDIS), Gamma-Ray and Neutron Spectrometer (GRNS), X-ray Spectrometer (XRS), Mercury Laser Altimeter (MLA), and Atmospheric and Surface Composition Spectrometer (MASCS). The Energetic Particle and Plasma Spectrometer (EPPS) is mounted on the side and top deck and the magnetometer (MAG) is at the end of the 3.6 m boom. Radio Science (RS) experiments will use the existing communications system.The Messenger MAG instrument is a miniature three-axis ring-core fluxgate magnetometer with low-noise electronics. It is mounted on a 3.6 m boom in the anti-sunward direction. The MAG has .. 1530 and ..51300 nT ranges with 20-bit internal resolution and 17-bit output resolution. The MAG probe samples magnetic field values along the X, Y, and Z axes at a rate of up to 20 samples/second (commandable and can vary). This dataset has 3-axis calibrated samples of the magnetic field in heliospheric RTN coordinates in units of nano-Tesla, Br, Bt, Bn. The spacecraft position is identified by radial distance from the Sun, latitude above the ecliptic plane, and azimuth with respect to the Earth-Sun line in the ecliptic plane. Anderson, B. J., M. H. Acuna, D. A. Lohr , J. Scheifele, A. Raval, H. Korth, and J. A. Slavin, \'The Magnetometer instrument on MESSENGER\', Space Science Reviews, 2007.[ANDREWSETAL2007]

MESSENGER Magnetometer, MAG, calibrated data. This volume contains the MAG data from Earth to Mercury over the time interval 2004-08-12 to 2015-04-30, hosted by the Planetary Data System, Planetary Plasma Interactions node, PSD-PPI.

General information concerning the MESSENGER, Magnetometer, MAG, instrument

The MESSENGER Magnetometer, MAG, calibrated observations consist of time and position tagged magnetic field samples in physical units and coordinate systems collected by the MAG instrument during fly-by and orbital operations of Mercury. See information given for time intervals more likely to have data quality issues.

MESSENGER Magnetometer, MAG, instrument, Space Science Reviews publication

Anderson, B.J., M.H. Acuna, D.A. Lohr, J. Scheifele, A. Raval, H. Korth, and J.A. Slavin, The Magnetometer instrument on MESSENGER, Space Sci. Rev., 2007, DOI: 10.1007/s11214-007-9246-7.

SPDF/CDAWeb. Please also acknowledge the data producer: Prof. Sean C. Solomon at Carnegie Institution of Washington

SPDF/SSCWeb. Please also acknowledge the data producer: Prof. Sean C. Solomon at Carnegie Institution of Washington

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Prof. Sean C. Solomon at Carnegie Institution of Washington

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_200.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_200.)

Magnetic Field instrument (from all.xml/instrument/description/@short)

Field in RTN coordinates (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/messenger/mag/rtn_cdf/2004/messenger_mag_rtn_20040812_v01.cdf. The most common cadence, 50 [ms] = PT0.05S, occurred for 99.8280% of the 431717 timesteps. 

----> Azimuthal angle from Earth-Sun line in ecliptic plane, positive in the direction of Earth's motion 

3-digit daily quality flag (222 or 223 = good = boom deployed, sensor in shadow, any heater contamination corrected)

----> Azimuthal angle from Earth-Sun line in ecliptic plane, positive in the direction of Earth's motion (0.5 sec cadence)

(Good values at 0.5 sec cadence only) B radial (Br) in RTN coordinates 

POES-SEM2 2-second Particle Precipitation Data, MetOp-B (MetOp-1 before Sept2012 launch) [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

POES N19 data: POES/MetOp: Particle Precipitation Data (These data have known contamination problems. Please consult provider rob.redmon@noaa.gov for usage recommendations.) 

MEPED Telescope Data Processing Algorithm Theoretical Basis Document (section 2.2.1)

Archive and Instrument Documentation at NOAA National Geophysical Data Center (NGDC)

MEPED Telescope Data Processing Algorithm Theoretical Basis Document, Section 2.2.1

POES/MetOp: Particle Precipitation Data (These data have known contamination problems. Please consult provider rob.redmon@noaa.gov for usage recommendations.) 

SPDF/CDAWeb. Please also acknowledge the data producer: NGDC and SWPC at NOAA

SPDF/SSCWeb. Please also acknowledge the data producer: NGDC and SWPC at NOAA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: NGDC and SWPC at NOAA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/metop1/sem2_fluxes-2sec/2012/metop1_poes-sem2_fluxes-2sec_20121003_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.8896% of the 42530 timesteps. 

POES-Space Environment Monitor 2 (from all.xml/instrument/description/@short)

Electron differential flux, TED, 0 degree telescope, 189-7980 eV

Electron differential flux, TED, 0 and 30 degree telescopes, 189 eV

Proton differential flux, TED, 0 and 30 degree telescopes, 189 eV

Electron integral energy flux, TED, 0 degree telescope, low energy (50-1000 eV)

Electron integral energy flux, TED, 0 degree telescope, high energy (1-20 keV)

Proton integral energy flux, TED, 0 degree telescope, low energy (50-1000 eV)

Proton integral energy flux, TED, 0 degree telescope, high energy (1-20 keV)

Electron atmospheric integral energy flux, TED, low energy (50-1000 eV), at 120 km

Proton atmospheric integral energy flux, TED, low energy (50-1000 eV), at 120 km

Electron and Proton total atmospheric integral energy flux, TED, at 120 km

Electron background integral energy flux, TED, 0 degree telescope, low energy

Proton background integral energy flux, TED, 0 degree telescope, low energy

Electron integral flux, MEPED, 0 degree telescope, >40 to >612 keV

Electron integral flux, MEPED, 90 degree telescope, >40 to >612 keV

Electron integral flux, MEPED, 0 and 90 degree telescopes, >40 keV

Proton differential flux, MEPED, 0 degree telescope, 39-2723 keV

Proton differential flux, MEPED, 90 degree telescope, 39-2723 keV

Proton differential flux, MEPED, 0 and 90 degree telescopes, 39 keV

Proton integral flux, MEPED, 0 and 90 degree telescopes, >6174 keV 

---> By IGRF satellite coordinates (opposite velocity direction)

POES-SEM2 2-second Particle Precipitation Data, MetOp-A (MetOp-2 before Oct2006 launch) [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/metop2/sem2_fluxes-2sec/2012/metop2_poes-sem2_fluxes-2sec_20120622_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.4968% of the 2768 timesteps. 

POES-SEM2 2-second Particle Precipitation Data, MetOp-C (MetOp-3 launched 07 November 2018) [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

SPDF/CDAWeb. Please also acknowledge the data producer: NCEI at NOAA

SPDF/SSCWeb. Please also acknowledge the data producer: NCEI at NOAA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: NCEI at NOAA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/metop3/sem2_fluxes-2sec/2019/metop3_poes-sem2_fluxes-2sec_20190101_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.8819% of the 43147 timesteps. 

The Mars Global Surveyor magnetic field instrument consists of dual, triaxial fluxgate magnetometers, capable of measuring fields between +/- 4 nT and +/- 65536 nT. Automated range switching allows the instrument to maintain maximum digital resolution over a wide range of field strengths. The text of this instrument description has been abstracted from the   instrument paper:  Acuna, M. A., J. E. P. Connerney, P. Wasilewski, R. P. Lin,     K. A. Anderson, C. W. Carlson, J. McFadden, D. W. Curtis, H. Reme,  A. Cros, J. L. Medale, J. A. Sauvaud, C. d'Uston, S. J. Bauer,  P. Cloutier, M. Mayhew, and N. F. Ness, Mars Observer Magnetic   Fields Investigation, J. Geophys. Res., 97, 7799-7814, 1992. 

Much of the information provided in this meta data originates from text files provided at: https://pds-ppi.igpp.ucla.edu/search/?sc=Mars%20Global%20Surveyor&i=MAG within the CATALOG folder and the AAREADME.txt files.  The development of the netCDF files was supported by the NASA Postdoctoral Program Fellowship awarded to Teresa Esman in 2022.  The success of the MGS MAG project is owed to, among others, the people listed here: https://mars.nasa.gov/mgs/people/.  Addtional information on the MAG dataset can be found at: https://mgs-mager.gsfc.nasa.gov/status.html. Documentation on MGS MAG data on the PDS has been maintained by J.E.P. Connerney, Mark Sharlow, D. Kazden, J. Springborn, and B. Semenov, among others.  Teresa Esman, now a NPP Fellow at NASA Goddard Space Flight Center, compiled MGS MAG low resolution and high resolution data products, translated time to unix time, and performed the  calculation and interpolation (to high resolution) of the altitude data product.

MGS MAG magnetic field .STS files from 1997-09-12 through 2006-11-02 are avalible at

SPDF/CDAWeb. Please also acknowledge the data producer: M. Acuna at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: M. Acuna at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M. Acuna at NASA/GSFC

Mars Global Surveyor (from all.xml/observatory/description/@short)

Magnetospheric Science, Ionospheric Science (from Master/CDFglobalAttributes/Discipline)

Mars Global Surveyor (from Master/CDFglobalAttributes/Source_name)

The Magnetospheric Multiscale (MMS) Mission home page hosted by the Laboratory of Atmospheric and Space Physics, Science Data Center (LASP, SDC) at the University of Colorado, Boulder.

The Magnetospheric Multiscale (MMS) Mission home page at Goddard Space Flight Center (GSFC)

The Magnetospheric Multiscale (MMS) Mission Home Page hosted by the Goddard Space Flight Center (GSFC).

The Magnetospheric Multiscale (MMS) ASPOC home page hosted by the Graz ASPOC team located at the Institut fur Weltraumforschung (IWF), Osterreichische Akademie der Wissenschaften (OAW).

SPDF/CDAWeb. Please also acknowledge the data producer: K. Torkar, R. Nakamura at IWF

SPDF/SSCWeb. Please also acknowledge the data producer: K. Torkar, R. Nakamura at IWF

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Torkar, R. Nakamura at IWF

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/aspoc/srvy/l2/2015/09/mms1_aspoc_srvy_l2_20150901_v2.0.0.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

MMS Satellite Number 1 (from all.xml/observatory/description/@short)

MMS Satellite Number 1 (from Master/CDFglobalAttributes/Source_name)

SCM Low frequency Magnetic spectral density from the FIELDS Digital Signal Processor

BPSD is the low frequency B spectral density covering the frequency range of .2 to 6000 Hz.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, R. Ergun, O. Le Contel at SWRI, LASP, LPP

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, R. Ergun, O. Le Contel at SWRI, LASP, LPP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, R. Ergun, O. Le Contel at SWRI, LASP, LPP

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/dsp/fast/l2/bpsd/2015/09/mms1_dsp_fast_l2_bpsd_20150901_v2.1.1.cdf. The most common cadence, 2000024736 [ns] = PT2.000025S, occurred for 1.1884% of the 300 timesteps. 

Digital Signal Processor (from all.xml/instrument/description/@short)

SCM B Spectral Density (from Master/CDFglobalAttributes/Data_type)

SCM Axis 2 (Y, ~direction of S/C Z) component magnetic power spectral density

Omni-directional magnetic power spectral density: square root of the sum of the squares of 3 components

Low and medium frequency Electric Field spectral density from the FIELDS Digital Signal Processor

EPSD combines the low frequency E spectral density covering the frequency range of 1 to 8000 Hz and the  medium frequency E spectral density covering the frequency range of .25 to 100 kHz.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, R. Ergun at SWRI, LASP

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, R. Ergun at SWRI, LASP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, R. Ergun at SWRI, LASP

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/dsp/fast/l2/epsd/2015/09/mms1_dsp_fast_l2_epsd_20150901_v0.6.4.cdf. The most common cadence, 2000024736 [ns] = PT2.000025S, occurred for 1.1884% of the 300 timesteps. 

Fast Mode L2 E Spectral Density (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/dsp/slow/l2/bpsd/2015/09/mms1_dsp_slow_l2_bpsd_20150901_v2.1.0.cdf. The most common cadence, 16000183019 [ns] = PT16.000183S, occurred for 1.7881% of the 40 timesteps. 

SCM2 component magnetic power spectral density - NO DATA in Slow Survey

Omni-directional magnetic power spectral density: square root of the sum of the squares of 2 components

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/dsp/slow/l2/epsd/2015/09/mms1_dsp_slow_l2_epsd_20150901_v0.6.4.cdf. The most common cadence, 16000183019 [ns] = PT16.000183S, occurred for 1.7873% of the 40 timesteps. 

The Magnetospheric Multiscale (MMS) FIELDS Instrument Suite home page. The web page is hosted by the University of New Hampshire (UNH).

SPDF/CDAWeb. Please also acknowledge the data producer: Roy Torbert, Hans Vaith at UNH

SPDF/SSCWeb. Please also acknowledge the data producer: Roy Torbert, Hans Vaith at UNH

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Roy Torbert, Hans Vaith at UNH

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_timetag, @1 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_timetag, @1 => Epoch.)

Burst L2 Ambient Electron Flux (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/amb/2015/09/mms1_edi_brst_l2_amb_20150901121114_v3.1.1.cdf. The most common cadence, 1000012000 [ns] = PT1.000012S, occurred for 51.8135% of the 300 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/amb/2015/09/mms1_edi_brst_l2_amb_20150901121114_v3.1.1.cdf. The most common cadence, 976563 [ns] = PT0.000976563S, occurred for 50.0001% of the 296960 timesteps. 

Trajectory of flux1 0-degree pitch angle electrons in GSE coordinates.

---> Trajectory of flux2 0-degree pitch angle electrons in GSE coordinates.

---> Trajectory of flux3 0-degree pitch angle electrons in GSE coordinates.

---> Trajectory of flux4 0-degree pitch angle electrons in GSE coordinates.

Trajectory of flux1 180-degree pitch angle electrons in GSE coordinates.

---> Trajectory of flux2 180-degree pitch angle electrons in GSE coordinates.

---> Trajectory of flux3 180-degree pitch angle electrons in GSE coordinates.

---> Trajectory of flux4 180-degree pitch angle electrons in GSE coordinates.

Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates.

---> Trajectory of flux2 0-degree pitch angle electrons in GSM coordinates.

---> Trajectory of flux3 0-degree pitch angle electrons in GSM coordinates.

---> Trajectory of flux4 0-degree pitch angle electrons in GSM coordinates.

Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates.

---> Trajectory of flux2 180-degree pitch angle electrons in GSM coordinates.

---> Trajectory of flux3 180-degree pitch angle electrons in GSM coordinates.

---> Trajectory of flux4 180-degree pitch angle electrons in GSM coordinates.

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates.

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/amb-pm2/2016/01/mms1_edi_brst_l2_amb-pm2_20160114204504_v4.1.0.cdf. The most common cadence, 1000012535 [ns] = PT1.000013S, occurred for all 168 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/amb-pm2/2016/01/mms1_edi_brst_l2_amb-pm2_20160114204504_v4.1.0.cdf. The most common cadence, 976575 [ns] = PT0.000976575S, occurred for 74.2059% of the 128417 timesteps. 

---> Error in field-aligned electron flux from channel 1 of both GDUs.

---> Error in anti-field-aligned electron flux from channel 1 of both GDUs.

---> Error in field-aligned electron flux from channel 2 of both GDUs.

---> Error in anti-field-aligned electron flux from channel 2 of both GDUs.

---> Error in field-aligned electron flux from channel 3 of both GDUs.

---> Error in anti-field-aligned electron flux from channel 3 of both GDUs.

---> Error in field-aligned electron flux from channel 4 of both GDUs.

---> Error in anti-field-aligned electron flux from channel 4 of both GDUs.

Trajectory of field-aligned electrons from channel 1 of both GDUs in GSE coordinates.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs, in GSE coordinates.

Trajectory of field-aligned electrons from channel 2 of both GDUs in GSE coordinates.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs, in GSE coordinates.

Trajectory of field-aligned electrons from channel 3 of both GDUs in GSE coordinates.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs, in GSE coordinates.

Trajectory of field-aligned electrons from channel 4 of both GDUs in GSE coordinates.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs, in GSE coordinates.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates.

SPDF/CDAWeb. Please also acknowledge the data producer: Hans Vaith at UNH

SPDF/SSCWeb. Please also acknowledge the data producer: Hans Vaith at UNH

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Hans Vaith at UNH

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/efield/2015/09/mms1_edi_brst_l2_efield_20150914141304_v1.5.0.cdf. The most common cadence, 5000000000 [ns] = PT5S, occurred for 38.8889% of the 14 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_timetag, @1 => epoch_gdu1, @2 => epoch_gdu2.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_timetag, @1 => epoch_gdu1, @2 => epoch_gdu2.)

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/q0/2016/04/mms1_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 1000011000 [ns] = PT1.000011S, occurred for 46.4286% of the 13 timesteps. 

Counts based on variable 'epoch_gdu1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/q0/2016/04/mms1_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 95.7488% of the 3446 timesteps. 

GDU1 electron incident trajectory vectors in spherical BCS coordinates.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates.

GDU1 electron incident trajectory vectors in spherical GSE coordinates.

GDU1 electron incident trajectory vectors in spherical GSM coordinates.

Counts based on variable 'epoch_gdu2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/brst/l2/q0/2016/04/mms1_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 94.3785% of the 3341 timesteps. 

GDU2 Electron incident trajectory vectors in spherical BCS coordinates.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates.

Survey L2 Ambient Electron Flux (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/srvy/l2/amb/2015/09/mms1_edi_srvy_l2_amb_20150901_v4.1.0.cdf. The most common cadence, 4000049472 [ns] = PT4.000049S, occurred for 7.1161% of the 759 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/srvy/l2/amb/2015/09/mms1_edi_srvy_l2_amb_20150901_v4.1.0.cdf. The most common cadence, 31250386 [ns] = PT0.03125S, occurred for 11.5902% of the 158250 timesteps. 

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates.

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/srvy/l2/amb-pm2/2016/01/mms1_edi_srvy_l2_amb-pm2_20160106_v2.1.1.cdf. The most common cadence, 4000052288 [ns] = PT4.000052S, occurred for 98.1132% of the 156 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/srvy/l2/amb-pm2/2016/01/mms1_edi_srvy_l2_amb-pm2_20160106_v2.1.1.cdf. The most common cadence, 31250000 [ns] = PT0.03125S, occurred for 94.5359% of the 19360 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edi/srvy/l2/efield/2015/09/mms1_edi_srvy_l2_efield_20150901_v1.6.2.cdf. The most common cadence, 9728105856 [ns] = PT9.728106S, occurred for 0.0823% of the 1 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: J.Burch, R.Ergun, P.Lindqvist. at SWRI, LASP, KTH

SPDF/SSCWeb. Please also acknowledge the data producer: J.Burch, R.Ergun, P.Lindqvist. at SWRI, LASP, KTH

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.Burch, R.Ergun, P.Lindqvist. at SWRI, LASP, KTH

Counts based on variable 'mms1_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/brst/l2/dce/2015/09/mms1_edp_brst_l2_dce_20150901121114_v2.2.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 74.1173% of the 3521579 timesteps. 

Electric Double Probe (from all.xml/instrument/description/@short)

Burst Mode L2 DC Efields (from Master/CDFglobalAttributes/Data_type)

L2 DC E Field (GSE coords) calibrated for SDP and ADP, all flag values included

L2 DC E Field (DSL coords) calibrated for SDP and ADP, all flag values included

Quality indicator (3 good), (2 ok data, use with some caution), (1 bad data, use with caution), (0 Really bad data or no data at all)

SPDF/CDAWeb. Please also acknowledge the data producer: Burch, J, Ergun, R., Lindqvist, P. at SwRI, LASP, KTH

SPDF/SSCWeb. Please also acknowledge the data producer: Burch, J, Ergun, R., Lindqvist, P. at SwRI, LASP, KTH

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Burch, J, Ergun, R., Lindqvist, P. at SwRI, LASP, KTH

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/brst/l2/hmfe/2015/09/mms1_edp_brst_l2_hmfe_20150901121114_v1.0.1.cdf. The most common cadence, 15259 [ns] = PT0.000015259S, occurred for 96.7379% of the 9763313 timesteps. 

Axial Double Probe- Spin Plane Double Probe (from all.xml/instrument/description/@short)

http://mms.gsfc.nasa.gov/The full name of PI affiliations: SWRI - Southwest Research Institute. LASP - Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan (Swedish Royal Institute of Technology). 

Counts based on variable 'mms1_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/brst/l2/scpot/2015/09/mms1_edp_brst_l2_scpot_20150901121114_v2.4.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 74.1173% of the 3521579 timesteps. 

Counts based on variable 'mms1_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/fast/l2/dce/2015/09/mms1_edp_fast_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 31250375 [ns] = PT0.03125S, occurred for 71.7507% of the 1159491 timesteps. 

Fast Mode L2 DC Efields (from Master/CDFglobalAttributes/Data_type)

Approximate DC E field error derived from SDP (quality and bitmask) and ADP (residue)

Counts based on variable 'mms1_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/fast/l2/scpot/2015/09/mms1_edp_fast_l2_scpot_20150901000000_v2.7.2.cdf. The most common cadence, 31250375 [ns] = PT0.03125S, occurred for 71.7507% of the 1159491 timesteps. 

Counts based on variable 'mms1_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/slow/l2/dce/2015/09/mms1_edp_slow_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 125001496 [ns] = PT0.125001S, occurred for 94.6788% of the 271644 timesteps. 

Slow Mode L2 DC Efields (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'mms1_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/slow/l2/scpot/2015/09/mms1_edp_slow_l2_scpot_20150901000000_v2.7.1.cdf. The most common cadence, 125001496 [ns] = PT0.125001S, occurred for 94.6788% of the 271644 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/edp/srvy/l2/hfesp/2015/09/mms1_edp_srvy_l2_hfesp_20150901_v0.4.0.cdf. The most common cadence, 16000198016 [ns] = PT16.000198S, occurred for 4.7795% of the 258 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: B. Mauk at JHU/APL

SPDF/SSCWeb. Please also acknowledge the data producer: B. Mauk at JHU/APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: B. Mauk at JHU/APL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/epd-eis/brst/l2/extof/2015/09/mms1_epd-eis_brst_l2_extof_20150901121114_v3.0.0.cdf. The most common cadence, 604749918 [ns] = PT0.60475S, occurred for 20.4807% of the 196 timesteps. 

Energetic Ion Spectrometer (from all.xml/instrument/description/@short)

---> Quality Word. Note: CDF_UINT4 data was converted to HAPI double.

MMS1 ExTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Burst proton_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst proton_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst proton_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst oxygen_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst oxygen_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst oxygen_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst helium_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst helium_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst helium_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst alpha_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst alpha_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst alpha_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst dump_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst dump_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 ExTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 ExTOF-Burst dump_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

Valid Time of Flight by Pulse Height Energy Events per second MMS1

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/epd-eis/brst/l2/phxtof/2015/09/mms1_epd-eis_brst_l2_phxtof_20150901121114_v3.0.0.cdf. The most common cadence, 604749918 [ns] = PT0.60475S, occurred for 20.4807% of the 196 timesteps. 

MMS1 PhxTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Burst proton_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst proton_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst proton_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst oxygen_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst oxygen_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst oxygen_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst dump_P5_counts_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst dump_P5_cps_t0 [data available from 2019/12/06 to 2025/01/06]

MMS1 PhxTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/05]

MMS1 PhxTOF-Burst dump_P5_flux_t0 [data available from 2019/12/06 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/epd-eis/srvy/l2/electronenergy/2015/09/mms1_epd-eis_srvy_l2_electronenergy_20150901_v3.0.0.cdf. The most common cadence, 2418874979 [ns] = PT2.418875S, occurred for 23.2830% of the 8316 timesteps. 

srvy_L2_ElectronEnergy (from Master/CDFglobalAttributes/Data_type)

Quality Word. Note: CDF_UINT4 data was converted to HAPI double.

MMS1 ElectronEnergy-Survey electron_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ElectronEnergy-Survey electron_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ElectronEnergy-Survey electron_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ElectronEnergy-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ElectronEnergy-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ElectronEnergy-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ElectronEnergy-Survey electron_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 ElectronEnergy-Survey electron_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 ElectronEnergy-Survey electron_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 ElectronEnergy-Survey electron_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 ElectronEnergy-Survey electron_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 ElectronEnergy-Survey electron_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 ElectronEnergy-Survey electron_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ElectronEnergy-Survey electron_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ElectronEnergy-Survey electron_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ElectronEnergy-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ElectronEnergy-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 ElectronEnergy-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 ElectronEnergy-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ElectronEnergy-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 ElectronEnergy-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 ElectronEnergy-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ElectronEnergy-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 ElectronEnergy-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/epd-eis/srvy/l2/extof/2015/09/mms1_epd-eis_srvy_l2_extof_20150901_v3.0.0.cdf. The most common cadence, 2418874979 [ns] = PT2.418875S, occurred for 22.4458% of the 5097 timesteps. 

MMS1 ExTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 ExTOF-Survey proton_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey proton_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey proton_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey oxygen_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey oxygen_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey oxygen_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey helium_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey helium_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey helium_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey alpha_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey alpha_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey alpha_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey dump_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey dump_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS1 ExTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 ExTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS1 ExTOF-Survey dump_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/epd-eis/srvy/l2/phxtof/2015/09/mms1_epd-eis_srvy_l2_phxtof_20150901_v3.0.0.cdf. The most common cadence, 2418874979 [ns] = PT2.418875S, occurred for 22.4546% of the 5099 timesteps. 

MMS1 PhxTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS1 PhxTOF-Survey proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS1 PhxTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS1 PhxTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS1 PhxTOF-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

SPDF/CDAWeb. Please also acknowledge the data producer: STP at LASP

SPDF/SSCWeb. Please also acknowledge the data producer: STP at LASP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: STP at LASP

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/feeps/brst/l2/electron/2015/09/mms1_feeps_brst_l2_electron_20150901121114_v7.1.1.cdf. The most common cadence, 302383872 [ns] = PT0.302384S, occurred for 25.5608% of the 490 timesteps. 

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 1

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 2

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 3

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 4

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 5

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 9

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 10

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 11

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 12

MMS1 FEEPS top side burst mode electron count error statistics sensor 1

MMS1 FEEPS top side burst mode electron count error statistics sensor 2

MMS1 FEEPS top side burst mode electron count error statistics sensor 3

MMS1 FEEPS top side burst mode electron count error statistics sensor 4

MMS1 FEEPS top side burst mode electron count error statistics sensor 5

MMS1 FEEPS top side burst mode electron count error statistics sensor 9

MMS1 FEEPS top side burst mode electron count error statistics sensor 10

MMS1 FEEPS top side burst mode electron count error statistics sensor 11

MMS1 FEEPS top side burst mode electron count error statistics sensor 12

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 1

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 2

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 3

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 4

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 5

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 9

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 10

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 11

MMS1 FEEPS bottom side burst mode electron count error statistics sensor 12

The angle formed by the normal vector of the sensor plane and the magnetic field (BField)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/feeps/brst/l2/ion/2015/09/mms1_feeps_brst_l2_ion_20150901121114_v7.1.1.cdf. The most common cadence, 302383872 [ns] = PT0.302384S, occurred for 25.5608% of the 490 timesteps. 

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 6

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 7

Quality Indicator (0=VALID FOR SCIENCE, 1=CAUTION, 2=PROBLEMATIC, 3=NOT VALID FOR SCIENCE, 4=CALIBRATION) sensor 8

MMS1 FEEPS top side burst mode ion count error statistics sensor 6

MMS1 FEEPS top side burst mode ion count error statistics sensor 7

MMS1 FEEPS top side burst mode ion count error statistics sensor 8

MMS1 FEEPS bottom side burst mode ion count error statistics sensor 6

MMS1 FEEPS bottom side burst mode ion count error statistics sensor 7

MMS1 FEEPS bottom side burst mode ion count error statistics sensor 8

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/feeps/srvy/l2/electron/2015/09/mms1_feeps_srvy_l2_electron_20150901000000_v7.1.1.cdf. The most common cadence, 2418976000 [ns] = PT2.418976S, occurred for 5.3649% of the 1271 timesteps. 

MMS1 FEEPS bottom side survey mode electron count rate sensor 10

MMS1 FEEPS bottom side survey mode electron count rate sensor 11

MMS1 FEEPS bottom side survey mode electron count rate sensor 12

MMS1 FEEPS top side survey mode electron count error statistics sensor 1

MMS1 FEEPS top side survey mode electron count error statistics sensor 2

MMS1 FEEPS top side survey mode electron count error statistics sensor 3

MMS1 FEEPS top side survey mode electron count error statistics sensor 4

MMS1 FEEPS top side survey mode electron count error statistics sensor 5

MMS1 FEEPS top side survey mode electron count error statistics sensor 9

MMS1 FEEPS top side survey mode electron count error statistics sensor 10

MMS1 FEEPS top side survey mode electron count error statistics sensor 11

MMS1 FEEPS top side survey mode electron count error statistics sensor 12

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 1

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 2

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 3

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 4

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 5

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 9

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 10

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 11

MMS1 FEEPS bottom side survey mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/feeps/srvy/l2/ion/2015/09/mms1_feeps_srvy_l2_ion_20150901000000_v7.1.1.cdf. The most common cadence, 2418976000 [ns] = PT2.418976S, occurred for 5.3649% of the 1271 timesteps. 

MMS1 FEEPS top side survey mode ion count error statistics sensor 6

MMS1 FEEPS top side survey mode ion count error statistics sensor 7

MMS1 FEEPS top side survey mode ion count error statistics sensor 8

MMS1 FEEPS bottom side survey mode ion count error statistics sensor 6

MMS1 FEEPS bottom side survey mode ion count error statistics sensor 7

MMS1 FEEPS bottom side survey mode ion count error statistics sensor 8

Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 1

The Magnetospheric Multiscale (MMS) Flux Gate Magnetometer (FGM) home page hosted by the Institut fur Weltraumforschung (IWF), Osterreichische Akademie der Wissenschaften (OAW).

See MMS Data Rights and Rules for Use https://lasp.colorado.edu/galaxy/display/mms/MMS+Data+Rights+and+Rules+for+Data+Use

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, C. Russell, W. Magnus at SWRI, UCLA, IWF

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, C. Russell, W. Magnus at SWRI, UCLA, IWF

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, C. Russell, W. Magnus at SWRI, UCLA, IWF

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_state.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_state.)

Flux Gate Magnetometer (from all.xml/instrument/description/@short)

Magnetic field vector in Geocentric Solar Ecliptic (GSE) cartesian coordinates plus Btotal (128 S/s)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fgm/brst/l2/2015/09/mms1_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 7812591 [ns] = PT0.007813S, occurred for 67.7649% of the 50308 timesteps. 

---> Magnetic field vector in Geocentric Solar Ecliptic (GSE) cartesian coordinates plus Btotal (8 or 16 S/s), including flagged data

Magnetic field vector in Geocentric Solar Magnetospheric (GSM) cartesian coordinates plus Btotal (128 S/s)

---> Magnetic field vector in Geocentric Solar Magnetospheric (GSM) cartesian coordinates plus Btotal (8 or 16 S/s), including flagged data

Magnetic field vector in Despun MPA-aligned cartesian coordinates plus Btotal (128 S/s)

---> Magnetic field vector in Despun MPA-aligned cartesian coordinates plus Btotal (128 S/s), including flagged data

Magnetic field vector in Body Coordinate System cartesian coordinates plus Btotal (128 S/s)

---> Magnetic field vector in Body Coordinate System cartesian coordinates plus Btotal (128 S/s), including flagged data

Quality Flag:  0 = No identified problems, non-zero = blank out the data. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fgm/brst/l2/2015/09/mms1_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 21 timesteps. 

Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 1

Magnetic field vector in Geocentric Solar Ecliptic (GSE) cartesian coordinates plus Btotal (8 or 16 S/s)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fgm/srvy/l2/2015/09/mms1_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 62500751 [ns] = PT0.062501S, occurred for 39.5882% of the 433595 timesteps. 

Magnetic field vector in Geocentric Solar Magnetospheric (GSM) cartesian coordinates plus Btotal (8 or 16 S/s)

Magnetic field vector in Despun MPA-aligned cartesian coordinates plus Btotal (8 or 16 S/s)

---> Magnetic field vector in Despun MPA-aligned cartesian coordinates plus Btotal (8 or 16 S/s), including flagged data

Magnetic field vector in Body Coordinate System cartesian coordinates plus Btotal (8 or 16 S/s)

---> Magnetic field vector in Body Coordinate System cartesian coordinates plus Btotal (8 or 16 S/s), including flagged data

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fgm/srvy/l2/2015/09/mms1_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2882 timesteps. 

MMS Satellite Number 1 Dual Electron Spectrometer Burst-resolution instrument distributions

The MMS Mission home page at the Science Data Center (SDC) LASP, UC Boulder

The Magnetospheric Multiscale (MMS) Mission Home Page hosted by the Laboratory of Atmospheric and Space Physics, Science Data Center (LASP, SDC) at the University of Colorado, Boulder

NASA Web Page providing Inforamtion for the Magnetospheric Multiscale (MMS) Fast Plasma Investigation (FPI) Instrument

NASA Web Page providing an Overview of the Magnetospheric Multiscale (MMS) Fast Plasma Investigation (FPI) Instrument

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, C. Pollock at SwRI, NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, C. Pollock at SwRI, NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, C. Pollock at SwRI, NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/brst/l2/des-dist/2015/09/mms1_fpi_brst_l2_des-dist_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0050% of the 18753 timesteps. 

Dual Electron Spectrometers (from all.xml/instrument/description/@short)

Burst L2 Electron Distribution (from Master/CDFglobalAttributes/Data_type)

[CDAWeb List/Download/Create ONLY] MMS1 FPI/DES burst sky-map instrument distribution

MMS1 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even)

MMS1 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even)

MMS1 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even)

MMS1 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even)

MMS1 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even)

MMS1 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even)

MMS1 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even)

MMS1 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even)

MMS1 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even)

MMS1 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even)

MMS1 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd)

MMS1 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even)

MMS1 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS1 FPI/DES burst sky-map instrument distribution

MMS1 FPI/DES vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS1 FPI/DES compression lossless/lossy indicator at survey-start time

---> MMS1 FPI/DES Del-Phi (obs spin-phase) count at burst-start time

---> MMS1 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 1 Dual Electron Spectrometer Burst-resolution distribution moments

SPDF/CDAWeb. Please also acknowledge the data producer: J.Burch; C.Pollock, B.Giles at SwRI, NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J.Burch; C.Pollock, B.Giles at SwRI, NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.Burch; C.Pollock, B.Giles at SwRI, NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/brst/l2/des-moms/2015/09/mms1_fpi_brst_l2_des-moms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0050% of the 18753 timesteps. 

MMS1 FPI/DES 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS1 FPI/DES electron pitch-angle distribution for "low" energies during this burst

---> MMS1 FPI/DES electron pitch-angle distribution for "mid" energies during this burst

---> MMS1 FPI/DES electron pitch-angle distribution for "high" energies during this burst

MMS1 FPI/DES electron energy spectrum "near" +X_DSC during this burst

---> MMS1 FPI/DES electron energy spectrum "near" -X_DSC during this burst

---> MMS1 FPI/DES electron energy spectrum "near" +Y_DSC during this burst

---> MMS1 FPI/DES electron energy spectrum "near" -Y_DSC during this burst

---> MMS1 FPI/DES electron energy spectrum "near" +Z_DSC during this burst

---> MMS1 FPI/DES electron energy spectrum "near" -Z_DSC during this burst

MMS1 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this burst

---> MMS1 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this burst

---> MMS1 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this burst

MMS1 FPI/DES omni-directional electron energy spectrum during this burst

---> MMS1 FPI/DES electron number density error during this burst

MMS1 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS1 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS1 FPI/DES electron bulk-velocity DBCS vector during this burst

MMS1 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this burst

MMS1 FPI/DES electron bulk-velocity GSE vector during this burst

MMS1 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this burst

MMS1 FPI/DES electron bulk-velocity spintone vector in DBCS during this burst

MMS1 FPI/DES electron bulk-velocity spintone vector in GSE during this burst

MMS1 FPI/DES electron pressure tensor DBCS matrix during this burst

MMS1 FPI/DES electron pressure tensor GSE matrix during this burst

MMS1 FPI/DES electron temperature tensor DBCS matrix during this burst

MMS1 FPI/DES electron temperature tensor GSE matrix during this burst

MMS Satellite Number 1 Dual Electron Spectrometer Burst-resolution partial moments

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s, etc) resolution.  Per mission design, not all burst-resolution data are downlinked, but all survey data are downlinked. Planning around calibration activities, avoidance of Earth radiation belts, etc, when possible, FPI usually operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s resolution survey data are available. This product contains partial moments that come from performing the standard moment integrals over a limited portion of velocity space. The resulting quantities are named similarly to their corresponding standard moments, but are decorated with 'part' to differentiate. For example, density_part is the density moment integrated from a particular energy step to infinity. These partial moments are formed from the indicated data type (DES/DIS burst, FS or SS). For convenience, some additional parameters are included to augment those most commonly found in a moments product of this sort, plus time-stamps and other annotation characterizing the state of the instrument system at the indicated time.

See FPI Version Release Notes (https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for rules of use.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, B. Giles at SwRI, GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, B. Giles at SwRI, GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, B. Giles at SwRI, GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/brst/l2/des-partmoms/2015/09/mms1_fpi_brst_l2_des-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0050% of the 18753 timesteps. 

brst_l2_des-partmoms (from Master/CDFglobalAttributes/Data_type)

MMS1 FPI/DES partial electron bulk-velocity vector in DBCS during this burst

MMS1 FPI/DES partial electron bulk-velocity vector in GSE during this burst

MMS1 FPI/DES partial electron pressure tensor in DBCS during this burst

MMS1 FPI/DES partial electron pressure tensor in GSE during this burst

MMS1 FPI/DES partial electron temperature tensor in DBCS during this burst

MMS1 FPI/DES partial electron temperature tensor in GSE during this burst

MMS1 FPI/DES partial electron parallel temperature during this burst

MMS1 FPI/DES partial electron perpendicular temperature during this burst

MMS Satellite Number 1 Dual Ion Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/brst/l2/dis-dist/2015/09/mms1_fpi_brst_l2_dis-dist_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0194% of the 3286 timesteps. 

Dual Ion Spectrometers (from all.xml/instrument/description/@short)

Burst L2 Ion Distribution (from Master/CDFglobalAttributes/Data_type)

[CDAWeb List/Download/Create ONLY] MMS1 FPI/DIS burst sky-map instrument distribution

MMS1 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd)

MMS1 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even)

MMS1 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS1 FPI/DIS burst sky-map instrument distribution

MMS1 FPI/DIS vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 1 Dual Ion Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/brst/l2/dis-moms/2015/09/mms1_fpi_brst_l2_dis-moms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0194% of the 3286 timesteps. 

MMS1 FPI/DIS 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS1 FPI/DIS ion energy spectrum "near" +X_DSC during this burst

---> MMS1 FPI/DIS ion energy spectrum "near" -X_DSC during this burst

---> MMS1 FPI/DIS ion energy spectrum "near" +Y_DSC during this burst

---> MMS1 FPI/DIS ion energy spectrum "near" -Y_DSC during this burst

---> MMS1 FPI/DIS ion energy spectrum "near" +Z_DSC during this burst

---> MMS1 FPI/DIS ion energy spectrum "near" -Z_DSC during this burst

MMS1 FPI/DIS omni-directional ion energy spectrum during this burst

MMS1 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS1 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this burst

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this burst

MMS1 FPI/DIS ion bulk-velocity spintone vector in DBCS during this burst

MMS1 FPI/DIS ion bulk-velocity spintone vector in GSE during this burst

MMS1 FPI/DIS ion temperature tensor DBCS matrix during this burst

MMS1 FPI/DIS ion temperature tensor GSE matrix during this burst

MMS Satellite Number 1 Dual Ion Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/brst/l2/dis-partmoms/2015/09/mms1_fpi_brst_l2_dis-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0194% of the 3286 timesteps. 

brst_l2_dis-partmoms (from Master/CDFglobalAttributes/Data_type)

MMS1 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst

MMS1 FPI/DIS partial ion bulk-velocity vector in GSE during this burst

MMS1 FPI/DIS partial ion pressure tensor in DBCS during this burst

MMS1 FPI/DIS partial ion pressure tensor in GSE during this burst

MMS1 FPI/DIS partial ion temperature tensor in DBCS during this burst

MMS1 FPI/DIS partial ion temperature tensor in GSE during this burst

MMS1 FPI/DIS partial ion perpendicular temperature during this burst

MMS Satellite Number 1 Dual Electron Spectrometer Fast Survey-resolution instrument distributions

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch; C. Pollock and B. Giles at SwRI; NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch; C. Pollock and B. Giles at SwRI; NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch; C. Pollock and B. Giles at SwRI; NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/des-dist/2015/09/mms1_fpi_fast_l2_des-dist_20150901000000_v3.4.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps. 

Fast Mode L2 Electron Distributions (from Master/CDFglobalAttributes/Data_type)

MMS1 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS1 FPI/DES fast sky-map instrument distribution 1-sigma error

MMS1 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS1 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS1 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 1 Dual Electron Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/des-moms/2015/09/mms1_fpi_fast_l2_des-moms_20150901000000_v3.4.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps. 

MMS1 FPI/DES 32-bit vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS1 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

---> MMS1 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS1 FPI/DES electron pitch-angle distribution for "low" energies during this survey

---> MMS1 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

---> MMS1 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS1 FPI/DES electron energy spectrum "near" +X_DSC during this survey

---> MMS1 FPI/DES electron energy spectrum "near" -X_DSC during this survey

---> MMS1 FPI/DES electron energy spectrum "near" +Y_DSC during this survey

---> MMS1 FPI/DES electron energy spectrum "near" -Y_DSC during this survey

---> MMS1 FPI/DES electron energy spectrum "near" +Z_DSC during this survey

---> MMS1 FPI/DES electron energy spectrum "near" -Z_DSC during this survey

MMS1 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this survey

---> MMS1 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this survey

---> MMS1 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this survey

MMS1 FPI/DES omni-directional electron energy spectrum during this survey

---> MMS1 FPI/DES electron number density error during this survey

MMS1 FPI/DES electron bulk-velocity DBCS vector during this survey

MMS1 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey

MMS1 FPI/DES electron bulk-velocity GSE vector during this survey

MMS1 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey

MMS1 FPI/DES electron bulk-velocity spintone vector in DBCS during this survey

MMS1 FPI/DES electron bulk-velocity spintone vector in GSE during this survey

MMS1 FPI/DES electron pressure tensor DBCS matrix during this survey

MMS1 FPI/DES electron pressure tensor GSE matrix during this survey

MMS1 FPI/DES electron temperature tensor DBCS matrix during this survey

MMS1 FPI/DES electron temperature tensor GSE matrix during this survey

MMS Satellite Number 1 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s) resolution. Per mission design, not all burst-resolution data are downlinked, but all survey data are downlinked. Planning around calibration activities, avoidance of Earth radiation belts, etc, when possible, FPI usually operates in Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains partial moments that come from performing the standard moment integrals over a limited portion of velocity space. The resulting quantities are named similarly to their corresponding standard moments, but are decorated with 'part' to differentiate. For example, density_part is the density moment integrated from a particular energy step to infinity. These partial moments are formed from the indicated data type (DES/DIS burst, FS or SS). For convenience, some additional parameters are included to augment those most commonly found in a moments product of this sort, plus time-stamps and other annotation characterizing the state of the instrument system at the indicated time.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/des-momsaux/2015/09/mms1_fpi_fast_l2_des-momsaux_20150901000000_v3.4.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps.

MMS1 FPI/DES vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS1 FPI/DES partial electron bulk-velocity vector in DBCS during this survey

MMS1 FPI/DES partial electron bulk-velocity vector in GSE during this survey

MMS1 FPI/DES partial electron pressure tensor in DBCS during this survey

MMS1 FPI/DES partial electron pressure tensor in GSE during this survey

MMS1 FPI/DES partial electron temperature tensor in DBCS during this survey

MMS1 FPI/DES partial electron temperature tensor in GSE during this survey

MMS1 FPI/DES partial electron parallel temperature during this survey

MMS1 FPI/DES partial electron perpendicular temperature during this survey

MMS1 FPI/DES recommended energy index for partial moments during this survey

MMS1 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

MMS1 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS1 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

MMS1 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS1 FPI/DES electron energy spectrum "near" +X_DBCS during this survey

MMS1 FPI/DES electron energy spectrum "near" -X_DBCS during this survey

MMS1 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey

MMS1 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey

MMS1 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey

MMS1 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey

MMS1 FPI/DES electron energy parallel to the magnetic field direction during this survey

MMS1 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey

MMS1 FPI/DES electron energy perpendicular to the magnetic field direction during this survey

MMS1 FPI/DES electron bulk-velocity vector in DBCS during this survey

MMS1 FPI/DES electron bulk-velocity vector in GSE during this survey

MMS1 FPI/DES electron pressure tensor in DBCS during this survey

MMS1 FPI/DES electron temperature tensor in DBCS during this survey

MMS1 FPI/DES electron temperature tensor in GSE during this survey

MMS1 FPI/DES electron heat-flux vector in DBCS during this survey

MMS1 FPI/DES electron heat-flux vector in GSE during this survey

MMS1 FPI/DES Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments

MMS Satellite Number 1 Dual Electron Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/des-partmoms/2015/09/mms1_fpi_fast_l2_des-partmoms_20150901000000_v3.3.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps. 

fast_l2_des-partmoms (from Master/CDFglobalAttributes/Data_type)

MMS Satellite Number 1 Dual Ion Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/dis-dist/2015/09/mms1_fpi_fast_l2_dis-dist_20150901000000_v3.4.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps. 

MMS1 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS1 FPI/DIS fast sky-map instrument distribution 1-sigma error

MMS1 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 1 Dual Ion Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/dis-moms/2015/09/mms1_fpi_fast_l2_dis-moms_20150901000000_v3.4.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps. 

MMS1 FPI/DIS vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS1 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey

---> MMS1 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

---> MMS1 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

---> MMS1 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

---> MMS1 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

---> MMS1 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS1 FPI/DIS omni-directional ion energy spectrum during this survey

MMS1 FPI/DIS ion bulk-velocity vector in DBCS during this survey

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey

MMS Satellite Number 1 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/dis-momsaux/2015/09/mms1_fpi_fast_l2_dis-momsaux_20150901000000_v3.4.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps.

MMS1 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey

MMS1 FPI/DIS partial ion bulk-velocity vector in GSE during this survey

MMS1 FPI/DIS partial ion pressure tensor in DBCS during this survey

MMS1 FPI/DIS partial ion pressure tensor in GSE during this survey

MMS1 FPI/DIS partial ion temperature tensor in DBCS during this survey

MMS1 FPI/DIS partial ion temperature tensor in GSE during this survey

MMS1 FPI/DIS partial ion parallel temperature during this survey

MMS1 FPI/DIS partial ion perpendicular temperature during this survey

MMS1 FPI/DIS recommended energy index for partial moments during this survey

MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS1 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

MMS1 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

MMS1 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

MMS1 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

MMS1 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS1 FPI/DIS Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 1 Dual Ion Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/fast/l2/dis-partmoms/2015/09/mms1_fpi_fast_l2_dis-partmoms_20150901000000_v3.3.0.cdf. The most common cadence, 4500031000 [ns] = PT4.500031S, occurred for 30.9859% of the 22 timesteps. 

fast_l2_dis-partmoms (from Master/CDFglobalAttributes/Data_type)

MMS Satellite Number 1 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest (ROI) for the current Mission Phase.  Data captured from one of the four dual spectrometers over three spacecraft spins are reported at about 60 s resolution in this mode.  This product contains phase-space distribution maps of those survey-resolution data from Slow Mode.  In particular, the (highest possible quality at the time of release) corrected/converted "Slow Survey SkyMap" distributions are reported with time-stamps and other annotation characterizing the state of the instrument system at the indicated time.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, D. Gershman at SwRI, GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, D. Gershman at SwRI, GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, D. Gershman at SwRI, GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/slow/l2/des-dist/2015/09/mms1_fpi_slow_l2_des-dist_20150901003255_v3.4.0.cdf. The most common cadence, 58055327000 [ns] = PT58.055327S, occurred for 1.8519% of the 2 timesteps.

MMS1 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 1 Dual Electron Spectrometer SlowSurvey-resolution distribution moments

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest (ROI) for the current Mission Phase.  Data captured from one of the four dual spectrometers over three spacecraft spins are reported at about 60 s resolution in this mode. This moments product contains results from integrating the standard moments of phase-space distributions formed during Slow Mode. For convenience, some additional parameters are included to augment those most commonly found in a moments product of this sort, plus time-stamps and other annotations characterizing the state of the instrument system at the indicated time.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/slow/l2/des-moms/2015/09/mms1_fpi_slow_l2_des-moms_20150901003255_v3.4.0.cdf. The most common cadence, 58055327000 [ns] = PT58.055327S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 1 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/slow/l2/des-momsaux/2015/09/mms1_fpi_slow_l2_des-momsaux_20150901003255_v3.4.0.cdf. The most common cadence, 58055327000 [ns] = PT58.055327S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 1 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/slow/l2/dis-dist/2015/09/mms1_fpi_slow_l2_dis-dist_20150901003255_v3.4.0.cdf. The most common cadence, 58055327000 [ns] = PT58.055327S, occurred for 1.8349% of the 2 timesteps.

MMS1 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 1 Dual Ion Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/slow/l2/dis-moms/2015/09/mms1_fpi_slow_l2_dis-moms_20150901003255_v3.4.0.cdf. The most common cadence, 58055327000 [ns] = PT58.055327S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 1 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/fpi/slow/l2/dis-momsaux/2015/09/mms1_fpi_slow_l2_dis-momsaux_20150901003255_v3.4.0.cdf. The most common cadence, 58055327000 [ns] = PT58.055327S, occurred for 1.8349% of the 2 timesteps.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, S. Fuselier at SWRI

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, S. Fuselier at SWRI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, S. Fuselier at SWRI

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/hpca/brst/l2/ion/2015/09/mms1_hpca_brst_l2_ion_20150901121114_v4.1.0.cdf. The most common cadence, 624988000 [ns] = PT0.624988S, occurred for 70.5502% of the 654 timesteps. 

Hot Plasma Composition Analyzer (from all.xml/instrument/description/@short)

Science Mode Value as defined in the HPCA Science Algorithm Document

H+ per sweep status (0=bad): see Data_Quality_Key global attribute

Hydrogen+ Phase Space Density for all Elevation Anodes across all energies

He+ per sweep status (0=bad): see Data_Quality_Key global attribute

Helium+ Phase Space Density for all Elevation Anodes across all energies

He++ per sweep status (0=bad): see Data_Quality_Key global attribute

Helium++ Phase Space Density for all Elevation Anodes across all energies

O+ per sweep status (0=bad): see Data_Quality_Key global attribute

Oxygen+ Phase Space Density for all Elevation Anodes across all energies

Magnetic field vector in DMPA plus Btotal (8 or 16 S/s), Despun MPA-aligned cartesian coordinates

---> Magnetic field vector in GSM plus Btotal (8 or 16 S/s), Geocentric Solar Magnetospheric (GSM) cartesian coordinates

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/hpca/brst/l2/moments/2015/09/mms1_hpca_brst_l2_moments_20150901121114_v4.1.0.cdf. The most common cadence, 9999805000 [ns] = PT9.999805S, occurred for 57.1429% of the 32 timesteps. 

---> Ion Bulk Velocity Hydrogen+ for each HPCA half-spin (x, y, z)

---> (no CDAWeb plots) Ion Pressure Tensor Hydrogen+ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> (no CDAWeb plots) Ion Temp. Tensor Hydrogen+ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> Ion Bulk Velocity Helium+ for each HPCA half-spin (x, y, z)

---> (no CDAWeb plots) Ion Pressure Tensor Helium+ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> (no CDAWeb plots) Ion Temp. Tensor Helium+ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> Ion Bulk Velocity Helium++ for each HPCA half-spin (x, y, z)

---> (no CDAWeb plots) Ion Pressure Tensor Helium++ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> (no CDAWeb plots) Ion Temp. Tensor Helium++ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> Ion Bulk Velocity Oxygen+ for each HPCA half-spin (x, y, z)

---> (no CDAWeb plots) Ion Pressure Tensor Oxygen+ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

---> (no CDAWeb plots) Ion Temp. Tensor Oxygen+ for each HPCA half-spin (xx,yx,zx,xy,yy,zy,xz,yz,zz)

Magnetic field vector in DMPA plus Btotal (8 or 16 S/s) for each HPCA half-spin (x, y, z, total)

---> Magnetic field vector in GSM plus Btotal (8 or 16 S/s) for each HPCA half-spin (x, y, z, total)

---> Vperp vector plus Magnitude for H+ for each HPCA half-spin (x, y, z, total)

---> Vparallel vector plus Magnitude for H+ for each HPCA half-spin (x, y, z, total)

---> Vperp vector plus Magnitude in GSM for H+ for each HPCA half-spin (x, y, z, total)

---> Vparallel vector plus Magnitude in GSM for H+ for each HPCA half-spin (x, y, z, total)

---> Vperp vector plus Magnitude for He+ for each HPCA half-spin (x, y, z, total)

---> Vparallel vector plus Magnitude for He+ for each HPCA half-spin (x, y, z, total)

---> Vperp vector plus Magnitude in GSM for He+ for each HPCA half-spin (x, y, z, total)

---> Vparallel vector plus Magnitude in GSM for He+ for each HPCA half-spin (x, y, z, total)

Vperp vector plus Magnitude for He++ for each HPCA half-spin (x, y, z, total)

---> Vparallel vector plus Magnitude for He++ for each HPCA half-spin (x, y, z, total)

Vperp vector plus Magnitude in GSM for He++ for each HPCA half-spin (x, y, z, total)

Vparallel vector plus Magnitude in GSM for He++ for each HPCA half-spin (x, y, z, total)

---> Vperp vector plus Magnitude for O+ for each HPCA half-spin (x, y, z, total)

---> Vparallel vector plus Magnitude for O+ for each HPCA half-spin (x, y, z, total)

---> Vperp vector plus Magnitude in GSM for O+ for each HPCA half-spin (x, y, z, total)

--->Vparallel vector plus Magnitude in GSM for O+ for each HPCA half-spin (x, y, z, total)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/hpca/srvy/l2/ion/2015/09/mms1_hpca_srvy_l2_ion_20150901000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 50.0000% of the 1617 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/hpca/srvy/l2/moments/2015/09/mms1_hpca_srvy_l2_moments_20150901000000_v4.1.0.cdf. The most common cadence, 9999825000 [ns] = PT9.999825S, occurred for 15.9204% of the 32 timesteps. 

MMS Science instrument descriptions, hosted by National Aeronautics and Space Administration, NASA

MMS Hot Plasma Composition Analyzer, HPCA, Space Science Reviews instrument paper

Young, D. T. , J.L. Burch, R.G. Gomez, A. De Los Santos, G.P. Miller, P. Wilson, IV, N. Paschalidis, S.A. Fuselier, K. Pickens, E. Hertzberg, C.J. Pollock, J. Scherrer, P.B. Wood, E.T. Donald, D. Aaron, J. Furman, D. George, R.S. Gurnee, R.S. Hourani, A. Jacques, T. Johnson, T. Orr, K.S. Pan, S. Persyn, S. Pope, J. Roberts, M.R. Stokes, K.J. Trattner, and J.M. Webster, Hot Plasma Composition Analyzer for the Magnetospheric Multiscale Mission, Space Sci. Rev., 199, 407-470, 2016, DOI: 10.1007/s11214-014-0119-6

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/hpca/srvy/l2/tof-counts/2018/11/mms1_hpca_srvy_l2_tof-counts_20181115000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 92.5131% of the 74115 timesteps. 

srvy_l1b_tof_histogram (from Master/CDFglobalAttributes/Data_type)

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution is Los Alamos National Laboratory (LANL)

SPDF/CDAWeb. Please also acknowledge the data producer: M. G. Henderson, S. K. Morley at Los Alamos National Laboratory (LANL)

SPDF/SSCWeb. Please also acknowledge the data producer: M. G. Henderson, S. K. Morley at Los Alamos National Laboratory (LANL)

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M. G. Henderson, S. K. Morley at Los Alamos National Laboratory (LANL)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/mec/brst/l2/epht89d/2015/12/mms1_mec_brst_l2_epht89d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Magnetic Ephemeris and Coordinates (from all.xml/instrument/description/@short)

Dipole tilt angle. Rotation angle (around Y-axis) between GSM and SM coordinate systems. In units of degrees.

Quaternion rotation from GEI/J2000 to BCS (ECI to BCS). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to DBCS (ECI to DBCS). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to DMPA (ECI to DMPA). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to SMPA (ECI to SMPA). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to DSL (ECI to DSL). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to SSL (ECI to SSL). ((qx,qy,qz), qw)

Right ascension (deg) and declination (deg) of angular momentum (L)

Right ascension (deg) and declination (deg) of Major Principal Axis

L-phase (Sun-to-body-X dihedral angle about angular momentum vector L) (deg)

Z-phase (Sun-to-body-X dihedral angle about the body-Z vector) (deg)

P-phase (Sun-to-body-X dihedral angle about the major principal axis, P) (deg)

Kp index from QinDenton files (used as input to magnetic field models)

Dst index from QinDenton files. Used as input to magnetic field models

Earth eclipse flag: 0 = no eclipse; 1 = penumbral eclipse; 2 = umbral eclipse.

Moon eclipse flag: 0 = no eclipse; 1 = penumbral eclipse; 2 = umbral eclipse.

Geocentric Equatorial Inertial (GEI/J2000) position vector of mms1 (km)

Velocity of mms1 spacecraft in GEI/J2000 (i.e. ECI) coordinates (km/s)

Geocentric Solar Magnetospheric (GSM) position vector of mms1 (km)

Quaternion rotation from GEI/J2000 to GSM (ECI to GSM). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to GEO (ECI to GEO). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to SM (ECI to SM). ((qx,qy,qz), qw)

Quaternion rotation from GEI/J2000 to GSE (ECI to GSE). ((qx,qy,qz), qw)

Geocentric Solar Ecliptic (J2000 Pole, GSE2000) position vector of mms1 (km)

Quaternion rotation from GEI/J2000 to GSE2000 (ECI to GSE2000). ((qx,qy,qz), qw)

Geodetic height of mms1 spacecraft. (Height above WGS84 Spheroid.)

Geocentric position vector (in km) of the Sun in GEI/J2000 Coordinates.

Geocentric position vector (in km) of the Moon in GEI/J2000 Coordinates.

Fieldline Type: 0 = IMF; 1 = Closed; 2 = Open Northern Lobe; 3 = Open Southern Lobe; -1 = Inside Earth; -2 = Target Height Unreachable; -3 = Bad Trace (error).

Geodetic latitude and longitude of southern footpoint (100km geodetic height) of field threading the mms1 spacecraft

Geodetic latitude and longitude of northern footpoint (100km geodetic height) of field threading the mms1 spacecraft

GSM position southern footpoint (100km geodetic height) of field threading the mms1 spacecraft

Magnetic field (in GSM) at southern footpoint (100km geodetic height) of field threading the mms1 spacecraft

GSM position northern footpoint (100km geodetic height) of field threading the mms1 spacecraft

Magnetic field (in GSM) at northern footpoint (100km geodetic height) of field threading the mms1 spacecraft

GSM position of min-B point of field threading the mms1 spacecraft

Magnetic field (in GSM) at min-B point of field threading the mms1 spacecraft

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/mec/brst/l2/epht89q/2015/12/mms1_mec_brst_l2_epht89q_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/mec/brst/l2/ephts04d/2015/12/mms1_mec_brst_l2_ephts04d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/mec/srvy/l2/epht89d/2015/09/mms1_mec_srvy_l2_epht89d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/mec/srvy/l2/epht89q/2015/09/mms1_mec_srvy_l2_epht89q_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/mec/srvy/l2/ephts04d/2015/09/mms1_mec_srvy_l2_ephts04d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Level 2 Search Coil Magnetometer AC Magnetic Field Burst (8192S/s) Data

The French involment (SCM instruments) on MMS is supported by CNES, CNRS-INSIS and CNRS-INSU.

The MMS LPP SCM Team home page at LPP, CNRS École Polytechnique and Sorbonne Université

The Magnetospheric Multiscale (MMS) Search-Coil Magnetometer (SCM) home page hosted by the Laboratoire de Physique des Plasma (LPP), CNRS École Polytechnique and Sorbonne Université

See https://lasp.colorado.edu/galaxy/display/mms/MMS+Data+Rights+and+Rules+for+Data+Use and the acknowledgment informations given in this file.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Burch, O. Le Contel at SWRI, LPP

SPDF/SSCWeb. Please also acknowledge the data producer: J. Burch, O. Le Contel at SWRI, LPP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Burch, O. Le Contel at SWRI, LPP

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/scm/brst/l2/scb/2015/09/mms1_scm_brst_l2_scb_20150901121114_v2.2.1.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 74.1097% of the 3521219 timesteps. 

Search Coil Magnetometer (from all.xml/instrument/description/@short)

(List/Create Only) Quality Factor (one letter per antenna, G=good)

Level 2 Search Coil Magnetometer AC Magnetic Field High Burst (16384S/s) Data

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier provides the three-dimensional measurement of the magnetic field fluctuations. The analog magnetic waveforms measured by the SCM are digitized and processed inside the digital signal processor (DSP), collected and stored by the central instrument data processor (CIDP) via the Fields central electronics box (CEB). Prior to launch, all SCM Flight models were calibrated by LPP at the National Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM transfer function is checked thanks to the onboard calibration signal provided by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI, burst mode data are also acquired as well as high burst mode data. SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in the GSE frame.The instrument paper for SCM can be found at http://link.springer.com/article/10.1007/s11214-014-0096-9

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/scm/brst/l2/schb/2015/09/mms1_scm_brst_l2_schb_20150901121114_v2.2.0.cdf. The most common cadence, 61036 [ns] = PT0.000061036S, occurred for 86.9490% of the 2193905 timesteps. 

Level 2 Search Coil Magnetometer AC Magnetic Field Survey (32S/s) Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms1/scm/srvy/l2/scsrvy/2015/09/mms1_scm_srvy_l2_scsrvy_20150902_v2.2.1.cdf. The most common cadence, 31250376 [ns] = PT0.03125S, occurred for 88.7298% of the 2448120 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/aspoc/srvy/l2/2015/09/mms2_aspoc_srvy_l2_20150901_v2.0.0.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

MMS Satellite Number 2 (from all.xml/observatory/description/@short)

MMS Satellite Number 2 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/dsp/fast/l2/bpsd/2015/09/mms2_dsp_fast_l2_bpsd_20150901_v2.1.1.cdf. The most common cadence, 2000020964 [ns] = PT2.000021S, occurred for 2.3745% of the 600 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/dsp/fast/l2/epsd/2015/09/mms2_dsp_fast_l2_epsd_20150901_v0.6.5.cdf. The most common cadence, 2000020964 [ns] = PT2.000021S, occurred for 2.3744% of the 600 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/dsp/slow/l2/bpsd/2015/09/mms2_dsp_slow_l2_bpsd_20150901_v2.1.0.cdf. The most common cadence, 16000166671 [ns] = PT16.000167S, occurred for 1.6987% of the 38 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/dsp/slow/l2/epsd/2015/09/mms2_dsp_slow_l2_epsd_20150901_v0.6.5.cdf. The most common cadence, 16000166671 [ns] = PT16.000167S, occurred for 1.6995% of the 38 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/amb/2015/09/mms2_edi_brst_l2_amb_20150901121114_v3.1.1.cdf. The most common cadence, 1000010000 [ns] = PT1.00001S, occurred for 56.1313% of the 325 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/amb/2015/09/mms2_edi_brst_l2_amb_20150901121114_v3.1.1.cdf. The most common cadence, 976563 [ns] = PT0.000976563S, occurred for 50.0001% of the 296960 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/amb-pm2/2016/01/mms2_edi_brst_l2_amb-pm2_20160104222503_v4.1.0.cdf. The most common cadence, 1000011322 [ns] = PT1.000011S, occurred for all 59 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/amb-pm2/2016/01/mms2_edi_brst_l2_amb-pm2_20160104222503_v4.1.0.cdf. The most common cadence, 976574 [ns] = PT0.000976574S, occurred for 55.6780% of the 34208 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/efield/2015/09/mms2_edi_brst_l2_efield_20150914141304_v1.5.0.cdf. The most common cadence, 5000000000 [ns] = PT5S, occurred for 45.9459% of the 17 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/q0/2016/01/mms2_edi_brst_l2_q0_20160101052814_v4.0.0.cdf. The most common cadence, 1000012000 [ns] = PT1.000012S, occurred for 48.1481% of the 52 timesteps. 

Counts based on variable 'epoch_gdu1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/q0/2016/01/mms2_edi_brst_l2_q0_20160101052814_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 78.5565% of the 6019 timesteps. 

Counts based on variable 'epoch_gdu2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/brst/l2/q0/2016/01/mms2_edi_brst_l2_q0_20160101052814_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 70.2554% of the 4979 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/srvy/l2/amb/2015/09/mms2_edi_srvy_l2_amb_20150901_v4.1.0.cdf. The most common cadence, 4000041856 [ns] = PT4.000042S, occurred for 5.1776% of the 554 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/srvy/l2/amb/2015/09/mms2_edi_srvy_l2_amb_20150901_v4.1.0.cdf. The most common cadence, 31250326 [ns] = PT0.03125S, occurred for 52.3438% of the 716967 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/srvy/l2/amb-pm2/2016/01/mms2_edi_srvy_l2_amb-pm2_20160104_v4.1.0.cdf. The most common cadence, 4000044736 [ns] = PT4.000045S, occurred for 23.0871% of the 1572 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/srvy/l2/amb-pm2/2016/01/mms2_edi_srvy_l2_amb-pm2_20160104_v4.1.0.cdf. The most common cadence, 31250350 [ns] = PT0.03125S, occurred for 22.5000% of the 196128 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edi/srvy/l2/efield/2015/09/mms2_edi_srvy_l2_efield_20150901_v1.6.2.cdf. The most common cadence, 224464492416 [ns] = PT3M44.464492S, occurred for 0.4016% of the 1 timesteps. 

Counts based on variable 'mms2_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/brst/l2/dce/2015/09/mms2_edp_brst_l2_dce_20150901121114_v2.2.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 56.6902% of the 2693554 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/brst/l2/hmfe/2015/09/mms2_edp_brst_l2_hmfe_20150901121114_v1.0.1.cdf. The most common cadence, 15259 [ns] = PT0.000015259S, occurred for 94.5678% of the 9544297 timesteps. 

Counts based on variable 'mms2_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/brst/l2/scpot/2015/09/mms2_edp_brst_l2_scpot_20150901121114_v2.4.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 56.6902% of the 2693554 timesteps. 

Counts based on variable 'mms2_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/fast/l2/dce/2015/09/mms2_edp_fast_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 31250327 [ns] = PT0.03125S, occurred for 77.1945% of the 1248401 timesteps. 

Counts based on variable 'mms2_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/fast/l2/scpot/2015/09/mms2_edp_fast_l2_scpot_20150901000000_v2.7.2.cdf. The most common cadence, 31250327 [ns] = PT0.03125S, occurred for 77.1945% of the 1248401 timesteps. 

Counts based on variable 'mms2_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/slow/l2/dce/2015/09/mms2_edp_slow_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 125001282 [ns] = PT0.125001S, occurred for 63.5851% of the 182189 timesteps. 

Counts based on variable 'mms2_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/slow/l2/scpot/2015/09/mms2_edp_slow_l2_scpot_20150901000000_v2.7.0.cdf. The most common cadence, 125001282 [ns] = PT0.125001S, occurred for 63.5851% of the 182189 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/edp/srvy/l2/hfesp/2015/09/mms2_edp_srvy_l2_hfesp_20150901_v0.4.0.cdf. The most common cadence, 16000167936 [ns] = PT16.000168S, occurred for 3.2049% of the 173 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/epd-eis/brst/l2/extof/2015/09/mms2_epd-eis_brst_l2_extof_20150901121114_v3.0.0.cdf. The most common cadence, 604906082 [ns] = PT0.604906S, occurred for 25.1829% of the 241 timesteps. 

MMS2 ExTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Burst proton_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst proton_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst proton_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst oxygen_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst oxygen_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst oxygen_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst helium_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst helium_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst helium_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst alpha_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst alpha_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst alpha_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst dump_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst dump_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS2 ExTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ExTOF-Burst dump_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

Valid Time of Flight by Pulse Height Energy Events per second MMS2

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/epd-eis/brst/l2/phxtof/2015/09/mms2_epd-eis_brst_l2_phxtof_20150901121114_v3.0.0.cdf. The most common cadence, 604906082 [ns] = PT0.604906S, occurred for 25.1829% of the 241 timesteps. 

MMS2 PhxTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Burst proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Burst dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/epd-eis/srvy/l2/electronenergy/2015/09/mms2_epd-eis_srvy_l2_electronenergy_20150901_v3.0.0.cdf. The most common cadence, 2419625044 [ns] = PT2.419625S, occurred for 11.8573% of the 1861 timesteps. 

MMS2 ElectronEnergy-Survey electron_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ElectronEnergy-Survey electron_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ElectronEnergy-Survey electron_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ElectronEnergy-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ElectronEnergy-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ElectronEnergy-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ElectronEnergy-Survey electron_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 ElectronEnergy-Survey electron_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 ElectronEnergy-Survey electron_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 ElectronEnergy-Survey electron_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ElectronEnergy-Survey electron_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ElectronEnergy-Survey electron_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ElectronEnergy-Survey electron_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ElectronEnergy-Survey electron_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ElectronEnergy-Survey electron_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ElectronEnergy-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ElectronEnergy-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ElectronEnergy-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 ElectronEnergy-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ElectronEnergy-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ElectronEnergy-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 ElectronEnergy-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ElectronEnergy-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 ElectronEnergy-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/epd-eis/srvy/l2/extof/2015/09/mms2_epd-eis_srvy_l2_extof_20150901_v3.0.0.cdf. The most common cadence, 2419625044 [ns] = PT2.419625S, occurred for 27.2455% of the 5451 timesteps. 

MMS2 ExTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 ExTOF-Survey proton_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey proton_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey proton_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey oxygen_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey oxygen_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey oxygen_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey helium_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey helium_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey helium_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey alpha_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey alpha_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey alpha_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey dump_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey dump_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS2 ExTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 ExTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS2 ExTOF-Survey dump_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/epd-eis/srvy/l2/phxtof/2015/09/mms2_epd-eis_srvy_l2_phxtof_20150901_v3.0.0.cdf. The most common cadence, 2419625044 [ns] = PT2.419625S, occurred for 27.2368% of the 5449 timesteps. 

MMS2 PhxTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS2 PhxTOF-Survey proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS2 PhxTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS2 PhxTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS2 PhxTOF-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/feeps/brst/l2/electron/2015/09/mms2_feeps_brst_l2_electron_20150901121114_v7.1.1.cdf. The most common cadence, 302464000 [ns] = PT0.302464S, occurred for 49.0871% of the 941 timesteps. 

MMS2 FEEPS top side burst mode electron count error statistics sensor 1

MMS2 FEEPS top side burst mode electron count error statistics sensor 2

MMS2 FEEPS top side burst mode electron count error statistics sensor 3

MMS2 FEEPS top side burst mode electron count error statistics sensor 4

MMS2 FEEPS top side burst mode electron count error statistics sensor 5

MMS2 FEEPS top side burst mode electron count error statistics sensor 9

MMS2 FEEPS top side burst mode electron count error statistics sensor 10

MMS2 FEEPS top side burst mode electron count error statistics sensor 11

MMS2 FEEPS top side burst mode electron count error statistics sensor 12

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 1

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 2

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 3

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 4

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 5

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 9

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 10

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 11

MMS2 FEEPS bottom side burst mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/feeps/brst/l2/ion/2015/09/mms2_feeps_brst_l2_ion_20150901121114_v7.1.1.cdf. The most common cadence, 302464000 [ns] = PT0.302464S, occurred for 49.0871% of the 941 timesteps. 

MMS2 FEEPS top side burst mode ion count error statistics sensor 6

MMS2 FEEPS top side burst mode ion count error statistics sensor 7

MMS2 FEEPS top side burst mode ion count error statistics sensor 8

MMS2 FEEPS bottom side burst mode ion count error statistics sensor 6

MMS2 FEEPS bottom side burst mode ion count error statistics sensor 7

MMS2 FEEPS bottom side burst mode ion count error statistics sensor 8

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/feeps/srvy/l2/electron/2015/09/mms2_feeps_srvy_l2_electron_20150901000000_v7.1.1.cdf. The most common cadence, 2419712000 [ns] = PT2.419712S, occurred for 13.6245% of the 3229 timesteps. 

MMS2 FEEPS bottom side survey mode electron count rate sensor 10

MMS2 FEEPS bottom side survey mode electron count rate sensor 11

MMS2 FEEPS bottom side survey mode electron count rate sensor 12

MMS2 FEEPS top side survey mode electron count error statistics sensor 1

MMS2 FEEPS top side survey mode electron count error statistics sensor 2

MMS2 FEEPS top side survey mode electron count error statistics sensor 3

MMS2 FEEPS top side survey mode electron count error statistics sensor 4

MMS2 FEEPS top side survey mode electron count error statistics sensor 5

MMS2 FEEPS top side survey mode electron count error statistics sensor 9

MMS2 FEEPS top side survey mode electron count error statistics sensor 10

MMS2 FEEPS top side survey mode electron count error statistics sensor 11

MMS2 FEEPS top side survey mode electron count error statistics sensor 12

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 1

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 2

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 3

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 4

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 5

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 9

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 10

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 11

MMS2 FEEPS bottom side survey mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/feeps/srvy/l2/ion/2015/09/mms2_feeps_srvy_l2_ion_20150901000000_v7.1.1.cdf. The most common cadence, 2419712000 [ns] = PT2.419712S, occurred for 13.6245% of the 3229 timesteps. 

MMS2 FEEPS top side survey mode ion count error statistics sensor 6

MMS2 FEEPS top side survey mode ion count error statistics sensor 7

MMS2 FEEPS top side survey mode ion count error statistics sensor 8

MMS2 FEEPS bottom side survey mode ion count error statistics sensor 6

MMS2 FEEPS bottom side survey mode ion count error statistics sensor 7

MMS2 FEEPS bottom side survey mode ion count error statistics sensor 8

Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 2

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fgm/brst/l2/2015/09/mms2_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 7812580 [ns] = PT0.007813S, occurred for 79.6185% of the 59108 timesteps. 

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fgm/brst/l2/2015/09/mms2_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 21 timesteps. 

Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 2

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fgm/srvy/l2/2015/09/mms2_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 62500654 [ns] = PT0.062501S, occurred for 39.2349% of the 429923 timesteps. 

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fgm/srvy/l2/2015/09/mms2_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2883 timesteps. 

MMS Satellite Number 2 Dual Electron Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/brst/l2/des-dist/2015/09/mms2_fpi_brst_l2_des-dist_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0051% of the 18754 timesteps. 

[CDAWeb List/Download/Create ONLY] MMS2 FPI/DES burst sky-map instrument distribution

MMS2 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even)

MMS2 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even)

MMS2 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even)

MMS2 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even)

MMS2 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even)

MMS2 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even)

MMS2 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even)

MMS2 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even)

MMS2 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even)

MMS2 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even)

MMS2 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd)

MMS2 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even)

MMS2 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS2 FPI/DES burst sky-map instrument distribution

MMS2 FPI/DES vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS2 FPI/DES compression lossless/lossy indicator at survey-start time

---> MMS2 FPI/DES Del-Phi (obs spin-phase) count at burst-start time

---> MMS2 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 2 Dual Electron Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/brst/l2/des-moms/2015/09/mms2_fpi_brst_l2_des-moms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0051% of the 18754 timesteps. 

MMS2 FPI/DES 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS2 FPI/DES electron pitch-angle distribution for "low" energies during this burst

---> MMS2 FPI/DES electron pitch-angle distribution for "mid" energies during this burst

---> MMS2 FPI/DES electron pitch-angle distribution for "high" energies during this burst

MMS2 FPI/DES electron energy spectrum "near" +X_DSC during this burst

---> MMS2 FPI/DES electron energy spectrum "near" -X_DSC during this burst

---> MMS2 FPI/DES electron energy spectrum "near" +Y_DSC during this burst

---> MMS2 FPI/DES electron energy spectrum "near" -Y_DSC during this burst

---> MMS2 FPI/DES electron energy spectrum "near" +Z_DSC during this burst

---> MMS2 FPI/DES electron energy spectrum "near" -Z_DSC during this burst

MMS2 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this burst

---> MMS2 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this burst

---> MMS2 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this burst

MMS2 FPI/DES omni-directional electron energy spectrum during this burst

---> MMS2 FPI/DES electron number density error during this burst

MMS2 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS2 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS2 FPI/DES electron bulk-velocity DBCS vector during this burst

MMS2 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this burst

MMS2 FPI/DES electron bulk-velocity GSE vector during this burst

MMS2 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this burst

MMS2 FPI/DES electron bulk-velocity spintone vector in DBCS during this burst

MMS2 FPI/DES electron bulk-velocity spintone vector in GSE during this burst

MMS2 FPI/DES electron pressure tensor DBCS matrix during this burst

MMS2 FPI/DES electron pressure tensor GSE matrix during this burst

MMS2 FPI/DES electron temperature tensor DBCS matrix during this burst

MMS2 FPI/DES electron temperature tensor GSE matrix during this burst

MMS Satellite Number 2 Dual Electron Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/brst/l2/des-partmoms/2015/09/mms2_fpi_brst_l2_des-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0051% of the 18754 timesteps. 

MMS2 FPI/DES partial electron bulk-velocity vector in DBCS during this burst

MMS2 FPI/DES partial electron bulk-velocity vector in GSE during this burst

MMS2 FPI/DES partial electron pressure tensor in DBCS during this burst

MMS2 FPI/DES partial electron pressure tensor in GSE during this burst

MMS2 FPI/DES partial electron temperature tensor in DBCS during this burst

MMS2 FPI/DES partial electron temperature tensor in GSE during this burst

MMS2 FPI/DES partial electron parallel temperature during this burst

MMS2 FPI/DES partial electron perpendicular temperature during this burst

MMS Satellite Number 2 Dual Ion Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/brst/l2/dis-dist/2015/09/mms2_fpi_brst_l2_dis-dist_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0233% of the 3287 timesteps. 

[CDAWeb List/Download/Create ONLY] MMS2 FPI/DIS burst sky-map instrument distribution

MMS2 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd)

MMS2 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even)

MMS2 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS2 FPI/DIS burst sky-map instrument distribution

MMS2 FPI/DIS vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 2 Dual Ion Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/brst/l2/dis-moms/2015/09/mms2_fpi_brst_l2_dis-moms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0233% of the 3287 timesteps. 

MMS2 FPI/DIS 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS2 FPI/DIS ion energy spectrum "near" +X_DSC during this burst

---> MMS2 FPI/DIS ion energy spectrum "near" -X_DSC during this burst

---> MMS2 FPI/DIS ion energy spectrum "near" +Y_DSC during this burst

---> MMS2 FPI/DIS ion energy spectrum "near" -Y_DSC during this burst

---> MMS2 FPI/DIS ion energy spectrum "near" +Z_DSC during this burst

---> MMS2 FPI/DIS ion energy spectrum "near" -Z_DSC during this burst

MMS2 FPI/DIS omni-directional ion energy spectrum during this burst

MMS2 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS2 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this burst

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this burst

MMS2 FPI/DIS ion bulk-velocity spintone vector in DBCS during this burst

MMS2 FPI/DIS ion bulk-velocity spintone vector in GSE during this burst

MMS2 FPI/DIS ion temperature tensor DBCS matrix during this burst

MMS2 FPI/DIS ion temperature tensor GSE matrix during this burst

MMS Satellite Number 2 Dual Ion Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/brst/l2/dis-partmoms/2015/09/mms2_fpi_brst_l2_dis-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0233% of the 3287 timesteps. 

MMS2 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst

MMS2 FPI/DIS partial ion bulk-velocity vector in GSE during this burst

MMS2 FPI/DIS partial ion pressure tensor in DBCS during this burst

MMS2 FPI/DIS partial ion pressure tensor in GSE during this burst

MMS2 FPI/DIS partial ion temperature tensor in DBCS during this burst

MMS2 FPI/DIS partial ion temperature tensor in GSE during this burst

MMS2 FPI/DIS partial ion perpendicular temperature during this burst

MMS Satellite Number 2 Dual Electron Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/des-dist/2015/09/mms2_fpi_fast_l2_des-dist_20150901080000_v3.4.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps. 

MMS2 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS2 FPI/DES fast sky-map instrument distribution 1-sigma error

MMS2 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS2 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS2 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 2 Dual Electron Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/des-moms/2015/09/mms2_fpi_fast_l2_des-moms_20150901080000_v3.4.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps. 

MMS2 FPI/DES 32-bit vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS2 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

---> MMS2 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS2 FPI/DES electron pitch-angle distribution for "low" energies during this survey

---> MMS2 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

---> MMS2 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS2 FPI/DES electron energy spectrum "near" +X_DSC during this survey

---> MMS2 FPI/DES electron energy spectrum "near" -X_DSC during this survey

---> MMS2 FPI/DES electron energy spectrum "near" +Y_DSC during this survey

---> MMS2 FPI/DES electron energy spectrum "near" -Y_DSC during this survey

---> MMS2 FPI/DES electron energy spectrum "near" +Z_DSC during this survey

---> MMS2 FPI/DES electron energy spectrum "near" -Z_DSC during this survey

MMS2 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this survey

---> MMS2 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this survey

---> MMS2 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this survey

MMS2 FPI/DES omni-directional electron energy spectrum during this survey

---> MMS2 FPI/DES electron number density error during this survey

MMS2 FPI/DES electron bulk-velocity DBCS vector during this survey

MMS2 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey

MMS2 FPI/DES electron bulk-velocity GSE vector during this survey

MMS2 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey

MMS2 FPI/DES electron bulk-velocity spintone vector in DBCS during this survey

MMS2 FPI/DES electron bulk-velocity spintone vector in GSE during this survey

MMS2 FPI/DES electron pressure tensor DBCS matrix during this survey

MMS2 FPI/DES electron pressure tensor GSE matrix during this survey

MMS2 FPI/DES electron temperature tensor DBCS matrix during this survey

MMS2 FPI/DES electron temperature tensor GSE matrix during this survey

MMS Satellite Number 2 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/des-momsaux/2015/09/mms2_fpi_fast_l2_des-momsaux_20150901080000_v3.4.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps.

MMS2 FPI/DES vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS2 FPI/DES partial electron bulk-velocity vector in DBCS during this survey

MMS2 FPI/DES partial electron bulk-velocity vector in GSE during this survey

MMS2 FPI/DES partial electron pressure tensor in DBCS during this survey

MMS2 FPI/DES partial electron pressure tensor in GSE during this survey

MMS2 FPI/DES partial electron temperature tensor in DBCS during this survey

MMS2 FPI/DES partial electron temperature tensor in GSE during this survey

MMS2 FPI/DES partial electron parallel temperature during this survey

MMS2 FPI/DES partial electron perpendicular temperature during this survey

MMS2 FPI/DES recommended energy index for partial moments during this survey

MMS2 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

MMS2 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS2 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

MMS2 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS2 FPI/DES electron energy spectrum "near" +X_DBCS during this survey

MMS2 FPI/DES electron energy spectrum "near" -X_DBCS during this survey

MMS2 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey

MMS2 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey

MMS2 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey

MMS2 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey

MMS2 FPI/DES electron energy parallel to the magnetic field direction during this survey

MMS2 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey

MMS2 FPI/DES electron energy perpendicular to the magnetic field direction during this survey

MMS2 FPI/DES electron bulk-velocity vector in DBCS during this survey

MMS2 FPI/DES electron bulk-velocity vector in GSE during this survey

MMS2 FPI/DES electron pressure tensor in DBCS during this survey

MMS2 FPI/DES electron temperature tensor in DBCS during this survey

MMS2 FPI/DES electron temperature tensor in GSE during this survey

MMS2 FPI/DES electron heat-flux vector in DBCS during this survey

MMS2 FPI/DES electron heat-flux vector in GSE during this survey

MMS2 FPI/DES Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 2 Dual Electron Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/des-partmoms/2015/09/mms2_fpi_fast_l2_des-partmoms_20150901080000_v3.3.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps. 

MMS Satellite Number 2 Dual Ion Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/dis-dist/2015/09/mms2_fpi_fast_l2_dis-dist_20150901080000_v3.4.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps. 

MMS2 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS2 FPI/DIS fast sky-map instrument distribution 1-sigma error

MMS2 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 2 Dual Ion Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/dis-moms/2015/09/mms2_fpi_fast_l2_dis-moms_20150901080000_v3.4.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps. 

MMS2 FPI/DIS vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS2 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey

---> MMS2 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

---> MMS2 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

---> MMS2 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

---> MMS2 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

---> MMS2 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS2 FPI/DIS omni-directional ion energy spectrum during this survey

MMS2 FPI/DIS ion bulk-velocity vector in DBCS during this survey

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey

MMS Satellite Number 2 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/dis-momsaux/2015/09/mms2_fpi_fast_l2_dis-momsaux_20150901080000_v3.4.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps.

MMS2 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey

MMS2 FPI/DIS partial ion bulk-velocity vector in GSE during this survey

MMS2 FPI/DIS partial ion pressure tensor in DBCS during this survey

MMS2 FPI/DIS partial ion pressure tensor in GSE during this survey

MMS2 FPI/DIS partial ion temperature tensor in DBCS during this survey

MMS2 FPI/DIS partial ion temperature tensor in GSE during this survey

MMS2 FPI/DIS partial ion parallel temperature during this survey

MMS2 FPI/DIS partial ion perpendicular temperature during this survey

MMS2 FPI/DIS recommended energy index for partial moments during this survey

MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS2 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

MMS2 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

MMS2 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

MMS2 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

MMS2 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS2 FPI/DIS Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 2 Dual Ion Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/fast/l2/dis-partmoms/2015/09/mms2_fpi_fast_l2_dis-partmoms_20150901080000_v3.3.0.cdf. The most common cadence, 4500054000 [ns] = PT4.500054S, occurred for 19.7861% of the 37 timesteps. 

MMS Satellite Number 2 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/slow/l2/des-dist/2015/09/mms2_fpi_slow_l2_des-dist_20150902002703_v3.4.0.cdf. The most common cadence, 58085164000 [ns] = PT58.085164S, occurred for 1.8349% of the 2 timesteps.

MMS2 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 2 Dual Electron Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/slow/l2/des-moms/2015/09/mms2_fpi_slow_l2_des-moms_20150902002703_v3.4.0.cdf. The most common cadence, 58085164000 [ns] = PT58.085164S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 2 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/slow/l2/des-momsaux/2015/09/mms2_fpi_slow_l2_des-momsaux_20150902002703_v3.4.0.cdf. The most common cadence, 58085164000 [ns] = PT58.085164S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 2 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/slow/l2/dis-dist/2015/09/mms2_fpi_slow_l2_dis-dist_20150902002703_v3.4.0.cdf. The most common cadence, 58085164000 [ns] = PT58.085164S, occurred for 1.8349% of the 2 timesteps.

MMS2 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 2 Dual Ion Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/slow/l2/dis-moms/2015/09/mms2_fpi_slow_l2_dis-moms_20150902002703_v3.4.0.cdf. The most common cadence, 58085164000 [ns] = PT58.085164S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 2 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/fpi/slow/l2/dis-momsaux/2015/09/mms2_fpi_slow_l2_dis-momsaux_20150902002703_v3.4.0.cdf. The most common cadence, 58085164000 [ns] = PT58.085164S, occurred for 1.8349% of the 2 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/hpca/brst/l2/ion/2015/09/mms2_hpca_brst_l2_ion_20150901121114_v4.1.0.cdf. The most common cadence, 624988000 [ns] = PT0.624988S, occurred for 37.4326% of the 347 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/hpca/brst/l2/moments/2015/09/mms2_hpca_brst_l2_moments_20150901121114_v4.1.0.cdf. The most common cadence, 9999767000 [ns] = PT9.999767S, occurred for 58.9286% of the 33 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/hpca/srvy/l2/ion/2015/09/mms2_hpca_srvy_l2_ion_20150901000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 50.0450% of the 556 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/hpca/srvy/l2/moments/2015/09/mms2_hpca_srvy_l2_moments_20150901000100_v4.1.0.cdf. The most common cadence, 69998359000 [ns] = PT1M9.998359S, occurred for 4.4776% of the 3 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/hpca/srvy/l2/tof-counts/2018/11/mms2_hpca_srvy_l2_tof-counts_20181115000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 92.5109% of the 74129 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/mec/brst/l2/epht89d/2015/12/mms2_mec_brst_l2_epht89d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Geocentric Equatorial Inertial (GEI/J2000) position vector of mms2 (km)

Velocity of mms2 spacecraft in GEI/J2000 (i.e. ECI) coordinates (km/s)

Geocentric Solar Magnetospheric (GSM) position vector of mms2 (km)

Geocentric Solar Ecliptic (J2000 Pole, GSE2000) position vector of mms2 (km)

Geodetic height of mms2 spacecraft. (Height above WGS84 Spheroid.)

Geodetic latitude and longitude of southern footpoint (100km geodetic height) of field threading the mms2 spacecraft

Geodetic latitude and longitude of northern footpoint (100km geodetic height) of field threading the mms2 spacecraft

GSM position southern footpoint (100km geodetic height) of field threading the mms2 spacecraft

Magnetic field (in GSM) at southern footpoint (100km geodetic height) of field threading the mms2 spacecraft

GSM position northern footpoint (100km geodetic height) of field threading the mms2 spacecraft

Magnetic field (in GSM) at northern footpoint (100km geodetic height) of field threading the mms2 spacecraft

GSM position of min-B point of field threading the mms2 spacecraft

Magnetic field (in GSM) at min-B point of field threading the mms2 spacecraft

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/mec/brst/l2/epht89q/2015/12/mms2_mec_brst_l2_epht89q_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/mec/brst/l2/ephts04d/2015/12/mms2_mec_brst_l2_ephts04d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/mec/srvy/l2/epht89d/2015/09/mms2_mec_srvy_l2_epht89d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/mec/srvy/l2/epht89q/2015/09/mms2_mec_srvy_l2_epht89q_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/mec/srvy/l2/ephts04d/2015/09/mms2_mec_srvy_l2_ephts04d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/scm/brst/l2/scb/2015/09/mms2_scm_brst_l2_scb_20150901121114_v2.2.1.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 56.6902% of the 2693554 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/scm/brst/l2/schb/2015/09/mms2_scm_brst_l2_schb_20150901121114_v2.2.0.cdf. The most common cadence, 61036 [ns] = PT0.000061036S, occurred for 78.2690% of the 1974889 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms2/scm/srvy/l2/scsrvy/2015/09/mms2_scm_srvy_l2_scsrvy_20150902_v2.2.1.cdf. The most common cadence, 31250326 [ns] = PT0.03125S, occurred for 76.0320% of the 2097876 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/aspoc/srvy/l2/2015/09/mms3_aspoc_srvy_l2_20150901_v2.0.0.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

MMS Satellite Number 3 (from all.xml/observatory/description/@short)

MMS Satellite Number 3 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/dsp/fast/l2/bpsd/2015/09/mms3_dsp_fast_l2_bpsd_20150901_v2.1.1.cdf. The most common cadence, 2000024448 [ns] = PT2.000024S, occurred for 3.5638% of the 900 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/dsp/fast/l2/epsd/2015/09/mms3_dsp_fast_l2_epsd_20150901_v0.6.4.cdf. The most common cadence, 2000023933 [ns] = PT2.000024S, occurred for 73.5294% of the 25 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/dsp/slow/l2/bpsd/2015/09/mms3_dsp_slow_l2_bpsd_20150901_v2.1.0.cdf. The most common cadence, 16000186402 [ns] = PT16.000186S, occurred for 1.7881% of the 40 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/dsp/slow/l2/epsd/2015/09/mms3_dsp_slow_l2_epsd_20150901_v0.6.4.cdf. The most common cadence, 2000024448 [ns] = PT2.000024S, occurred for 3.2779% of the 900 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/amb/2015/09/mms3_edi_brst_l2_amb_20150901121114_v3.1.1.cdf. The most common cadence, 1000012000 [ns] = PT1.000012S, occurred for 57.6857% of the 334 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/amb/2015/09/mms3_edi_brst_l2_amb_20150901121114_v3.1.1.cdf. The most common cadence, 976563 [ns] = PT0.000976563S, occurred for 50.0001% of the 296960 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/amb-pm2/2016/01/mms3_edi_brst_l2_amb-pm2_20160104222503_v4.1.0.cdf. The most common cadence, 1000013017 [ns] = PT1.000013S, occurred for all 58 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/amb-pm2/2016/01/mms3_edi_brst_l2_amb-pm2_20160104222503_v4.1.0.cdf. The most common cadence, 976575 [ns] = PT0.000976575S, occurred for 78.7685% of the 47588 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/efield/2015/09/mms3_edi_brst_l2_efield_20150914141304_v1.6.2.cdf. The most common cadence, 7188493824 [ns] = PT7.188494S, occurred for 50.0000% of the 1 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/q0/2016/04/mms3_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 1000013000 [ns] = PT1.000013S, occurred for 39.2857% of the 11 timesteps. 

Counts based on variable 'epoch_gdu1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/q0/2016/04/mms3_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 97.1030% of the 3553 timesteps. 

Counts based on variable 'epoch_gdu2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/brst/l2/q0/2016/04/mms3_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 96.1538% of the 3475 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/srvy/l2/amb/2015/09/mms3_edi_srvy_l2_amb_20150901_v3.1.1.cdf. The most common cadence, 4000048896 [ns] = PT4.000049S, occurred for 18.6256% of the 1927 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/srvy/l2/amb/2015/09/mms3_edi_srvy_l2_amb_20150901_v3.1.1.cdf. The most common cadence, 31250000 [ns] = PT0.03125S, occurred for 94.5313% of the 1251987 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/srvy/l2/amb-pm2/2016/01/mms3_edi_srvy_l2_amb-pm2_20160104_v4.1.0.cdf. The most common cadence, 4000051328 [ns] = PT4.000051S, occurred for 15.8891% of the 1083 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/srvy/l2/amb-pm2/2016/01/mms3_edi_srvy_l2_amb-pm2_20160104_v4.1.0.cdf. The most common cadence, 31250401 [ns] = PT0.03125S, occurred for 20.5731% of the 179516 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edi/srvy/l2/efield/2015/09/mms3_edi_srvy_l2_efield_20150901_v1.6.2.cdf. The most common cadence, 3396187904 [ns] = PT3.396188S, occurred for 0.0414% of the 1 timesteps. 

Counts based on variable 'mms3_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/brst/l2/dce/2015/09/mms3_edp_brst_l2_dce_20150901121114_v2.2.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 76.6133% of the 3639683 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/brst/l2/hmfe/2015/09/mms3_edp_brst_l2_hmfe_20150901121114_v1.0.1.cdf. The most common cadence, 15259 [ns] = PT0.000015259S, occurred for 97.0698% of the 9796815 timesteps. 

Counts based on variable 'mms3_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/brst/l2/scpot/2015/09/mms3_edp_brst_l2_scpot_20150901121114_v2.4.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 76.6133% of the 3639683 timesteps. 

Counts based on variable 'mms3_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/fast/l2/dce/2015/09/mms3_edp_fast_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 31250376 [ns] = PT0.03125S, occurred for 86.1352% of the 1391888 timesteps. 

Counts based on variable 'mms3_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/fast/l2/scpot/2015/09/mms3_edp_fast_l2_scpot_20150901000000_v2.7.0.cdf. The most common cadence, 31250376 [ns] = PT0.03125S, occurred for 86.1352% of the 1391888 timesteps. 

Counts based on variable 'mms3_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/slow/l2/dce/2015/09/mms3_edp_slow_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 125001486 [ns] = PT0.125001S, occurred for 64.2007% of the 184116 timesteps. 

Counts based on variable 'mms3_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/slow/l2/scpot/2015/09/mms3_edp_slow_l2_scpot_20150901000000_v2.7.0.cdf. The most common cadence, 125001486 [ns] = PT0.125001S, occurred for 64.2007% of the 184116 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/edp/srvy/l2/hfesp/2015/09/mms3_edp_srvy_l2_hfesp_20150901_v0.4.0.cdf. The most common cadence, 16000192000 [ns] = PT16.000192S, occurred for 1.7599% of the 95 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/epd-eis/brst/l2/extof/2015/09/mms3_epd-eis_brst_l2_extof_20150901121114_v3.0.0.cdf. The most common cadence, 604780912 [ns] = PT0.604781S, occurred for 16.1964% of the 155 timesteps. 

MMS3 ExTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Burst proton_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst proton_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst proton_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst oxygen_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst oxygen_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst oxygen_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst helium_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst helium_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst helium_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst alpha_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst alpha_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst alpha_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst dump_P5_counts_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst dump_P5_cps_t0 [data available from 2020/09/24 to 2025/01/06]

MMS3 ExTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ExTOF-Burst dump_P5_flux_t0 [data available from 2020/09/24 to 2025/01/06]

Valid Time of Flight by Pulse Height Energy Events per second MMS3

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/epd-eis/brst/l2/phxtof/2015/09/mms3_epd-eis_brst_l2_phxtof_20150901121114_v3.0.0.cdf. The most common cadence, 604780912 [ns] = PT0.604781S, occurred for 16.1964% of the 155 timesteps. 

MMS3 PhxTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Burst proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Burst dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/epd-eis/srvy/l2/electronenergy/2015/09/mms3_epd-eis_srvy_l2_electronenergy_20150901_v3.0.0.cdf. The most common cadence, 2419125080 [ns] = PT2.419125S, occurred for 13.4183% of the 4791 timesteps. 

MMS3 ElectronEnergy-Survey electron_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ElectronEnergy-Survey electron_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ElectronEnergy-Survey electron_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ElectronEnergy-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ElectronEnergy-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ElectronEnergy-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ElectronEnergy-Survey electron_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 ElectronEnergy-Survey electron_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 ElectronEnergy-Survey electron_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 ElectronEnergy-Survey electron_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ElectronEnergy-Survey electron_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ElectronEnergy-Survey electron_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ElectronEnergy-Survey electron_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ElectronEnergy-Survey electron_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ElectronEnergy-Survey electron_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ElectronEnergy-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ElectronEnergy-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ElectronEnergy-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 ElectronEnergy-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ElectronEnergy-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ElectronEnergy-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 ElectronEnergy-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ElectronEnergy-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 ElectronEnergy-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/epd-eis/srvy/l2/extof/2015/09/mms3_epd-eis_srvy_l2_extof_20150901_v3.0.0.cdf. The most common cadence, 2419125080 [ns] = PT2.419125S, occurred for 14.8152% of the 3274 timesteps. 

MMS3 ExTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 ExTOF-Survey proton_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey proton_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey proton_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey oxygen_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey oxygen_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey oxygen_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey helium_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey helium_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey helium_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey alpha_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey alpha_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey alpha_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey dump_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey dump_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS3 ExTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 ExTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS3 ExTOF-Survey dump_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/epd-eis/srvy/l2/phxtof/2015/09/mms3_epd-eis_srvy_l2_phxtof_20150901_v3.0.0.cdf. The most common cadence, 2419125080 [ns] = PT2.419125S, occurred for 14.8152% of the 3274 timesteps. 

MMS3 PhxTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS3 PhxTOF-Survey proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS3 PhxTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS3 PhxTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS3 PhxTOF-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/feeps/brst/l2/electron/2015/09/mms3_feeps_brst_l2_electron_20150901121114_v7.1.1.cdf. The most common cadence, 302400000 [ns] = PT0.3024S, occurred for 37.6630% of the 722 timesteps. 

MMS3 FEEPS top side burst mode electron count error statistics sensor 1

MMS3 FEEPS top side burst mode electron count error statistics sensor 2

MMS3 FEEPS top side burst mode electron count error statistics sensor 3

MMS3 FEEPS top side burst mode electron count error statistics sensor 4

MMS3 FEEPS top side burst mode electron count error statistics sensor 5

MMS3 FEEPS top side burst mode electron count error statistics sensor 9

MMS3 FEEPS top side burst mode electron count error statistics sensor 10

MMS3 FEEPS top side burst mode electron count error statistics sensor 11

MMS3 FEEPS top side burst mode electron count error statistics sensor 12

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 1

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 2

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 3

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 4

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 5

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 9

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 10

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 11

MMS3 FEEPS bottom side burst mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/feeps/brst/l2/ion/2015/09/mms3_feeps_brst_l2_ion_20150901121114_v7.1.1.cdf. The most common cadence, 302400000 [ns] = PT0.3024S, occurred for 37.6630% of the 722 timesteps. 

MMS3 FEEPS top side burst mode ion count error statistics sensor 6

MMS3 FEEPS top side burst mode ion count error statistics sensor 7

MMS3 FEEPS top side burst mode ion count error statistics sensor 8

MMS3 FEEPS bottom side burst mode ion count error statistics sensor 6

MMS3 FEEPS bottom side burst mode ion count error statistics sensor 7

MMS3 FEEPS bottom side burst mode ion count error statistics sensor 8

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/feeps/srvy/l2/electron/2015/09/mms3_feeps_srvy_l2_electron_20150901000000_v7.1.1.cdf. The most common cadence, 2419200000 [ns] = PT2.4192S, occurred for 9.5741% of the 2268 timesteps. 

MMS3 FEEPS bottom side survey mode electron count rate sensor 10

MMS3 FEEPS bottom side survey mode electron count rate sensor 11

MMS3 FEEPS bottom side survey mode electron count rate sensor 12

MMS3 FEEPS top side survey mode electron count error statistics sensor 1

MMS3 FEEPS top side survey mode electron count error statistics sensor 2

MMS3 FEEPS top side survey mode electron count error statistics sensor 3

MMS3 FEEPS top side survey mode electron count error statistics sensor 4

MMS3 FEEPS top side survey mode electron count error statistics sensor 5

MMS3 FEEPS top side survey mode electron count error statistics sensor 9

MMS3 FEEPS top side survey mode electron count error statistics sensor 10

MMS3 FEEPS top side survey mode electron count error statistics sensor 11

MMS3 FEEPS top side survey mode electron count error statistics sensor 12

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 1

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 2

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 3

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 4

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 5

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 9

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 10

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 11

MMS3 FEEPS bottom side survey mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/feeps/srvy/l2/ion/2015/09/mms3_feeps_srvy_l2_ion_20150901000000_v7.1.1.cdf. The most common cadence, 2419200000 [ns] = PT2.4192S, occurred for 9.5741% of the 2268 timesteps. 

MMS3 FEEPS top side survey mode ion count error statistics sensor 6

MMS3 FEEPS top side survey mode ion count error statistics sensor 7

MMS3 FEEPS top side survey mode ion count error statistics sensor 8

MMS3 FEEPS bottom side survey mode ion count error statistics sensor 6

MMS3 FEEPS bottom side survey mode ion count error statistics sensor 7

MMS3 FEEPS bottom side survey mode ion count error statistics sensor 8

Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 3

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fgm/brst/l2/2015/09/mms3_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 7812593 [ns] = PT0.007813S, occurred for 99.0989% of the 73570 timesteps. 

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fgm/brst/l2/2015/09/mms3_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 21 timesteps. 

Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 3

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fgm/srvy/l2/2015/09/mms3_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 62500752 [ns] = PT0.062501S, occurred for 54.2056% of the 593760 timesteps. 

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fgm/srvy/l2/2015/09/mms3_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2883 timesteps. 

MMS Satellite Number 3 Dual Electron Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/brst/l2/des-dist/2015/09/mms3_fpi_brst_l2_des-dist_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0047% of the 18751 timesteps. 

[CDAWeb List/Download/Create ONLY] MMS3 FPI/DES burst sky-map instrument distribution

MMS3 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even)

MMS3 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even)

MMS3 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even)

MMS3 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even)

MMS3 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even)

MMS3 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even)

MMS3 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even)

MMS3 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even)

MMS3 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even)

MMS3 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even)

MMS3 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd)

MMS3 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even)

MMS3 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS3 FPI/DES burst sky-map instrument distribution

MMS3 FPI/DES vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS3 FPI/DES compression lossless/lossy indicator at survey-start time

---> MMS3 FPI/DES Del-Phi (obs spin-phase) count at burst-start time

---> MMS3 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 3 Dual Electron Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/brst/l2/des-moms/2015/09/mms3_fpi_brst_l2_des-moms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0047% of the 18751 timesteps. 

MMS3 FPI/DES 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS3 FPI/DES electron pitch-angle distribution for "low" energies during this burst

---> MMS3 FPI/DES electron pitch-angle distribution for "mid" energies during this burst

---> MMS3 FPI/DES electron pitch-angle distribution for "high" energies during this burst

MMS3 FPI/DES electron energy spectrum "near" +X_DSC during this burst

---> MMS3 FPI/DES electron energy spectrum "near" -X_DSC during this burst

---> MMS3 FPI/DES electron energy spectrum "near" +Y_DSC during this burst

---> MMS3 FPI/DES electron energy spectrum "near" -Y_DSC during this burst

---> MMS3 FPI/DES electron energy spectrum "near" +Z_DSC during this burst

---> MMS3 FPI/DES electron energy spectrum "near" -Z_DSC during this burst

MMS3 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this burst

---> MMS3 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this burst

---> MMS3 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this burst

MMS3 FPI/DES omni-directional electron energy spectrum during this burst

---> MMS3 FPI/DES electron number density error during this burst

MMS3 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS3 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS3 FPI/DES electron bulk-velocity DBCS vector during this burst

MMS3 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this burst

MMS3 FPI/DES electron bulk-velocity GSE vector during this burst

MMS3 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this burst

MMS3 FPI/DES electron bulk-velocity spintone vector in DBCS during this burst

MMS3 FPI/DES electron bulk-velocity spintone vector in GSE during this burst

MMS3 FPI/DES electron pressure tensor DBCS matrix during this burst

MMS3 FPI/DES electron pressure tensor GSE matrix during this burst

MMS3 FPI/DES electron temperature tensor DBCS matrix during this burst

MMS3 FPI/DES electron temperature tensor GSE matrix during this burst

MMS Satellite Number 3 Dual Electron Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/brst/l2/des-partmoms/2015/09/mms3_fpi_brst_l2_des-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0047% of the 18751 timesteps. 

MMS3 FPI/DES partial electron bulk-velocity vector in DBCS during this burst

MMS3 FPI/DES partial electron bulk-velocity vector in GSE during this burst

MMS3 FPI/DES partial electron pressure tensor in DBCS during this burst

MMS3 FPI/DES partial electron pressure tensor in GSE during this burst

MMS3 FPI/DES partial electron temperature tensor in DBCS during this burst

MMS3 FPI/DES partial electron temperature tensor in GSE during this burst

MMS3 FPI/DES partial electron parallel temperature during this burst

MMS3 FPI/DES partial electron perpendicular temperature during this burst

MMS Satellite Number 3 Dual Ion Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/brst/l2/dis-dist/2015/09/mms3_fpi_brst_l2_dis-dist_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0233% of the 3287 timesteps. 

[CDAWeb List/Download/Create ONLY] MMS3 FPI/DIS burst sky-map instrument distribution

MMS3 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd)

MMS3 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even)

MMS3 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS3 FPI/DIS burst sky-map instrument distribution

MMS3 FPI/DIS vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 3 Dual Ion Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/brst/l2/dis-moms/2015/09/mms3_fpi_brst_l2_dis-moms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0233% of the 3287 timesteps. 

MMS3 FPI/DIS 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS3 FPI/DIS ion energy spectrum "near" +X_DSC during this burst

---> MMS3 FPI/DIS ion energy spectrum "near" -X_DSC during this burst

---> MMS3 FPI/DIS ion energy spectrum "near" +Y_DSC during this burst

---> MMS3 FPI/DIS ion energy spectrum "near" -Y_DSC during this burst

---> MMS3 FPI/DIS ion energy spectrum "near" +Z_DSC during this burst

---> MMS3 FPI/DIS ion energy spectrum "near" -Z_DSC during this burst

MMS3 FPI/DIS omni-directional ion energy spectrum during this burst

MMS3 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS3 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this burst

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this burst

MMS3 FPI/DIS ion bulk-velocity spintone vector in DBCS during this burst

MMS3 FPI/DIS ion bulk-velocity spintone vector in GSE during this burst

MMS3 FPI/DIS ion temperature tensor DBCS matrix during this burst

MMS3 FPI/DIS ion temperature tensor GSE matrix during this burst

MMS Satellite Number 3 Dual Ion Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/brst/l2/dis-partmoms/2015/09/mms3_fpi_brst_l2_dis-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.0233% of the 3287 timesteps. 

MMS3 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst

MMS3 FPI/DIS partial ion bulk-velocity vector in GSE during this burst

MMS3 FPI/DIS partial ion pressure tensor in DBCS during this burst

MMS3 FPI/DIS partial ion pressure tensor in GSE during this burst

MMS3 FPI/DIS partial ion temperature tensor in DBCS during this burst

MMS3 FPI/DIS partial ion temperature tensor in GSE during this burst

MMS3 FPI/DIS partial ion perpendicular temperature during this burst

MMS Satellite Number 3 Dual Electron Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/des-dist/2015/09/mms3_fpi_fast_l2_des-dist_20150901080000_v3.4.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps. 

MMS3 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS3 FPI/DES fast sky-map instrument distribution 1-sigma error

MMS3 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS3 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS3 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 3 Dual Electron Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/des-moms/2015/09/mms3_fpi_fast_l2_des-moms_20150901080000_v3.4.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps. 

MMS3 FPI/DES 32-bit vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS3 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

---> MMS3 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS3 FPI/DES electron pitch-angle distribution for "low" energies during this survey

---> MMS3 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

---> MMS3 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS3 FPI/DES electron energy spectrum "near" +X_DSC during this survey

---> MMS3 FPI/DES electron energy spectrum "near" -X_DSC during this survey

---> MMS3 FPI/DES electron energy spectrum "near" +Y_DSC during this survey

---> MMS3 FPI/DES electron energy spectrum "near" -Y_DSC during this survey

---> MMS3 FPI/DES electron energy spectrum "near" +Z_DSC during this survey

---> MMS3 FPI/DES electron energy spectrum "near" -Z_DSC during this survey

MMS3 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this survey

---> MMS3 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this survey

---> MMS3 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this survey

MMS3 FPI/DES omni-directional electron energy spectrum during this survey

---> MMS3 FPI/DES electron number density error during this survey

MMS3 FPI/DES electron bulk-velocity DBCS vector during this survey

MMS3 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey

MMS3 FPI/DES electron bulk-velocity GSE vector during this survey

MMS3 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey

MMS3 FPI/DES electron bulk-velocity spintone vector in DBCS during this survey

MMS3 FPI/DES electron bulk-velocity spintone vector in GSE during this survey

MMS3 FPI/DES electron pressure tensor DBCS matrix during this survey

MMS3 FPI/DES electron pressure tensor GSE matrix during this survey

MMS3 FPI/DES electron temperature tensor DBCS matrix during this survey

MMS3 FPI/DES electron temperature tensor GSE matrix during this survey

MMS Satellite Number 3 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/des-momsaux/2015/09/mms3_fpi_fast_l2_des-momsaux_20150901080000_v3.4.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps.

MMS3 FPI/DES vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS3 FPI/DES partial electron bulk-velocity vector in DBCS during this survey

MMS3 FPI/DES partial electron bulk-velocity vector in GSE during this survey

MMS3 FPI/DES partial electron pressure tensor in DBCS during this survey

MMS3 FPI/DES partial electron pressure tensor in GSE during this survey

MMS3 FPI/DES partial electron temperature tensor in DBCS during this survey

MMS3 FPI/DES partial electron temperature tensor in GSE during this survey

MMS3 FPI/DES partial electron parallel temperature during this survey

MMS3 FPI/DES partial electron perpendicular temperature during this survey

MMS3 FPI/DES recommended energy index for partial moments during this survey

MMS3 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

MMS3 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS3 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

MMS3 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS3 FPI/DES electron energy spectrum "near" +X_DBCS during this survey

MMS3 FPI/DES electron energy spectrum "near" -X_DBCS during this survey

MMS3 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey

MMS3 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey

MMS3 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey

MMS3 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey

MMS3 FPI/DES electron energy parallel to the magnetic field direction during this survey

MMS3 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey

MMS3 FPI/DES electron energy perpendicular to the magnetic field direction during this survey

MMS3 FPI/DES electron bulk-velocity vector in DBCS during this survey

MMS3 FPI/DES electron bulk-velocity vector in GSE during this survey

MMS3 FPI/DES electron pressure tensor in DBCS during this survey

MMS3 FPI/DES electron temperature tensor in DBCS during this survey

MMS3 FPI/DES electron temperature tensor in GSE during this survey

MMS3 FPI/DES electron heat-flux vector in DBCS during this survey

MMS3 FPI/DES electron heat-flux vector in GSE during this survey

MMS3 FPI/DES Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 3 Dual Electron Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/des-partmoms/2015/09/mms3_fpi_fast_l2_des-partmoms_20150901080000_v3.3.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps. 

MMS Satellite Number 3 Dual Ion Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/dis-dist/2015/09/mms3_fpi_fast_l2_dis-dist_20150901080000_v3.4.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps. 

MMS3 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS3 FPI/DIS fast sky-map instrument distribution 1-sigma error

MMS3 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 3 Dual Ion Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/dis-moms/2015/09/mms3_fpi_fast_l2_dis-moms_20150901080000_v3.4.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps. 

MMS3 FPI/DIS vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS3 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey

---> MMS3 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

---> MMS3 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

---> MMS3 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

---> MMS3 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

---> MMS3 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS3 FPI/DIS omni-directional ion energy spectrum during this survey

MMS3 FPI/DIS ion bulk-velocity vector in DBCS during this survey

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey

MMS Satellite Number 3 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/dis-momsaux/2015/09/mms3_fpi_fast_l2_dis-momsaux_20150901080000_v3.4.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps.

MMS3 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey

MMS3 FPI/DIS partial ion bulk-velocity vector in GSE during this survey

MMS3 FPI/DIS partial ion pressure tensor in DBCS during this survey

MMS3 FPI/DIS partial ion pressure tensor in GSE during this survey

MMS3 FPI/DIS partial ion temperature tensor in DBCS during this survey

MMS3 FPI/DIS partial ion temperature tensor in GSE during this survey

MMS3 FPI/DIS partial ion parallel temperature during this survey

MMS3 FPI/DIS partial ion perpendicular temperature during this survey

MMS3 FPI/DIS recommended energy index for partial moments during this survey

MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS3 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

MMS3 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

MMS3 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

MMS3 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

MMS3 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS3 FPI/DIS Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 3 Dual Ion Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/fast/l2/dis-partmoms/2015/09/mms3_fpi_fast_l2_dis-partmoms_20150901080000_v3.3.0.cdf. The most common cadence, 4500019000 [ns] = PT4.500019S, occurred for 26.3158% of the 45 timesteps. 

MMS Satellite Number 3 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/slow/l2/des-dist/2015/09/mms3_fpi_slow_l2_des-dist_20150902002742_v3.4.0.cdf. The most common cadence, 58084069000 [ns] = PT58.084069S, occurred for 2.7523% of the 3 timesteps.

MMS3 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 3 Dual Electron Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/slow/l2/des-moms/2015/09/mms3_fpi_slow_l2_des-moms_20150902002742_v3.4.0.cdf. The most common cadence, 58084069000 [ns] = PT58.084069S, occurred for 2.7523% of the 3 timesteps.

MMS Satellite Number 3 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/slow/l2/des-momsaux/2015/09/mms3_fpi_slow_l2_des-momsaux_20150902002742_v3.4.0.cdf. The most common cadence, 58084069000 [ns] = PT58.084069S, occurred for 2.7523% of the 3 timesteps.

MMS Satellite Number 3 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/slow/l2/dis-dist/2015/09/mms3_fpi_slow_l2_dis-dist_20150902002742_v3.4.0.cdf. The most common cadence, 58084069000 [ns] = PT58.084069S, occurred for 2.7523% of the 3 timesteps.

MMS3 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 3 Dual Ion Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/slow/l2/dis-moms/2015/09/mms3_fpi_slow_l2_dis-moms_20150902002742_v3.4.0.cdf. The most common cadence, 58084069000 [ns] = PT58.084069S, occurred for 2.7523% of the 3 timesteps.

MMS Satellite Number 3 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/fpi/slow/l2/dis-momsaux/2015/09/mms3_fpi_slow_l2_dis-momsaux_20150902002742_v3.4.0.cdf. The most common cadence, 58084069000 [ns] = PT58.084069S, occurred for 2.7523% of the 3 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/hpca/brst/l2/ion/2015/09/mms3_hpca_brst_l2_ion_20150901121114_v4.1.0.cdf. The most common cadence, 624988000 [ns] = PT0.624988S, occurred for 37.5405% of the 348 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/hpca/brst/l2/moments/2015/09/mms3_hpca_brst_l2_moments_20150901121114_v4.1.0.cdf. The most common cadence, 9999749000 [ns] = PT9.999749S, occurred for 51.7857% of the 29 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/hpca/srvy/l2/ion/2015/09/mms3_hpca_srvy_l2_ion_20150901000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 50.0000% of the 1262 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/hpca/srvy/l2/moments/2015/09/mms3_hpca_srvy_l2_moments_20150901000000_v4.1.0.cdf. The most common cadence, 9999746000 [ns] = PT9.999746S, occurred for 24.3590% of the 38 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/hpca/srvy/l2/tof-counts/2018/11/mms3_hpca_srvy_l2_tof-counts_20181115000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 92.5140% of the 74088 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/mec/brst/l2/epht89d/2015/12/mms3_mec_brst_l2_epht89d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Geocentric Equatorial Inertial (GEI/J2000) position vector of mms3 (km)

Velocity of mms3 spacecraft in GEI/J2000 (i.e. ECI) coordinates (km/s)

Geocentric Solar Magnetospheric (GSM) position vector of mms3 (km)

Geocentric Solar Ecliptic (J2000 Pole, GSE2000) position vector of mms3 (km)

Geodetic height of mms3 spacecraft. (Height above WGS84 Spheroid.)

Geodetic latitude and longitude of southern footpoint (100km geodetic height) of field threading the mms3 spacecraft

Geodetic latitude and longitude of northern footpoint (100km geodetic height) of field threading the mms3 spacecraft

GSM position southern footpoint (100km geodetic height) of field threading the mms3 spacecraft

Magnetic field (in GSM) at southern footpoint (100km geodetic height) of field threading the mms3 spacecraft

GSM position northern footpoint (100km geodetic height) of field threading the mms3 spacecraft

Magnetic field (in GSM) at northern footpoint (100km geodetic height) of field threading the mms3 spacecraft

GSM position of min-B point of field threading the mms3 spacecraft

Magnetic field (in GSM) at min-B point of field threading the mms3 spacecraft

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/mec/brst/l2/epht89q/2015/12/mms3_mec_brst_l2_epht89q_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/mec/brst/l2/ephts04d/2015/12/mms3_mec_brst_l2_ephts04d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/mec/srvy/l2/epht89d/2015/09/mms3_mec_srvy_l2_epht89d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/mec/srvy/l2/epht89q/2015/09/mms3_mec_srvy_l2_epht89q_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/mec/srvy/l2/ephts04d/2015/09/mms3_mec_srvy_l2_ephts04d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/scm/brst/l2/scb/2015/09/mms3_scm_brst_l2_scb_20150901121114_v2.2.1.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 76.6133% of the 3639683 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/scm/brst/l2/schb/2015/09/mms3_scm_brst_l2_schb_20150901121114_v2.2.0.cdf. The most common cadence, 61036 [ns] = PT0.000061036S, occurred for 88.2768% of the 2227407 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms3/scm/srvy/l2/scsrvy/2015/09/mms3_scm_srvy_l2_scsrvy_20150902_v2.2.1.cdf. The most common cadence, 31250376 [ns] = PT0.03125S, occurred for 96.8559% of the 2672450 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/aspoc/srvy/l2/2015/09/mms4_aspoc_srvy_l2_20150901_v2.0.0.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

MMS Satellite Number 4 (from all.xml/observatory/description/@short)

MMS Satellite Number 4 (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/dsp/fast/l2/bpsd/2015/09/mms4_dsp_fast_l2_bpsd_20150901_v2.1.1.cdf. The most common cadence, 2000024192 [ns] = PT2.000024S, occurred for 3.5504% of the 900 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/dsp/fast/l2/epsd/2015/09/mms4_dsp_fast_l2_epsd_20150901_v0.6.3.cdf. The most common cadence, 2000024192 [ns] = PT2.000024S, occurred for 3.5504% of the 900 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/dsp/slow/l2/bpsd/2015/09/mms4_dsp_slow_l2_bpsd_20150901_v2.1.0.cdf. The most common cadence, 16000197118 [ns] = PT16.000197S, occurred for 2.1563% of the 48 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/dsp/slow/l2/epsd/2015/09/mms4_dsp_slow_l2_epsd_20150901_v0.6.3.cdf. The most common cadence, 16000197118 [ns] = PT16.000197S, occurred for 2.1563% of the 48 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/amb/2015/09/mms4_edi_brst_l2_amb_20150902133904_v3.2.1.cdf. The most common cadence, 1000012000 [ns] = PT1.000012S, occurred for 55.2699% of the 215 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/amb/2015/09/mms4_edi_brst_l2_amb_20150902133904_v3.2.1.cdf. The most common cadence, 976563 [ns] = PT0.000976563S, occurred for 50.0001% of the 199680 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/amb-pm2/2016/01/mms4_edi_brst_l2_amb-pm2_20160104222503_v4.2.0.cdf. The most common cadence, 1000013135 [ns] = PT1.000013S, occurred for all 59 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/amb-pm2/2016/01/mms4_edi_brst_l2_amb-pm2_20160104222503_v4.2.0.cdf. The most common cadence, 976575 [ns] = PT0.000976575S, occurred for 67.2114% of the 41294 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/efield/2015/09/mms4_edi_brst_l2_efield_20150914141304_v1.6.2.cdf. The most common cadence, 11333026816 [ns] = PT11.333027S, occurred for 50.0000% of the 1 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/q0/2016/04/mms4_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 1000013000 [ns] = PT1.000013S, occurred for 46.4286% of the 13 timesteps. 

Counts based on variable 'epoch_gdu1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/q0/2016/04/mms4_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 93.3981% of the 3268 timesteps. 

Counts based on variable 'epoch_gdu2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/brst/l2/q0/2016/04/mms4_edi_brst_l2_q0_20160412222414_v4.0.0.cdf. The most common cadence, 7812500 [ns] = PT0.007812S, occurred for 96.0044% of the 3460 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/srvy/l2/amb/2015/09/mms4_edi_srvy_l2_amb_20150902_v3.2.1.cdf. The most common cadence, 4000048832 [ns] = PT4.000049S, occurred for 38.0760% of the 4437 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/srvy/l2/amb/2015/09/mms4_edi_srvy_l2_amb_20150902_v3.2.1.cdf. The most common cadence, 31250000 [ns] = PT0.03125S, occurred for 94.5313% of the 1410134 timesteps. 

Counts based on variable 'epoch_timetag' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/srvy/l2/amb-pm2/2016/01/mms4_edi_srvy_l2_amb-pm2_20160104_v4.2.0.cdf. The most common cadence, 4000051904 [ns] = PT4.000052S, occurred for 13.2336% of the 902 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/srvy/l2/amb-pm2/2016/01/mms4_edi_srvy_l2_amb-pm2_20160104_v4.2.0.cdf. The most common cadence, 31250406 [ns] = PT0.03125S, occurred for 24.0317% of the 209695 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edi/srvy/l2/efield/2015/09/mms4_edi_srvy_l2_efield_20150902_v1.6.2.cdf. The most common cadence, 4562412864 [ns] = PT4.562413S, occurred for 0.4717% of the 1 timesteps. 

Counts based on variable 'mms4_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/brst/l2/dce/2015/09/mms4_edp_brst_l2_dce_20150901121114_v2.2.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 79.0411% of the 3755526 timesteps. 

L2 DC E Field calibrated for SDP and ADP (data begins 2023/07/04)

L2 DC E Field (GSE coords) calibrated for SDP and ADP, all flag values included (No data after 7/3/2023)

L2 DC E Field (DSL coords) calibrated for SDP and ADP, all flag values included  (No data after 7/3/2023) 

L2 DC E Parallel Field calibrated for SDP and ADP (No data after 7/3/2023)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/brst/l2/hmfe/2015/09/mms4_edp_brst_l2_hmfe_20150901121114_v1.0.1.cdf. The most common cadence, 15259 [ns] = PT0.000015259S, occurred for 97.3753% of the 7402638 timesteps. 

Counts based on variable 'mms4_edp_epoch_brst_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/brst/l2/scpot/2015/09/mms4_edp_brst_l2_scpot_20150901121114_v2.4.0.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 79.0411% of the 3755526 timesteps. 

Counts based on variable 'mms4_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/fast/l2/dce/2015/09/mms4_edp_fast_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 31250378 [ns] = PT0.03125S, occurred for 75.4733% of the 1224235 timesteps. 

L2 DC E Field (DSL coords) calibrated for SDP and ADP, all flag values included (No data after 7/3/2023)

L2 DC E Parallel Field with error calibrated for SDP and ADP (No data after 7/3/2023)

Counts based on variable 'mms4_edp_epoch_fast_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/fast/l2/scpot/2015/09/mms4_edp_fast_l2_scpot_20150901000000_v2.7.0.cdf. The most common cadence, 31250378 [ns] = PT0.03125S, occurred for 75.4733% of the 1224235 timesteps. 

Counts based on variable 'mms4_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/slow/l2/dce/2015/09/mms4_edp_slow_l2_dce_20150901_v2.1.0.cdf. The most common cadence, 125001510 [ns] = PT0.125002S, occurred for 82.0412% of the 233915 timesteps. 

Counts based on variable 'mms4_edp_epoch_slow_l2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/slow/l2/scpot/2015/09/mms4_edp_slow_l2_scpot_20150901000000_v2.7.0.cdf. The most common cadence, 125001510 [ns] = PT0.125002S, occurred for 82.0412% of the 233915 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/edp/srvy/l2/hfesp/2015/09/mms4_edp_srvy_l2_hfesp_20150901_v0.4.0.cdf. The most common cadence, 16000196992 [ns] = PT16.000197S, occurred for 5.2056% of the 281 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/epd-eis/brst/l2/extof/2015/09/mms4_epd-eis_brst_l2_extof_20150901121114_v3.0.0.cdf. The most common cadence, 605000019 [ns] = PT0.605S, occurred for 48.0669% of the 460 timesteps. 

MMS4 ExTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Burst proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst helium_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst helium_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst helium_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst alpha_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst alpha_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst alpha_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ExTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ExTOF-Burst dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Valid Time of Flight by Pulse Height Energy Events per second MMS4

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/epd-eis/brst/l2/phxtof/2015/09/mms4_epd-eis_brst_l2_phxtof_20150901121114_v3.0.0.cdf. The most common cadence, 605000019 [ns] = PT0.605S, occurred for 48.0669% of the 460 timesteps. 

MMS4 PhxTOF-Burst proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Burst proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Burst dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Burst dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Burst dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/epd-eis/srvy/l2/electronenergy/2015/09/mms4_epd-eis_srvy_l2_electronenergy_20150901_v3.0.0.cdf. The most common cadence, 2420000076 [ns] = PT2.42S, occurred for 12.0238% of the 1133 timesteps. 

MMS4 ElectronEnergy-Survey electron_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ElectronEnergy-Survey electron_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ElectronEnergy-Survey electron_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ElectronEnergy-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ElectronEnergy-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ElectronEnergy-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ElectronEnergy-Survey electron_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ElectronEnergy-Survey electron_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ElectronEnergy-Survey electron_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ElectronEnergy-Survey electron_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ElectronEnergy-Survey electron_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ElectronEnergy-Survey electron_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ElectronEnergy-Survey electron_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ElectronEnergy-Survey electron_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ElectronEnergy-Survey electron_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ElectronEnergy-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ElectronEnergy-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ElectronEnergy-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ElectronEnergy-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ElectronEnergy-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ElectronEnergy-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 ElectronEnergy-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ElectronEnergy-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 ElectronEnergy-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/epd-eis/srvy/l2/extof/2015/09/mms4_epd-eis_srvy_l2_extof_20150901_v3.0.0.cdf. The most common cadence, 2420125008 [ns] = PT2.420125S, occurred for 23.2722% of the 6115 timesteps. 

MMS4 ExTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey helium_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey helium_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey helium_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 ExTOF-Survey proton_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey proton_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey proton_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey oxygen_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey oxygen_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey oxygen_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey helium_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey helium_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey helium_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey alpha_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey alpha_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey alpha_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey alpha_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey alpha_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey alpha_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey dump_P5_counts_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey dump_P5_cps_t0 [data available from 2020/02/04 to 2025/01/06]

MMS4 ExTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 ExTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2020/02/03]

MMS4 ExTOF-Survey dump_P5_flux_t0 [data available from 2020/02/04 to 2025/01/06]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/epd-eis/srvy/l2/phxtof/2015/09/mms4_epd-eis_srvy_l2_phxtof_20150901_v3.0.0.cdf. The most common cadence, 2420125008 [ns] = PT2.420125S, occurred for 23.2760% of the 6116 timesteps. 

MMS4 PhxTOF-Survey proton_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey proton_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey proton_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey oxygen_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey oxygen_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey oxygen_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey dump_P6_counts_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey dump_P6_cps_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey dump_P6_flux_t0 [data available beginning on 2025/01/06]

MMS4 PhxTOF-Survey proton_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey proton_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey proton_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey oxygen_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey oxygen_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey oxygen_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey proton_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey proton_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey proton_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey oxygen_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey oxygen_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey oxygen_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey proton_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey proton_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey proton_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey oxygen_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey oxygen_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey oxygen_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey dump_P3_counts_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey dump_P4_counts_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey dump_P5_counts_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey dump_P3_cps_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey dump_P4_cps_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey dump_P5_cps_t0 [data available from 2019/12/20 to 2025/01/06]

MMS4 PhxTOF-Survey dump_P3_flux_t0 [data available from 2015/07/02 to 2016/09/28]

MMS4 PhxTOF-Survey dump_P4_flux_t0 [data available from 2016/09/29 to 2019/12/19]

MMS4 PhxTOF-Survey dump_P5_flux_t0 [data available from 2019/12/20 to 2025/01/06]

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/feeps/brst/l2/electron/2015/09/mms4_feeps_brst_l2_electron_20150901121114_v7.1.1.cdf. The most common cadence, 302511872 [ns] = PT0.302512S, occurred for 33.0203% of the 633 timesteps. 

MMS4 FEEPS top side burst mode electron count error statistics sensor 1

MMS4 FEEPS top side burst mode electron count error statistics sensor 2

MMS4 FEEPS top side burst mode electron count error statistics sensor 3

MMS4 FEEPS top side burst mode electron count error statistics sensor 4

MMS4 FEEPS top side burst mode electron count error statistics sensor 5

MMS4 FEEPS top side burst mode electron count error statistics sensor 9

MMS4 FEEPS top side burst mode electron count error statistics sensor 10

MMS4 FEEPS top side burst mode electron count error statistics sensor 11

MMS4 FEEPS top side burst mode electron count error statistics sensor 12

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 1

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 2

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 3

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 4

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 5

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 9

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 10

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 11

MMS4 FEEPS bottom side burst mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/feeps/brst/l2/ion/2015/09/mms4_feeps_brst_l2_ion_20150901121114_v7.1.1.cdf. The most common cadence, 302511872 [ns] = PT0.302512S, occurred for 33.0203% of the 633 timesteps. 

MMS4 FEEPS top side burst mode ion count error statistics sensor 6

MMS4 FEEPS top side burst mode ion count error statistics sensor 7

MMS4 FEEPS top side burst mode ion count error statistics sensor 8

MMS4 FEEPS bottom side burst mode ion count error statistics sensor 6

MMS4 FEEPS bottom side burst mode ion count error statistics sensor 7

MMS4 FEEPS bottom side burst mode ion count error statistics sensor 8

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/feeps/srvy/l2/electron/2015/09/mms4_feeps_srvy_l2_electron_20150901000000_v7.1.1.cdf. The most common cadence, 2420096000 [ns] = PT2.420096S, occurred for 11.7691% of the 2673 timesteps. 

MMS4 FEEPS bottom side survey mode electron count rate sensor 10

MMS4 FEEPS bottom side survey mode electron count rate sensor 11

MMS4 FEEPS bottom side survey mode electron count rate sensor 12

MMS4 FEEPS top side survey mode electron count error statistics sensor 1

MMS4 FEEPS top side survey mode electron count error statistics sensor 2

MMS4 FEEPS top side survey mode electron count error statistics sensor 3

MMS4 FEEPS top side survey mode electron count error statistics sensor 4

MMS4 FEEPS top side survey mode electron count error statistics sensor 5

MMS4 FEEPS top side survey mode electron count error statistics sensor 9

MMS4 FEEPS top side survey mode electron count error statistics sensor 10

MMS4 FEEPS top side survey mode electron count error statistics sensor 11

MMS4 FEEPS top side survey mode electron count error statistics sensor 12

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 1

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 2

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 3

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 4

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 5

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 9

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 10

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 11

MMS4 FEEPS bottom side survey mode electron count error statistics sensor 12

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/feeps/srvy/l2/ion/2015/09/mms4_feeps_srvy_l2_ion_20150901000000_v7.1.1.cdf. The most common cadence, 2420096000 [ns] = PT2.420096S, occurred for 11.7691% of the 2673 timesteps. 

MMS4 FEEPS top side survey mode ion count error statistics sensor 6

MMS4 FEEPS top side survey mode ion count error statistics sensor 7

MMS4 FEEPS top side survey mode ion count error statistics sensor 8

MMS4 FEEPS bottom side survey mode ion count error statistics sensor 6

MMS4 FEEPS bottom side survey mode ion count error statistics sensor 7

MMS4 FEEPS bottom side survey mode ion count error statistics sensor 8

Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 4

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fgm/brst/l2/2015/09/mms4_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 7812595 [ns] = PT0.007813S, occurred for 57.4240% of the 42631 timesteps. 

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fgm/brst/l2/2015/09/mms4_fgm_brst_l2_20150901121114_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 21 timesteps. 

Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 4

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fgm/srvy/l2/2015/09/mms4_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 62500756 [ns] = PT0.062501S, occurred for 37.3993% of the 410252 timesteps. 

Counts based on variable 'Epoch_state' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fgm/srvy/l2/2015/09/mms4_fgm_srvy_l2_20150901_v4.18.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2883 timesteps. 

MMS Satellite Number 4 Dual Electron Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/brst/l2/des-dist/2015/09/mms4_fpi_brst_l2_des-dist_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0463% of the 18761 timesteps. 

[CDAWeb List/Download/Create ONLY] MMS4 FPI/DES burst sky-map instrument distribution

MMS4 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even)

MMS4 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even)

MMS4 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even)

MMS4 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even)

MMS4 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even)

MMS4 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even)

MMS4 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even)

MMS4 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even)

MMS4 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even)

MMS4 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even)

MMS4 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd)

MMS4 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even)

MMS4 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS4 FPI/DES burst sky-map instrument distribution

MMS4 FPI/DES vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS4 FPI/DES compression lossless/lossy indicator at survey-start time

---> MMS4 FPI/DES Del-Phi (obs spin-phase) count at burst-start time

---> MMS4 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 4 Dual Electron Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/brst/l2/des-moms/2015/09/mms4_fpi_brst_l2_des-moms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0463% of the 18761 timesteps. 

MMS4 FPI/DES 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS4 FPI/DES electron pitch-angle distribution for "low" energies during this burst

---> MMS4 FPI/DES electron pitch-angle distribution for "mid" energies during this burst

---> MMS4 FPI/DES electron pitch-angle distribution for "high" energies during this burst

MMS4 FPI/DES electron energy spectrum "near" +X_DSC during this burst

---> MMS4 FPI/DES electron energy spectrum "near" -X_DSC during this burst

---> MMS4 FPI/DES electron energy spectrum "near" +Y_DSC during this burst

---> MMS4 FPI/DES electron energy spectrum "near" -Y_DSC during this burst

---> MMS4 FPI/DES electron energy spectrum "near" +Z_DSC during this burst

---> MMS4 FPI/DES electron energy spectrum "near" -Z_DSC during this burst

MMS4 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this burst

---> MMS4 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this burst

---> MMS4 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this burst

MMS4 FPI/DES omni-directional electron energy spectrum during this burst

---> MMS4 FPI/DES electron number density error during this burst

MMS4 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS4 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS4 FPI/DES electron bulk-velocity DBCS vector during this burst

MMS4 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this burst

MMS4 FPI/DES electron bulk-velocity GSE vector during this burst

MMS4 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this burst

MMS4 FPI/DES electron bulk-velocity spintone vector in DBCS during this burst

MMS4 FPI/DES electron bulk-velocity spintone vector in GSE during this burst

MMS4 FPI/DES electron pressure tensor DBCS matrix during this burst

MMS4 FPI/DES electron pressure tensor GSE matrix during this burst

MMS4 FPI/DES electron temperature tensor DBCS matrix during this burst

MMS4 FPI/DES electron temperature tensor GSE matrix during this burst

MMS Satellite Number 4 Dual Electron Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/brst/l2/des-partmoms/2015/09/mms4_fpi_brst_l2_des-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for 97.0463% of the 18761 timesteps. 

MMS4 FPI/DES partial electron bulk-velocity vector in DBCS during this burst

MMS4 FPI/DES partial electron bulk-velocity vector in GSE during this burst

MMS4 FPI/DES partial electron pressure tensor in DBCS during this burst

MMS4 FPI/DES partial electron pressure tensor in GSE during this burst

MMS4 FPI/DES partial electron temperature tensor in DBCS during this burst

MMS4 FPI/DES partial electron temperature tensor in GSE during this burst

MMS4 FPI/DES partial electron parallel temperature during this burst

MMS4 FPI/DES partial electron perpendicular temperature during this burst

MMS Satellite Number 4 Dual Ion Spectrometer Burst-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/brst/l2/dis-dist/2015/09/mms4_fpi_brst_l2_dis-dist_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.2302% of the 3295 timesteps. 

[CDAWeb List/Download/Create ONLY] MMS4 FPI/DIS burst sky-map instrument distribution

MMS4 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd)

MMS4 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even)

MMS4 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd)

[List/Create only in CDAWeb] 1-sigma error: MMS4 FPI/DIS burst sky-map instrument distribution

MMS4 FPI/DIS vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time

MMS Satellite Number 4 Dual Ion Spectrometer Burst-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/brst/l2/dis-moms/2015/09/mms4_fpi_brst_l2_dis-moms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.2302% of the 3295 timesteps. 

MMS4 FPI/DIS 32-bit vector of data-quality indicators at burst-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS4 FPI/DIS ion energy spectrum "near" +X_DSC during this burst

---> MMS4 FPI/DIS ion energy spectrum "near" -X_DSC during this burst

---> MMS4 FPI/DIS ion energy spectrum "near" +Y_DSC during this burst

---> MMS4 FPI/DIS ion energy spectrum "near" -Y_DSC during this burst

---> MMS4 FPI/DIS ion energy spectrum "near" +Z_DSC during this burst

---> MMS4 FPI/DIS ion energy spectrum "near" -Z_DSC during this burst

MMS4 FPI/DIS omni-directional ion energy spectrum during this burst

MMS4 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV

MMS4 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this burst

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this burst

MMS4 FPI/DIS ion bulk-velocity spintone vector in DBCS during this burst

MMS4 FPI/DIS ion bulk-velocity spintone vector in GSE during this burst

MMS4 FPI/DIS ion temperature tensor DBCS matrix during this burst

MMS4 FPI/DIS ion temperature tensor GSE matrix during this burst

MMS Satellite Number 4 Dual Ion Spectrometer Burst-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/brst/l2/dis-partmoms/2015/09/mms4_fpi_brst_l2_dis-partmoms_20150901121114_v3.3.0.cdf. The most common cadence, 150000000 [ns] = PT0.15S, occurred for 85.2302% of the 3295 timesteps. 

MMS4 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst

MMS4 FPI/DIS partial ion bulk-velocity vector in GSE during this burst

MMS4 FPI/DIS partial ion pressure tensor in DBCS during this burst

MMS4 FPI/DIS partial ion pressure tensor in GSE during this burst

MMS4 FPI/DIS partial ion temperature tensor in DBCS during this burst

MMS4 FPI/DIS partial ion temperature tensor in GSE during this burst

MMS4 FPI/DIS partial ion perpendicular temperature during this burst

MMS Satellite Number 4 Dual Electron Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/des-dist/2015/09/mms4_fpi_fast_l2_des-dist_20150901080000_v3.4.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps. 

MMS4 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS4 FPI/DES fast sky-map instrument distribution 1-sigma error

MMS4 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS4 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS4 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 4 Dual Electron Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/des-moms/2015/09/mms4_fpi_fast_l2_des-moms_20150901080000_v3.4.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps. 

MMS4 FPI/DES 32-bit vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS4 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

---> MMS4 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS4 FPI/DES electron pitch-angle distribution for "low" energies during this survey

---> MMS4 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

---> MMS4 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS4 FPI/DES electron energy spectrum "near" +X_DSC during this survey

---> MMS4 FPI/DES electron energy spectrum "near" -X_DSC during this survey

---> MMS4 FPI/DES electron energy spectrum "near" +Y_DSC during this survey

---> MMS4 FPI/DES electron energy spectrum "near" -Y_DSC during this survey

---> MMS4 FPI/DES electron energy spectrum "near" +Z_DSC during this survey

---> MMS4 FPI/DES electron energy spectrum "near" -Z_DSC during this survey

MMS4 FPI/DES electron energy parallel spectrum 30 degrees parallel to B during this survey

---> MMS4 FPI/DES electron energy anti-parallel spectrum 30 degrees anti-parallel to B during this survey

---> MMS4 FPI/DES electron energy perpendicular spectrum 60 degrees perpendicular to B during this survey

MMS4 FPI/DES omni-directional electron energy spectrum during this survey

---> MMS4 FPI/DES electron number density error during this survey

MMS4 FPI/DES electron bulk-velocity DBCS vector during this survey

MMS4 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey

MMS4 FPI/DES electron bulk-velocity GSE vector during this survey

MMS4 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey

MMS4 FPI/DES electron bulk-velocity spintone vector in DBCS during this survey

MMS4 FPI/DES electron bulk-velocity spintone vector in GSE during this survey

MMS4 FPI/DES electron pressure tensor DBCS matrix during this survey

MMS4 FPI/DES electron pressure tensor GSE matrix during this survey

MMS4 FPI/DES electron temperature tensor DBCS matrix during this survey

MMS4 FPI/DES electron temperature tensor GSE matrix during this survey

MMS Satellite Number 4 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/des-momsaux/2015/09/mms4_fpi_fast_l2_des-momsaux_20150901080000_v3.4.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps.

MMS4 FPI/DES vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

MMS4 FPI/DES partial electron bulk-velocity vector in DBCS during this survey

MMS4 FPI/DES partial electron bulk-velocity vector in GSE during this survey

MMS4 FPI/DES partial electron pressure tensor in DBCS during this survey

MMS4 FPI/DES partial electron pressure tensor in GSE during this survey

MMS4 FPI/DES partial electron temperature tensor in DBCS during this survey

MMS4 FPI/DES partial electron temperature tensor in GSE during this survey

MMS4 FPI/DES partial electron parallel temperature during this survey

MMS4 FPI/DES partial electron perpendicular temperature during this survey

MMS4 FPI/DES recommended energy index for partial moments during this survey

MMS4 FPI/DES Del-Phi (obs spin-phase) count at survey-start time

MMS4 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time

MMS4 FPI/DES electron pitch-angle distribution for "mid" energies during this survey

MMS4 FPI/DES electron pitch-angle distribution for "high" energies during this survey

MMS4 FPI/DES electron energy spectrum "near" +X_DBCS during this survey

MMS4 FPI/DES electron energy spectrum "near" -X_DBCS during this survey

MMS4 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey

MMS4 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey

MMS4 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey

MMS4 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey

MMS4 FPI/DES electron energy parallel to the magnetic field direction during this survey

MMS4 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey

MMS4 FPI/DES electron energy perpendicular to the magnetic field direction during this survey

MMS4 FPI/DES electron bulk-velocity vector in DBCS during this survey

MMS4 FPI/DES electron bulk-velocity vector in GSE during this survey

MMS4 FPI/DES electron pressure tensor in DBCS during this survey

MMS4 FPI/DES electron temperature tensor in DBCS during this survey

MMS4 FPI/DES electron temperature tensor in GSE during this survey

MMS4 FPI/DES electron heat-flux vector in DBCS during this survey

MMS4 FPI/DES electron heat-flux vector in GSE during this survey

MMS4 FPI/DES Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 4 Dual Electron Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/des-partmoms/2015/09/mms4_fpi_fast_l2_des-partmoms_20150901080000_v3.3.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps. 

MMS Satellite Number 4 Dual Ion Spectrometer Fast Survey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/dis-dist/2015/09/mms4_fpi_fast_l2_dis-dist_20150901080000_v3.4.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps. 

MMS4 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps

[Only List/Create in CDAWeb] MMS4 FPI/DIS fast sky-map instrument distribution 1-sigma error

MMS4 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time

MMS Satellite Number 4 Dual Ion Spectrometer Survey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/dis-moms/2015/09/mms4_fpi_fast_l2_dis-moms_20150901080000_v3.4.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps. 

MMS4 FPI/DIS vector of data-quality indicators at survey-start time. Note: CDF_UINT4 data was converted to HAPI double.

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS4 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey

---> MMS4 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

---> MMS4 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

---> MMS4 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

---> MMS4 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

---> MMS4 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS4 FPI/DIS omni-directional ion energy spectrum during this survey

MMS4 FPI/DIS ion bulk-velocity vector in DBCS during this survey

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey

MMS Satellite Number 4 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/dis-momsaux/2015/09/mms4_fpi_fast_l2_dis-momsaux_20150901080000_v3.4.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps.

MMS4 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey

MMS4 FPI/DIS partial ion bulk-velocity vector in GSE during this survey

MMS4 FPI/DIS partial ion pressure tensor in DBCS during this survey

MMS4 FPI/DIS partial ion pressure tensor in GSE during this survey

MMS4 FPI/DIS partial ion temperature tensor in DBCS during this survey

MMS4 FPI/DIS partial ion temperature tensor in GSE during this survey

MMS4 FPI/DIS partial ion parallel temperature during this survey

MMS4 FPI/DIS partial ion perpendicular temperature during this survey

MMS4 FPI/DIS recommended energy index for partial moments during this survey

MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time

MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time

MMS4 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey

MMS4 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey

MMS4 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey

MMS4 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey

MMS4 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey

MMS4 FPI/DIS Mag data X,Y,Z,Norm DSC  components [nT] at survey-start time

MMS Satellite Number 4 Dual Ion Spectrometer FastSurvey-resolution partial moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/fast/l2/dis-partmoms/2015/09/mms4_fpi_fast_l2_dis-partmoms_20150901080000_v3.3.0.cdf. The most common cadence, 4500002000 [ns] = PT4.500002S, occurred for 39.2045% of the 69 timesteps. 

MMS Satellite Number 4 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/slow/l2/des-dist/2015/09/mms4_fpi_slow_l2_des-dist_20150902002846_v3.4.0.cdf. The most common cadence, 58084161000 [ns] = PT58.084161S, occurred for 1.8349% of the 2 timesteps.

MMS4 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 4 Dual Electron Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/slow/l2/des-moms/2015/09/mms4_fpi_slow_l2_des-moms_20150902002846_v3.4.0.cdf. The most common cadence, 58084161000 [ns] = PT58.084161S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 4 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/slow/l2/des-momsaux/2015/09/mms4_fpi_slow_l2_des-momsaux_20150902002846_v3.4.0.cdf. The most common cadence, 58084161000 [ns] = PT58.084161S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 4 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/slow/l2/dis-dist/2015/09/mms4_fpi_slow_l2_dis-dist_20150902002846_v3.4.0.cdf. The most common cadence, 58084161000 [ns] = PT58.084161S, occurred for 1.8349% of the 2 timesteps.

MMS4 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error

MMS Satellite Number 4 Dual Ion Spectrometer SlowSurvey-resolution distribution moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/slow/l2/dis-moms/2015/09/mms4_fpi_slow_l2_dis-moms_20150902002846_v3.4.0.cdf. The most common cadence, 58084161000 [ns] = PT58.084161S, occurred for 1.8349% of the 2 timesteps.

MMS Satellite Number 4 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/fpi/slow/l2/dis-momsaux/2015/09/mms4_fpi_slow_l2_dis-momsaux_20150902002846_v3.4.0.cdf. The most common cadence, 58084161000 [ns] = PT58.084161S, occurred for 1.8349% of the 2 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/hpca/brst/l2/ion/2015/09/mms4_hpca_brst_l2_ion_20150901121114_v4.1.0.cdf. The most common cadence, 624988000 [ns] = PT0.624988S, occurred for 37.4326% of the 347 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/hpca/brst/l2/moments/2015/09/mms4_hpca_brst_l2_moments_20150901121114_v4.1.0.cdf. The most common cadence, 9999765000 [ns] = PT9.999765S, occurred for 42.8571% of the 24 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/hpca/srvy/l2/ion/2015/09/mms4_hpca_srvy_l2_ion_20150901000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 50.0000% of the 1759 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/hpca/srvy/l2/moments/2015/09/mms4_hpca_srvy_l2_moments_20150901000000_v4.1.0.cdf. The most common cadence, 9999758000 [ns] = PT9.999758S, occurred for 22.0183% of the 48 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/hpca/srvy/l2/tof-counts/2018/11/mms4_hpca_srvy_l2_tof-counts_20181115000000_v4.1.0.cdf. The most common cadence, 625000000 [ns] = PT0.625S, occurred for 92.5122% of the 74130 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/mec/brst/l2/epht89d/2015/12/mms4_mec_brst_l2_epht89d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Geocentric Equatorial Inertial (GEI/J2000) position vector of mms4 (km)

Velocity of mms4 spacecraft in GEI/J2000 (i.e. ECI) coordinates (km/s)

Geocentric Solar Magnetospheric (GSM) position vector of mms4 (km)

Geocentric Solar Ecliptic (J2000 Pole, GSE2000) position vector of mms4 (km)

Geodetic height of mms4 spacecraft. (Height above WGS84 Spheroid.)

Geodetic latitude and longitude of southern footpoint (100km geodetic height) of field threading the mms4 spacecraft

Geodetic latitude and longitude of northern footpoint (100km geodetic height) of field threading the mms4 spacecraft

GSM position southern footpoint (100km geodetic height) of field threading the mms4 spacecraft

Magnetic field (in GSM) at southern footpoint (100km geodetic height) of field threading the mms4 spacecraft

GSM position northern footpoint (100km geodetic height) of field threading the mms4 spacecraft

Magnetic field (in GSM) at northern footpoint (100km geodetic height) of field threading the mms4 spacecraft

GSM position of min-B point of field threading the mms4 spacecraft

Magnetic field (in GSM) at min-B point of field threading the mms4 spacecraft

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/mec/brst/l2/epht89q/2015/12/mms4_mec_brst_l2_epht89q_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/mec/brst/l2/ephts04d/2015/12/mms4_mec_brst_l2_ephts04d_20151206002305_v2.2.0.cdf. The most common cadence, 30000000 [ns] = PT0.03S, occurred for all 4999 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/mec/srvy/l2/epht89d/2015/09/mms4_mec_srvy_l2_epht89d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/mec/srvy/l2/epht89q/2015/09/mms4_mec_srvy_l2_epht89q_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/mec/srvy/l2/ephts04d/2015/09/mms4_mec_srvy_l2_ephts04d_20150901_v2.0.0.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for all 2879 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/scm/brst/l2/scb/2015/09/mms4_scm_brst_l2_scb_20150901121114_v2.2.1.cdf. The most common cadence, 122072 [ns] = PT0.000122072S, occurred for 79.0411% of the 3755526 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/scm/brst/l2/schb/2015/09/mms4_scm_brst_l2_schb_20150901121114_v2.2.0.cdf. The most common cadence, 61036 [ns] = PT0.000061036S, occurred for 89.4984% of the 1701006 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/mms/mms4/scm/srvy/l2/scsrvy/2015/09/mms4_scm_srvy_l2_scsrvy_20150902_v2.2.1.cdf. The most common cadence, 31250378 [ns] = PT0.03125S, occurred for 64.2788% of the 1773830 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/msl/helio1day/msl_helio1day_position_20111127_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 253 timesteps. 

Mars Science Laboratory (from all.xml/observatory/description/@short)

Mars Science Laboratory (from Master/CDFglobalAttributes/Source_name)

The Radiation Assessment Detector (RAD) and its data products are described in detail in the literature (Hassler et al., 2012). Each RAD observation contains the following: (1) Instrument counters, (2) Neutral particle count histograms in detectors D and E, (3) LET count histograms, (4) Absorbed dose rate in detectors B and E, (5) High-cadence dose rate in B and E (16 rates per observation).

Please acknowledge the RAD Principal Investigator Dr. Hassler of Southwest Research Institute Boulder.

The RAD data are archived as fully citable data. Please consult the RAD team for further details on processing and usage of these data.

SPDF/CDAWeb. Please also acknowledge the data producer: D. Hassler at SwRI-Boulder

SPDF/SSCWeb. Please also acknowledge the data producer: D. Hassler at SwRI-Boulder

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Hassler at SwRI-Boulder

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/msl/rad/cdf/obs-l1/2015/msl_rad_obs-l1_2015002_v00.cdf. The most common cadence, 1021000000000 [ns] = PT17M1S, occurred for 48.8095% of the 41 timesteps. 

Radiation Assessment Detector (from all.xml/instrument/description/@short)

RAD Flight Software checksum. Note: CDF_UINT4 data was converted to HAPI double.

EVIL Table checksum. Note: CDF_UINT4 data was converted to HAPI double.

Setup Table checksum. Note: CDF_UINT4 data was converted to HAPI double.

Temperature adjustment table checksum. Note: CDF_UINT4 data was converted to HAPI double.

Observation id in database as primary key. Note: CDF_UINT4 data was converted to HAPI double.

Spacecraft Clock at beginning of observation. Note: CDF_UINT4 data was converted to HAPI double.

Spacecraft Clock at end of observation. Note: CDF_UINT4 data was converted to HAPI double.

How many fast triggers hardware detected. Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 0 (F2H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 0 (F2H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 1 (EL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 1 (EL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 2 (EN). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 2 (EN). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 3 (EM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 3 (EM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 4 (EI). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 4 (EI). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 5 (EH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 5 (EH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 6 (EU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 6 (EU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 7 (DL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 7 (DL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 8 (DN). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 8 (DN). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 9 (DM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 9 (DM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 10 (DI). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 10 (DI). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 11 (DH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 11 (DH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 12 (DU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 12 (DU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 13 (CL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 13 (CL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 14 (CM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 14 (CM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 15 (CH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 15 (CH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 16 (CU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 16 (CU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 17 (C2L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 17 (C2L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 18 (C2H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 18 (C2H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 19 (BL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 19 (BL). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 20 (BM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 20 (BM). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 21 (BH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 21 (BH). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 22 (BU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 22 (BU). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 23 (A2L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 23 (A2L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 24 (A2M). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 24 (A2M). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 25 (A2H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 25 (A2H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 26 (A2U). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 26 (A2U). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 27 (A1L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 27 (A1L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 28 (A1M). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 28 (A1M). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 29 (A1H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 29 (A1H). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 30 (A1U). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 30 (A1U). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Fast channel 31 (F1L). Note: CDF_UINT4 data was converted to HAPI double.

Triggers for Slow channel 31 (F1L). Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 0 [A1U and BU and not C2L]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 1 [A2U and BU and not C2L]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 2 [A1M and BM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 3 [A2M and BM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 4 [BU]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 5 [EH and EI]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 6 [not F1L and not BU and not C2H and not C2L and not CU and EH and EI and EM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 7 [not F1L and not BU and not C2H and not C2L and not CU and DH and DI]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 8 [not F1L and not BU and not C2H and not C2L and not CU and DH and DI and EH and EI]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 9 [DM and DL]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 10 [not F1L and not A1U and not A2U and BU and not BH and not C2H and not C2L and not CU and not DH and not EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 11 [A2U and BU and CU and DH and EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 12 [not A1U and not A2U and not BU and not CU and DH and EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 13 [A2U and BU and CU and DH and not EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 14 [not A1M and not A2M and BM and not CM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that matched  for index 15 NA. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 0 [A1U and BU and not C2L]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 1 [A2U and BU and not C2L]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 2 [A1M and BM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 3 [A2M and BM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 4 [BU]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 5 [EH and EI]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 6 [not F1L and not BU and not C2H and not C2L and not CU and EH and EI and EM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 7 [not F1L and not BU and not C2H and not C2L and not CU and DH and DI]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 8 [not F1L and not BU and not C2H and not C2L and not CU and DH and DI and EH and EI]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 9 [DM and DL]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 10 [not F1L and not A1U and not A2U and BU and not BH and not C2H and not C2L and not CU and not DH and not EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 11 [A2U and BU and CU and DH and EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 12 [not A1U and not A2U and not BU and not CU and DH and EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 13 [A2U and BU and CU and DH and not EH]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 14 [not A1M and not A2M and BM and not CM]. Note: CDF_UINT4 data was converted to HAPI double.

Particle events that were analyzed by hardware  for index 15 NA. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/msl/rad/cdf/obs-l2/2015/msl_rad_obs-l2_2015001_v00.cdf. The most common cadence, 1021000000000 [ns] = PT17M1S, occurred for 43.0233% of the 37 timesteps. 

[Quality filtered] Radiation dose rate on Mars (recorded in Si, corrected for MMRTG contribution, and tissue-equivalent plastic)

Total Dose for B and E in 1/16th time increments of an observation

[Quality filtered] Total Dose for an observation at 1/16th timeslice of an observation

[Quality filtered] LET spectrum on Mars in Si (geometric factor ~ 0.9 cm^2 sr)

[Quality filtered] Neutral particle (neutrons + gamma rays) counts on Mars

[Quality filtered] Neutral particle counts in tissue-equivalent plastic

[All quality] Radiation dose rate on Mars (recorded in Si, corrected for MMRTG contribution, and tissue-equivalent plastic)

[All quality] Total Dose for an observation at 1/16th timeslice of an observation

[All quality] LET spectrum on Mars in Si (geometric factor ~ 0.9 cm^2 sr)

[All quality] Neutral particle (neutrons + gamma rays) counts on Mars

[All quality] Neutral particle counts in tissue-equivalent plastic

[NO PLOT] Quality indicator - flagged data has quality issues from various sources, Commanding, DAN activity, Other; no value=good

Electron Fluxes 6eV to 20 keV, from the MEDUSA instrument on the Munin nanosat

Munin MEDUSA and PIA Instrument Description, Annales Geophysicae Publication

The MEDUSA Electron and Ion Spectrometer and the PIA Ultraviolet Photometers on Astrid-2, O. Norberg, J. D. Winningham, H. Lauche, W. Keith, W. Puccio, J. Olsen, K. Lundin, and J. Scherrer

eoPortal Munin Web Page, Spacecraft, Instrument, and Downlink Information

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/munin/cdfs/m1/mdse/2000/munin_m1_mdse_20001209114612_v01.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 98.7751% of the 887 timesteps. 

Ion Fluxes 1eV to 12 keV, from the MEDUSA instrument on the MUNIN nanosat

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/munin/cdfs/m1/mdsi/2000/munin_m1_mdsi_20001209114612_v01.cdf. The most common cadence, 500000000 [ns] = PT0.5S, occurred for 97.5446% of the 437 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Rymd Plasma Gruppen at Swedish Institute of Space Physics

SPDF/SSCWeb. Please also acknowledge the data producer: Rymd Plasma Gruppen at Swedish Institute of Space Physics

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Rymd Plasma Gruppen at Swedish Institute of Space Physics

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/munin/cdfs/m1/oa/2000/munin_m1_oa_20001208095108_v01.cdf. The most common cadence, 250000000 [ns] = PT0.25S, occurred for 99.1608% of the 1418 timesteps. 

Orbit and attitude data (from all.xml/instrument/description/@short)

The Mars Atmosphere and Volatile Evolution, MAVEN, Mission Home Page, LASP, UC Boulder

General Information about the Mars Atmosphere and Volatile Evolution, MAVEN, Mission, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, UCB

Document of MAVEN In Situ Key Parameters (Table 13 for the List of Variables)

The Mars Atmosphere and Volatile Evolution, MAVEN, Langmuir Probe and Waves Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Langmuir Probe and Waves Instrument Home Page, Laboratory for Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN Langmuir Probe and Waves, LPW, Instrument Space Science Reviews Publication

Andersson, L., Ergun, R.E., Delory, G.T., Eriksson, A., Westfall, J., Reed, H., McCauly, J., Summers, D., and D. Meyers, The Langmuir Probe and Waves (LPW) Instrument for MAVEN, Space Sci. Rev., 195, 173-198, 2015

NSSDC Master Catalog Listing, MAVEN Langmuir Probe and Waves, LPW, Instrument

NSSDC Master Catalog Listing for the MAVEN Langmuir Probe and Waves, LPW, Instrument, NSSDCA/COSPAR ID: 2013-063A-04

The Mars Atmosphere and Volatile Evolution, MAVEN, Langmuir Probe and Waves, LPW, Extreme Ultraviolet Monitor Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Langmuir Probe and Waves, LPW, Extreme Ultraviolet Monitor Instrument Home Page, Laboratory for Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN Langmuir Probe and Waves, LPW, Extreme Ultraviolet Monitor, EUV, Instrument Space Science Reviews Publication

Eparvier, F.G., Chamberlin, P.C., Woods, T.N., and E.M.B. Thiemann, The Solar Extreme Ultraviolet Monitor for MAVEN, Space Sci. Rev., 195, 293-301, 2015

The Mars Atmosphere and Volatile Evolution, MAVEN, Magnetometer Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Magnetometer Instrument Home Page, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder

MAVEN Magnetometer, MAG, Instrument Space Science Reviews Publication

Connerney, J.E.P., J. Espley, P. Lawton, S. Murphy, J. Odom, R. Oliversen, and D. Sheppard, The MAVEN Magnetic Field Investigation, Space Sci. Rev., 195, 257-291, 2015

NSSDC Master Catalog Listing, MAVEN Magnetometer, MAG, Instrument

NSSDC Master Catalog Listing for the MAVEN Magnetometer, MAG, Instrument, NSSDCA/COSPAR ID: 2013-063A-08

The Mars Atmosphere and Volatile Evolution, MAVEN, Neutral Gas and Ion Mass Spectrometer Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Neutral Gas and Ion Mass Spectrometer Instrument Home Page, Laboratory for Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN Neutral Gas and Ion Mass Spectrometer, NGIMS, Instrument Space Science Reviews Publication

Mahaffy, P.R., Benna, M., King, T., Harpold, D.N., Arvey, R., Barciniak, M., Bendt, M., Carrigan, D., Errigo, T., Holmes, V., Johnson, C.S., Kellogg, J., Kimvilakani, P., Lefavor, M., Hengemihle, J., Jaeger, F., Lyness, E., Maurer, J., Melak, A., Noreiga, F., Noriega, M., Patel, K., Prats, B., Raaen, E., Tan, F., Weidner, E., Gundersen, C., Battel, S., Block, B.P., Arnett, K., Miller, R., Cooper, C., Edmonson, C., and J.T. Nolan,, The Neutral Gas and Ion Mass Spectrometer on the Mars Atmosphere and Volatile Evolution Mission, Space Sci. Rev., 195, 49-73, 2015

NSSDC Master Catalog Listing, MAVEN Neutral Gas and Ion Mass Spectrometer, NGIMS, Instrument

NSSDC Master Catalog Listing for the MAVEN Neutral Gas and Ion Mass Spectrometer, NGIMS, Instrument, NSSDCA/COSPAR ID: 2013-063A-02

The Mars Atmosphere and Volatile Evolution, MAVEN, Solar Energetic Particle Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Solar Energetic Particle Instrument Home Page, Laboratory of Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN Solar Energetic Particle, SEP, Instrument Space Science Reviews Publication

Larson, D.E., Lillis, R.J., Lee, C.O., Dunn, P.A., Hatch, K., Robinson, M., Glaser, D., Chen, J., Curtis, D., Tiu, C., Lin, R.P., Luhmann, J.G., and B.M. Jakosky, The MAVEN Solar Energetic Particle Investigation, Space Sci. Rev., 195, 153-172, 2015

NSSDC Master Catalog Listing, MAVEN Solar Energetic Particle, SEP, Instrument

NSSDC Master Catalog Listing for the MAVEN Solar Energetic Particle, SEP, Instrument, NSSDCA/COSPAR ID: 2013-063A-05

The Mars Atmosphere and Volatile Evolution, MAVEN, SupraThermal And Thermal Ion Composition Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, SupraThermal And Thermal Ion Composition Instrument Home Page, Laboratory of Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN SupraThermal And Thermal Ion Composition, STATIC, Instrument Space Science Reviews Publication

McFadden, J.P., Kortmann, O., Curtis, D., Dalton, G., Johnson, G., Abiad, R., Sterling, R., Hatch, K., Berg, P., Tiu, C., Gordon, D., Heavner, S., Robinson, M., Marckwordt, M., Lin, R., and B.M. Jakosky, MAVEN SupraThermal and Thermal Ion Compostion (STATIC) Instrument, Space Sci. Rev., 195, 199-256, 2015

NSSDC Master Catalog Listing, MAVEN SupraThermal And Thermal Ion Composition, STATIC, Instrument

NSSDC Master Catalog Listing for the MAVEN SupraThermal And Thermal Ion Composition, STATIC, Instrument, NSSDCA/COSPAR ID: 2013-063A-03

The Mars Atmosphere and Volatile Evolution, MAVEN, Solar Wind Electron Analyzer Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Solar Wind Electron Analyzer Instrument Home Page, Laboratory of Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN Solar Wind Electron Analyzer, SWEA, Instrument Space Science Reviews Publication

Mitchell, D.L., Mazelle, C., Sauvaud, J.-A., Thocaven, J.-J., Rouzaud, J., Fedorov, A., Rouger, P., Toublanc, D., Taylor, E., Gordon, D., Robinson, M., Heavner, S., Turin, P., Diaz-Aguado, M., Curtis, D.W., Lin, R.P., and B.M. Jakosky, The MAVEN Solar Wind Electron Analyzer, Space Sci. Rev., 200, 495-528, 2016

NSSDC Master Catalog Listing, MAVEN Solar Wind Electron Analyzer, SWEA, Instrument

NSSDC Master Catalog Listing for the MAVEN Solar Wind Electron Analyzer, SWEA, Instrument, NSSDCA/COSPAR ID: 2013-063A-07

The Mars Atmosphere and Volatile Evolution, MAVEN, Solar Wind Ion Analyzer Instrument Home Page, LASP, UC Boulder

The Mars Atmosphere and Volatile Evolution, MAVEN, Solar Wind Ion Analyzer Instrument Home Page, Laboratory for Atmospheric and Space Physics, LASP, University of Colorado, Boulder

MAVEN Solar Wind Ion Analyzer, SWIA, Instrument Space Science Reviews Publication

Halekas, J.S., Taylor, E.R., Dalton, G., Johnson, G., Curtis, D.W., McFadden, J.P., Mitchell, D.L., Lin, R.P., and B.M. Jakosky, The Solar Wind Ion Analyzer for MAVEN, Space Sci. Rev., 195, 125-151, 2015

NSSDC Master Catalog Listing, MAVEN Solar Wind Ion Analyzer, SWIA, Instrument

NSSDC Master Catalog Listing for the MAVEN Solar Wind Ion Analyzer, SWIA, Instrument, NSSDCA/COSPAR ID: 2013-063A-06

SPDF/CDAWeb. Please also acknowledge the data producer: B.M. Jakosky at LASP/U. Colorado

SPDF/SSCWeb. Please also acknowledge the data producer: B.M. Jakosky at LASP/U. Colorado

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: B.M. Jakosky at LASP/U. Colorado

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/insitu/kp-4sec/cdfs/2014/03/mvn_insitu_kp-4sec_20140318_v13_r03.cdf. The most common cadence, 8000 [ms] = PT8S, occurred for all 10799 timesteps. 

Mars Atmosphere and Volatile Evolution Mission (from all.xml/observatory/description/@short)

Mars Atmosphere and Volatile Evolution Mission (from Master/CDFglobalAttributes/Source_name)

in situ data, key parameter 4-sec (from Master/CDFglobalAttributes/Data_type)

Spacecraft event time for this data record (UTC Epoch time from 01-Jan-0000 00:00:00.000 without leap seconds), one element per ion distribution (NUM_DISTS elements)

---> EUV irradiance wave power 0.1-7.0 nm data quality (LPW-EUV)

---> EUV irradiance wave power Lyman-alpha data quality (LPW-EUV)

---> Electron energy flux parallel 100-500 eV data quality (SWEA)

---> Electron energy flux parallel 500-1000 eV data quality (SWEA)

---> Electron energy flux anti-parallel 5-100 eV data quality (SWEA)

---> Electron energy flux anti-parallel 100-500 eV data quality (SWEA)

---> Electron energy flux anti-parallel 500-1000 eV data quality (SWEA)

Total ion density from onboard moment calculation, assuming 100% protons (SWIA)

Bulk ion flow velocity XYZ component from onboard moment calculation, assuming 100% protons (SWIA)

Scalar ion temperature from onboard moment calculation, assuming 100% protons (SWIA)

Ion dynamic pressure computed on ground from density and velocity moments, assuming 100% protons (SWIA)

O2+ MAVEN_APP XYZ component of velocity below TBD altitude determined from APID c6 while in Ram or Conic mode (STATIC)

---> O2+ MAVEN_APP XYZ component of velocity data quality (STATIC)

O2+ MSO XYZ component of velocity below TBD altitude while in Ram or Conic mode (STATIC)

H+ MSO X-direction of flux above TBD altitude determined from TBD APID while in Pickup and Scan mode (STATIC)

Dominant pickup ion MSO XYZ direction of flux above TBD altitude determined from APID D0 and CE while in Pickup, Eclipse and Protect mode

---> Dominant pickup ion characteristic angular width DQ (STATIC)

---> Electron energy flux (30-300 keV), FOV 1-F data quality (SEP)

---> Electron energy flux (30-300 keV), FOV 1-R data quality (SEP)

---> Electron energy flux (30-300 keV), FOV 2-F data quality (SEP)

---> Electron energy flux (30-300 keV), FOV 2-R data quality (SEP)

Magnetic field vector component in the XYZ direction in MSO coordinates (MAG)

---> Magnetic field vector component in MSO coordinates data quality (MAG)

Magnetic field vector component in the XYZ direction in GEO coordinates (MAG)

---> Magnetic field vector component in GEO coordinates data quality (MAG)

---> Deviations from the mean magnetic field magnitude data quality (MAG)

XYZ-component of spacecraft position in Mars planetocentric (geographic) GEO coordinates

XYZ-component of articulated payload platform (app) attitude in GEO coordinates

XYZ-component of articulated payload platform (app) attitude in MSO coordinates

SPDF/CDAWeb. Please also acknowledge the data producer: J. Connerney at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J. Connerney at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Connerney at NASA GSFC

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/mag/l2/sunstate-1sec/cdfs/2014/10/mvn_mag_l2-sunstate-1sec_20141010_v01_r01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 91.6866% of the 79142 timesteps. 

Level 2 data, sunstate 1sec (from Master/CDFglobalAttributes/Data_type)

UTC time from 01-Jan-2000 12:00:00.000 including leap seconds), one element per ion distribution (NUM_DISTS elements)

DERIVED FROM: MAVEN SEP (Solar Energetic Particle) Instrument Sensor 1 Fully Calibrated Spectra Survey

SPDF/CDAWeb. Please also acknowledge the data producer: D. Larson (davin@ssl.berkeley.edu) at U.C. Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: D. Larson (davin@ssl.berkeley.edu) at U.C. Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Larson (davin@ssl.berkeley.edu) at U.C. Berkeley Space Sciences Laboratory

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/sep/l2/s1-cal-svy-full/2014/09/mvn_sep_l2_s1-cal-svy-full_20140922_v04_r06.cdf. The most common cadence, 8000000000 [ns] = PT8S, occurred for 47.6277% of the 783 timesteps. 

Solar Energetic Particle Experiment (from all.xml/instrument/description/@short)

Survey Calibrated Particle Flux (from Master/CDFglobalAttributes/Data_type)

Differential ion flux in forward look direction (#/cm^2/sec/ster/keV)

Total (integrated) ion flux in forward look direction (#/cm^2/sec/ster)

Differential electron flux in forward look direction (#/cm^2/sec/ster/keV)

Total (integrated) electron flux in forward look direction (#/cm^2/sec/ster)

Differential ion flux in reverse look direction (#/cm^2/sec/ster/keV)

Total (integrated) ion flux in reverse look direction (#/cm^2/sec/ster)

Differential electron flux in reverse look direction (#/cm^2/sec/ster/keV)

Total (integrated) electron flux in reverse look direction (#/cm^2/sec/ster)

DERIVED FROM: MAVEN SEP (Solar Energetic Particle) Instrument Sensor 2 Fully Calibrated Spectra Survey

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/sep/l2/s2-cal-svy-full/2014/09/mvn_sep_l2_s2-cal-svy-full_20140922_v04_r06.cdf. The most common cadence, 8000000000 [ns] = PT8S, occurred for 47.6277% of the 783 timesteps. 

MAVEN STATIC (Supra-Thermal And Thermal Ion Composition) Particle Distributions 12 Event Rates Summed Over Energy

STATIC>Supra-Thermal And Thermal Ion Composition Particle Distributions

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/static/l2/d8-12r1e/2014/10/mvn_sta_l2_d8-12r1e_20141013_v02_r00.cdf. The most common cadence, 4000002368 [ns] = PT4.000002S, occurred for 33.0519% of the 7086 timesteps. 

Supra-Thermal Thermal Ion Composition Particle Distributions (from all.xml/instrument/description/@short)

Level 2 data, APID: d8, 12 Rates, 1 Energy (from Master/CDFglobalAttributes/Data_type)

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diag mode (bit 2), data comp type (bit 3-4), packet compn (bit 5)

---> Index that identifies the energy and deflector sweep look up tables (LUT) for the sensor

MAVEN STATIC (Supra-Thermal And Thermal Ion Composition) Particle Distributions 12 Event Rates 64 Energy

STATIC> Supra-Thermal And Thermal Ion Composition Particle Distributions

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/static/l2/d9-12r64e/2014/10/mvn_sta_l2_d9-12r64e_20141013_v02_r00.cdf. The most common cadence, 127999102848 [ns] = PT2M7.999103S, occurred for 26.4179% of the 177 timesteps. 

MAVEN STATIC (Supra-Thermal And Thermal Ion Composition) Particle Distributions 1 Selected Event Rate 64 Energy

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/static/l2/ca-16e4d16a/da-1r64e/2014/10/mvn_sta_l2_da-1r64e_20141013_v02_r00.cdf. The most common cadence, 4000002368 [ns] = PT4.000002S, occurred for 33.7702% of the 7240 timesteps. 

Level 2 data, APID: da, 1 Rate, 64 Energies (from Master/CDFglobalAttributes/Data_type)

DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Archive 3D Distributions 

SPDF/CDAWeb. Please also acknowledge the data producer: David L. Mitchell (mitchell@ssl.berkeley.edu) at UC Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: David L. Mitchell (mitchell@ssl.berkeley.edu) at UC Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David L. Mitchell (mitchell@ssl.berkeley.edu) at UC Berkeley Space Sciences Laboratory

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swea/l2/arc3d/2014/03/mvn_swe_l2_arc3d_20140320_v04_r01.cdf. The most common cadence, 8000020032 [ns] = PT8.00002S, occurred for 57.5467% of the 1079 timesteps. 

Solar Wind Electron Analyzer (from all.xml/instrument/description/@short)

Planetary Plasma Interactions (from Master/CDFglobalAttributes/Discipline)

Energy binning factor: 1 = 64 energies, 2 = 32 energies, 4 = 16 energies

Calibrated Differential Energy Flux [vary with time, energy, deflection index and azimuth angle] at 1st Deflection Index[Thumbnails, select a few hours]

Variance of differential energy flux (unavailable before 2014/11/15)

Secondary electron contamination (unavailable before 2014/11/15)

DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Archive Pitch Angle Distribution

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swea/l2/arcpad/2014/10/mvn_swe_l2_arcpad_20141018_v04_r01.cdf. The most common cadence, 2000001216 [ns] = PT2.000001S, occurred for 28.6890% of the 1639 timesteps. 

Mars Atmosphere and Volatile EvolutioN Mission (from all.xml/observatory/description/@short)

Mars Atmosphere and Volatile EvolutioN Mission (from Master/CDFglobalAttributes/Source_name)

Calibrated differential energy flux (energy vs pitch angles for 158eV)

Variance of differential energy flux (unavailable before 2014/11/16)

Secondary electron contamination (unavailable before 2014/11/16)

DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Survey 3D Distributions

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swea/l2/svy3d/2014/03/mvn_swe_l2_svy3d_20140319_v04_r01.cdf. The most common cadence, 32000049600 [ns] = PT32.00005S, occurred for 15.4545% of the 170 timesteps. 

Calibrated differential energy flux [vary with time, energy, deflection index and azimuth angle] at 1st Deflection Index [Thumbnails, select a few hours]

DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Survey Pitch Angle Distribution 

SPDF/CDAWeb. Please also acknowledge the data producer: David L. Mitchell (mitchell@ssl.berkeley.edu) at UCB/SSL

SPDF/SSCWeb. Please also acknowledge the data producer: David L. Mitchell (mitchell@ssl.berkeley.edu) at UCB/SSL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David L. Mitchell (mitchell@ssl.berkeley.edu) at UCB/SSL

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swea/l2/svypad/2014/10/mvn_swe_l2_svypad_20141010_v04_r01.cdf. The most common cadence, 3999972096 [ns] = PT3.999972S, occurred for 24.0836% of the 5197 timesteps. 

DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Energy Spectra Survey

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swea/l2/svyspec/2014/03/mvn_swe_l2_svyspec_20140319_v04_r01.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 93.7564% of the 8214 timesteps. 

MAVEN SWIA (Solar Wind Ion Analyzer) Level 2 Coarse 3D Distributions Archive Telemetry 

SPDF/CDAWeb. Please also acknowledge the data producer: J.S. Halekas at U Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: J.S. Halekas at U Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.S. Halekas at U Iowa

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swia/l2/coarsearc3d/2014/03/mvn_swi_l2_coarsearc3d_20140320_v02_r00.cdf. The most common cadence, 32000064832 [ns] = PT32.000065S, occurred for 33.7607% of the 158 timesteps. 

Solar Wind Ion Analyzer (from all.xml/instrument/description/@short)

Calibrated Differential Energy Flux [vary with time, energy, deflection index and anode angle] at 1st deflection index [Thumnails, select a few hours]

MAVEN SWIA (Solar Wind Ion Analyzer) Level 2 Coarse 3D Distributions Survey Telemetry 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swia/l2/coarsesvy3d/2014/03/mvn_swi_l2_coarsesvy3d_20140319_v02_r00.cdf. The most common cadence, 64000084160 [ns] = PT1M4.000084S, occurred for 7.7348% of the 42 timesteps. 

Calibrated Differential Energy Flux [vary with time, energy, deflection index and anode angle] at 1st deflection index[Thumbnails, select a few hours]

DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer) Level 2 Fine 3D Distributions Archive Telemetry

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swia/l2/finearc3d/2014/03/mvn_swi_l2_finearc3d_20140320_v02_r00.cdf. The most common cadence, 8000020032 [ns] = PT8.00002S, occurred for 58.1557% of the 1091 timesteps. 

Calibrated Differential Energy Flux [vary with time, energy, deflection index and anode angle] at 1st Deflection Index [Thumbnails, select a few hours]

DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer) Level 2 Fine 3D Distributions Survey Telemetry

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swia/l2/finesvy3d/2014/03/mvn_swi_l2_finesvy3d_20140319_v02_r00.cdf. The most common cadence, 8000004736 [ns] = PT8.000005S, occurred for 23.2360% of the 1011 timesteps. 

Calibrated Differential Energy Flux [vary with time, energy, deflection index and anode angle] at 1st Deflection Index[Thumbnails, select a few hours]

DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer) Onboard Moment Survey Telemetry

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swia/l2/onboardsvymom/2014/03/mvn_swi_l2_onboardsvymom_20140319_v02_r00.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 93.7608% of the 8175 timesteps. 

Onboard velocity moment (MSO [Mars-Sun Orbit] Coords), assuming 100% protons

Onboard temperature moment (Inst. Coords), assuming 100% protons

Onboard temperature moment (MSO [Mars-Sun Orbit] Coords), assuming 100% protons

Decommutation Flag: 0 = uncertain mode/attenuator flags, 1 = known mode/attenuator flags

DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer) Onboard Survey Energy Spectra

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/maven/swia/l2/onboardsvyspec/2014/03/mvn_swi_l2_onboardsvyspec_20140319_v02_r00.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 93.7608% of the 8160 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/neptune_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/neptune_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

New Horizons Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) corrected cosmic ray count per second

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. R = Rates (Energy Only): 1) High Energy, 2) Initially labelled as 'Electrons' but dominated by Cosmic Rays during cruise due to high geometry factor. R0 = Energy range 5-18 keV and > 735 keV R1 = Energy range 19-193 keVR2 = Energy range 194-734 keVJ = general marker of Solar Wind Activity J00 = 'Electron' events J01 = 'Triples' where NNNN = year from 2012 to 2025S = Detector SectorMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yThis particular dataset is related to original datafiles: Cosmic Rays Count per Second: PEPSSI_Reduced_CRCPS_NNNN.csv

the PEPSSI are archived as fully citable data. Please consult PEPPSI team publications and personnel for further details on production, processing, and usage of these data

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Ralph L.McNutt, Jr at Johns Hopkins University Applied Physics Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Ralph L.McNutt, Jr at Johns Hopkins University Applied Physics Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Ralph L.McNutt, Jr at Johns Hopkins University Applied Physics Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/cosmic-ray-corrected-count-rate-crcps/new-horizons_pepssi_cosmic-ray-corrected-count-rate-crcps_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9371% of the 6355 timesteps.

Pluto Energetic Particle Spectrometer Science Investigation (from all.xml/instrument/description/@short)

Cosmic Rays Count per Second (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/cosmic-ray-corrected-count-rate-crcps-spectra/new-horizons_pepssi_cosmic-ray-corrected-count-rate-crcps-spectra_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9371% of the 6355 timesteps.

New Horizons Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) background corrected cosmic ray flux in calibration regime 'A' or 'B' 

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. R = Rates (Energy Only): 1) High Energy, 2) Initially labelled as 'Electrons' but dominated by Cosmic Rays during cruise due to high geometry factor. R0 = Energy range 5-18 keV and > 735 keV R1 = Energy range 19-193 keVR2 = Energy range 194-734 keVS = Detector SectorMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yThis particular dataset is Cosmic Rays Background Corrected Flux (differential intensity):  related to original datafiles: PEPSSI_Reduced_CRFLUX_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'A' or 'B' is a calibration regime

the PEPSSI are archived as fully citable data. Please consultPEPPSI team publications and personnel for further details on production, processing, and usage of these data 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/cosmic-ray-corrected-flux-crflux-a/new-horizons_pepssi_cosmic-ray-corrected-flux-crflux-a_20110101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9886% of the 8782 timesteps.

Corrected Background Flux (from Master/CDFglobalAttributes/Data_type)

R0 Sector 0 Background Corrected Flux, Lower Bound-Upper Bound (keV): 21.5-22.5

R0 Sector 2 Background Corrected Flux, Lower Bound-Upper Bound (keV): 22.5-23.5

R0 Sector 5 Background Corrected Flux, Lower Bound-Upper Bound (keV): 23.5-24.5

R1 Sector 0 Background Corrected Flux, Lower Bound-Upper Bound (keV): 24.5-25.5

R1 Sector 2 Background Corrected Flux, Lower Bound-Upper Bound (keV): 25.5-26.5

R1 Sector 5 Background Corrected Flux, Lower Bound-Upper Bound (keV): 26.5-27.5

R2 Sector 0 Background Corrected Flux, Lower Bound-Upper Bound (keV): 27.5-28.5

R2 Sector 2 Background Corrected Flux, Lower Bound-Upper Bound (keV): 28.5-29.5

R2 Sector 5 Background Corrected Flux, Lower Bound-Upper Bound (keV): 29.5-30.5

the PEPSSI are archived as fully citable data. Please consultPEPPSI team publications and personnel for further details on production, processing, and usage of these data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/cosmic-ray-corrected-flux-crflux-spectra-a/new-horizons_pepssi_cosmic-ray-corrected-flux-crflux-spectra-a_20120101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9886% of the 8782 timesteps.

New Horizons Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) 'Doubles' low energy events counts per second, time-of-flight (TOF) only, ~2-250 keV/nuc He+ in calibration regime 'A' or 'B' 

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. L = Low energy rates 'doubles' time-of-flight (TOF) covers the lowest energy range particles events also overlaps with the 'triple' coincidence dataS = Detector Sector numberP = Calibrated assuming the particle is a protonMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yThis particular dataset is related to 'Doubles', suprathermal (low energy) particle events counts per second, time-of-flight (TOF) only, ~2-250 keV/nuc He+ The original datafiles: PEPSSI_Reduced_LCPS_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'A' or 'B' is a calibration regime

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-count-rate-tof-lcps-a/new-horizons_pepssi_doubles-count-rate-tof-lcps-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Suprathermal Particles (Low Energy) Doubles Count per Second (from Master/CDFglobalAttributes/Data_type)

L01 S00 P H+ Count per second, Lower-Upper Bound (keV): 31.562-53.761

L01 Sector 1 P H+ Count per second, Lower-Upper Bound (keV): 31.562-53.761

L01 S02 P H+ Count per second, Lower-Upper Bound (keV): 31.562-53.761

L01 S03 P H+ Count per second, Lower-Upper Bound (keV): 31.562-53.761

L01 S04 P H+ Count per second, Lower-Upper Bound (keV): 31.562-53.761

L01 S05 P H+ Count per second, Lower-Upper Bound (keV): 31.562-53.761

L03 S00 P H+ Count per second, Lower-Upper Bound (keV): 17.71-30.831

L03 S01 P H+ Count per second, Lower-Upper Bound (keV): 17.71-30.831

L03 S02 P H+ Count per second, Lower-Upper Bound (keV): 17.71-30.831

L03 S03 P H+ Count per second, Lower-Upper Bound (keV): 17.71-30.831

L03 S04 P H+ Count per second, Lower-Upper Bound (keV): 17.71-30.831

L03 S05 P H+ Count per second, Lower-Upper Bound (keV): 17.71-30.831

L05 S00 P H+ Count per second, Lower-Upper Bound (keV): 9.3786-17.389

L05 S01 P H+ Count per second, Lower-Upper Bound (keV): 9.3786-17.389

L05 S02 P H+ Count per second, Lower-Upper Bound (keV): 9.3786-17.389

L05 S03 P H+ Count per second, Lower-Upper Bound (keV): 9.3786-17.389

L05 S04 P H+ Count per second, Lower-Upper Bound (keV): 9.3786-17.389

L05 S05 P H+ Count per second, Lower-Upper Bound (keV): 9.3786-17.389

L07 S00 P H+ Count per second, Lower-Upper Bound (keV): 4.5207-9.2422

L07 S01 P H+ Count per second, Lower-Upper Bound (keV): 4.5207-9.2422

L07 S02 P H+ Count per second, Lower-Upper Bound (keV): 4.5207-9.2422

L07 S03 P H+ Count per second, Lower-Upper Bound (keV): 4.5207-9.2422

L07 S04 P H+ Count per second, Lower-Upper Bound (keV): 4.5207-9.2422

L07 S05 P H+ Count per second, Lower-Upper Bound (keV): 4.5207-9.2422

L09 S00 P H+ Count per second, Lower-Upper Bound (keV): 1.754-4.4634

L09 S01 P H+ Count per second, Lower-Upper Bound (keV): 1.754-4.4634

L09 S02 P H+ Count per second, Lower-Upper Bound (keV): 1.754-4.4634

L09 S03 P H+ Count per second, Lower-Upper Bound (keV): 1.754-4.4634

L09 S04 P H+ Count per second, Lower-Upper Bound (keV): 1.754-4.4634

L09 S05 P H+ Count per second, Lower-Upper Bound (keV): 1.754-4.4634

L11 S00 P H+ Count per second, Lower-Upper Bound (keV): 0.17848-1.7301

L11 S01 P H+ Count per second, Lower-Upper Bound (keV): 0.17848-1.7301

L11 S02 P H+ Count per second, Lower-Upper Bound (keV): 0.17848-1.7301

L11 S03 P H+ Count per second, Lower-Upper Bound (keV): 0.17848-1.7301

L11 S04 P H+ Count per second, Lower-Upper Bound (keV): 0.17848-1.7301

L11 S05 P H+ Count per second, Lower-Upper Bound (keV): 0.17848-1.7301

L13 S00 P H+ Count per second, Lower-Upper Bound (keV): 0.0-0.16835

L13 S01 P H+ Count per second, Lower-Upper Bound (keV): 0.0-0.16835

L13 S02 P H+ Count per second, Lower-Upper Bound (keV): 0.0-0.16835

L13 S03 P H+ Count per second, Lower-Upper Bound (keV): 0.0-0.16835

L13 S04 P H+ Count per second, Lower-Upper Bound (keV): 0.0-0.16835

L13 S05 P H+ Count per second, Lower-Upper Bound (keV): 0.0-0.16835

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-count-rate-tof-lcps-b/new-horizons_pepssi_doubles-count-rate-tof-lcps-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-count-rate-tof-lcps-spectra-a/new-horizons_pepssi_doubles-count-rate-tof-lcps-spectra-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-count-rate-tof-lcps-spectra-b/new-horizons_pepssi_doubles-count-rate-tof-lcps-spectra-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

PEPSSI>Pluto Energetic Particle Spectrometer Science Investigation suprathermal (lowest energy) particle time-of-flight (TOF)  differential intensity in calibration regime 'A' or 'B' 

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. L = Low energy rates 'doubles' time-of-flight (TOF) covers the lowest energy range particles events also overlaps with the 'triple' coincidence dataS = Detector Sector numberP = Calibrated assuming the particle is a protonMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yThis particular dataset is related to 'Doubles', suprathermal (lowest energy) particle differential intensity time-of-flight (TOF), ~2-250 keV/nuc He+ The original datafiles: PEPSSI_Reduced_LFLUX_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'A' or 'B' is a calibration regime

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-diff-intensity-tof-lflux-a/new-horizons_pepssi_doubles-diff-intensity-tof-lflux-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Suprathermal (Low Energy) Particles Doubles Time-of-Flight Differential Intensity (from Master/CDFglobalAttributes/Data_type)

H+ Flux, L11 Sector 0 P, Lower-Upper Bound (keV): 0.17848-1.7301

H+ Flux, L11 Sector 1 P, Lower-Upper Bound (keV): 0.17848-1.7301

H+ Flux, L11 Sector 2 P, Lower-Upper Bound (keV): 0.17848-1.7301

H+ Flux, L11 Sector 3 P, Lower-Upper Bound (keV): 0.17848-1.7301

H+ Flux, L11 Sector 4 P, Lower-Upper Bound (keV): 0.17848-1.7301

H+ Flux, L11 Sector 5 P, Lower-Upper Bound (keV): 0.17848-1.7301

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-diff-intensity-tof-lflux-b/new-horizons_pepssi_doubles-diff-intensity-tof-lflux-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-diff-intensity-tof-lflux-spectra-a/new-horizons_pepssi_doubles-diff-intensity-tof-lflux-spectra-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/doubles-diff-intensity-tof-lflux-spectra-b/new-horizons_pepssi_doubles-diff-intensity-tof-lflux-spectra-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

New Horizons NH Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) Box-shaped slab triples count per second, time of flight (TOF) vs energy space, ~15 keV to 1 MeV, H, He, O (CNO group) in calibration regime 'A' or 'B' 

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. B = box-like slab 2D shapes, roughly polygonS = Detector SectorMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yData type: BCPS ('Box' count per second: box-like slab 2D shape, roughly polygon, triples counts per second, time of flight (TOF) vs energy space, ~15 keV to 1 MeV, H, He, O (CNO group) The original datafiles:PEPSSI_Reduced_BCPS_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'A' or 'B' is a calibration regime

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Ralph L. McNutt, Jr at Johns Hopkins University Applied Physics Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Ralph L. McNutt, Jr at Johns Hopkins University Applied Physics Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Ralph L. McNutt, Jr at Johns Hopkins University Applied Physics Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-count-rate-bcps-a/new-horizons_pepssi_triples-count-rate-bcps-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Box Count per Second (from Master/CDFglobalAttributes/Data_type)

N2_2 count rate, Box 14 Sector 0, energy range 69.066-263.62 keV

N2_2 count rate, Box 14 Sector 1, energy range 69.066-263.62 keV

N2_2 count rate, Box 14 Sector 2, energy range 97.501-263.62 keV

N2_2 count rate, Box 14 Sector 3, energy range 69.066-263.62 keV

N2_2 count rate, Box 14 Sector 4, energy range 69.066-263.62 keV

N2_2 count rate, Box 14 Sector 5, energy range 88.856-263.62 keV

N2_2 count rate, Box 15 Sector 4,  energy range 265.5-597.45 keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-count-rate-bcps-b/new-horizons_pepssi_triples-count-rate-bcps-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-count-rate-bcps-spectra-a/new-horizons_pepssi_triples-count-rate-bcps-spectra-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. B = box-like slab 2D shapes, roughly polygonS = Detector SectorMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yData type: BCPS ('Box' count per second: box-like slab 2D shape, roughly polygon, triples counts per second, time of flight (TOF) vs energy space, ~15 keV to 1 MeV, H, He, O (CNO group) The original datafiles:PEPSSI_Reduced_BCPS_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'a' or 'b' is a calibration regime

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-count-rate-bcps-spectra-b/new-horizons_pepssi_triples-count-rate-bcps-spectra-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

New Horizons Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) Box-shaped slab triples count per second, time of flight (TOF) vs energy space, ~15 keV to 1 MeV, H, He, O (CNO group) in calibration regime 'A' or 'B' 

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. B = box-like slab 2D shapes, roughly polygonS = Detector SectorMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yThe original datafiles:PEPSSI_Reduced_BFLUX_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'A' or 'B' is a calibration regime

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-diff-intensity-bflux-a/new-horizons_pepssi_triples-diff-intensity-bflux-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-diff-intensity-bflux-b/new-horizons_pepssi_triples-diff-intensity-bflux-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

The New Horizons mission's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is made up of a time-of-flight (TOF)/mass spectrometer and the associated science investigation. The PEPSSI instrument is designed to measure pick-up ions, electrons, and other energetic ions energized by processes such as charge exchange of Pluto's escaping atmospheric neutrals with solar ions and photonsand by the expected bow shock resulting from the interaction between the solar wind plasma and the atmosphere. In addition to measurements in the Pluto/Charon system (closest approach planned for 14 July 2015), PEPSSI makes observations of energetic particles in the solar wind during the cruise to Pluto, and in 2007 made the most extensive energetic particle measurements in Jupiter's magnetotail as the spacecraft traveled over 1 AU down the tail. B = box-like slab 2D shapes, roughly polygonS = Detector SectorMain publication: McNutt et al. 2008: The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons MissionPublished: 25 October 2008Volume 140, pages 315-385, (2008)https://doi.org/10.1007/s11214-008-9436-yhttps://doi.org/10.1007/s11214-008-9436-yThis particular dataset is related to PEPSSI B (box-like slab 2D shape, roughly polygon) Triples Flux [or differential intensity, which is physically calibrated data with units of 1/(cm^2 sr s keV)] ~15 keV to 1 MeV, The original datafiles:PEPSSI_Reduced_BFLUX_NNNN_M.csvwhere NNNN = year from 2012 to 2025, and M = 'A' or 'B' is a calibration regime

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-diff-intensity-bflux-spectra-a/new-horizons_pepssi_triples-diff-intensity-bflux-spectra-a_20120128_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9549% of the 6644 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/pepssi/cdf/triples-diff-intensity-bflux-spectra-b/new-horizons_pepssi_triples-diff-intensity-bflux-spectra-b_20140703_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8333% of the 2994 timesteps.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/helio1hr/new_horizons_helio1hr_position_20060120_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 209927 timesteps. 

Data from New Horizons Solar Wind Around Pluto instrument.Elliott, H. A., D. J. McComas, Zirnstein, E. J., Randol, B. M., Delamere, P. A., Livadiotis, G., et al. (2019). Slowing of the Solar Wind in the Outer Heliosphere. Astrophysical Journal, 885(2). DOI 10.3847/1538-4357/ab3e49.Elliott, H. A., D. J. McComas, P. Valek, G. Nicolaou, S. Weidner, and G. Livadiotis (2016), ApJS, 223(2), 1-21, doi:10.3847/0067-0049/223/2/19.McComas, D. et al. (2008), The Solar Wind Around Pluto (SWAP) Instrument Aboard New Horizons, Space Sci Rev, 140(1), 261-313, doi:10.1007/s11214-007-9205-3.

NASA New Horizons Mission Page for the Solar Wind Around Pluto, SWAP, Instrument

SPDF/CDAWeb. Please also acknowledge the data producer: David J. McComas at Princeton

SPDF/SSCWeb. Please also acknowledge the data producer: David J. McComas at Princeton

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David J. McComas at Princeton

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/swap/ions/new_horizons_swap_pickup-ions_20081108180800_v1.0.0.cdf. The most common cadence, 1952000000000 [ns] = PT32M32S, occurred for 88.5678% of the 44562 timesteps. 

Solar Wind Around Pluto (from all.xml/instrument/description/@short)

The middle of the UTC time of the coarse-fine energy sweep used to determine the solar wind parameters.

NH SWAP: Index that characterizes non-adiabatic cooling of interstellar pickup ions

An index that characterizes non-adiabatic cooling of interstellar pickup ions

Data from New Horizons Solar Wind Around Pluto instrument.Elliott, H. A., D. J. McComas, P. Valek, G. Nicolaou, S. Weidner, and G. Livadiotis (2016), ApJS, 223(2), 1-21, doi:10.3847/0067-0049/223/2/19.McComas, D. et al. (2008), The Solar Wind Around Pluto (SWAP) Instrument Aboard New Horizons, Space Sci Rev, 140(1), 261-313, doi:10.1007/s11214-007-9205-3.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/new-horizons/swap/ions-histogram/new_horizons_swap_pickup-ions-histogram_20081031180800_v1.0.1.cdf. The most common cadence, 86400000000000 [ns] = P1D, occurred for 73.9394% of the 854 timesteps. 

The start UTC time of the coarse-fine energy sweep used to determine the solar wind parameters. (No Plot)

The stop UTC time of the coarse-fine energy sweep used to determine the solar wind parameters. (No Plot)

The start MET time of the coarse-fine energy sweep used to determine the solar wind parameters.

The stop MET time of the coarse-fine energy sweep used to determine the solar wind parameters.

NH SWAP: X component of the spacecraft position in Heliographic Inertial coordinates

The x component of the center of the spacecraft position in HGI coordinates in units of AU.

NH SWAP: Y component of the spacecraft position in Heliographic Inertial coordinates

The y component of the center of the NH spacecraft position in HGI coordinates in units of AU.

NH SWAP: Z component of the spacecraft position in Heliographic Inertial coordinates

The z component of the center of the spacecraft position in HGI coordinates in units of AU.

NH SWAP: Distance of the spacecraft in Heliographic Inertial coordinates

The distance to the center of the NH spacecraft position from the center of the HGI coordinate system (Sun) in units of AU.

NH SWAP: Latitude of the spacecraft in Heliographic Inertial coordinates

The latitude of the center of the NH spacecraft position in HGI coordinates in degrees.

NH SWAP: Longitude of the spacecraft in Heliographic Inertial coordinates

The longitude of the center of the NH spacecraft position in HGI coordinates in degrees.

NH SWAP: X component of the spacecraft position in Heliocentric Aries Ecliptic J2000 coordinates

The x component of the center of the spacecraft position in HAE coordinates in units of AU.

NH SWAP: Y component of the spacecraft position in Heliocentric Aries Ecliptic J2000 coordinates

The y component of the center of the spacecraft position in HAE coordinates in units of AU.

NH SWAP: Z component of the spacecraft position in Heliocentric Aries Ecliptic J2000 coordinates

NH SWAP: Latitude of the spacecraft in Heliocentric Aries Ecliptic J2000 coordinates

The latitude of the center of the spacecraft position in HAE coordinates in units of degrees.

NH SWAP: Longitude of the spacecraft in Heliocentric Aries Ecliptic J2000 coordinates

The longitude of the center of the spacecraft position in HAE coordinates in units of degrees.

NH SWAP: X component of the spacecraft position in Heliographic coordinates

The x component of the center of the spacecraft position in HG coordinates in units of AU.

NH SWAP: Y component of the spacecraft position in Heliographic coordinates

The y component of the center of the spacecraft position in HG coordinates in units of AU.

NH SWAP: Z component of the spacecraft position in Heliographic coordinates

The latitude of the center of the spacecraft position in HG coordinates in units of degrees.

NH SWAP: Longitude of the spacecraft in Heliographic coordinates

The longitude of the center of the spacecraft position in HG coordinates in units of degrees.

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-05/TIROS-N

TIROS/NOAA SEM MEPED Data Archive                                                   This is the re-processed version of the MEPED (Medium Energy Proton Electron Detector) data archive from the TIROS/NOAA spacecraft. The raw data from the NOAA archive have been processed to 1 minute resolution; magnetic field parameters (GSM Bx, By, Bz, B/Bmin, and L) are derived in 4 magnetic field models: IGRF, Tsyganenko 89 (T89), Tsyganenko 96 (T96), Tsyganenko 01 (T01); T89, T96, and T01 magnetic field models are driven with solar wind parameters and geomagnetic indices obtained from OMNI-2 data detector counts, omni and perpendicularelectron and proton flux are archived. Details of the processing can be found from http://radbelts.gsfc.nasa.gov.Processing was done by:                                                            Shing F. Fung, Lun C. Tan, Xi Shao                Space Physics Data Facility                 Goddard Space Flight Center, NASA                 Greenbelt, MD 20771                USA                                       .                              e-mail: Shing.F.Fung@nasa.gov        

NOAA/POES MEPED Data Documentation: NOAA-5 to NOAA-14 Data Reprocessed at GSFC/SPDF, authored by Tan, L.C., Fung, S.F., and X. Shao, internal White Paper hosted by the CDAWeb at Goddard Space Flight Center, GSFC.

SPDF/CDAWeb. Please also acknowledge the data producer: Shing F. Fung at SPDF, GSFC/NASA

SPDF/SSCWeb. Please also acknowledge the data producer: Shing F. Fung at SPDF, GSFC/NASA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Shing F. Fung at SPDF, GSFC/NASA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa05/1978/noaa05_meped1min_sem_19781102_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.6390% of the 552 timesteps. 

Polar Operational Environmental Satellite (from all.xml/observatory/description/@short)

Space Environment Monitor (from all.xml/instrument/description/@short)

Polar Operational Environmental Satellite (from Master/CDFglobalAttributes/Source_name)

MEPED Count Rates for 0 Deg. telescopes, 5 proton  and 3 electron energy bands (counts_0dg)

MEPED Count Rates for 81/83 Deg. telescopes, 5 proton  and 3 electron energy bands (counts_90dg)

MEPED Count Rates for omnidirectional proton telescope, 3 energy bands (counts_omni)

MEPED calculated perpendicular proton flux, 5 energy bands (Jperp_p)

MEPED calculated perpendicular electron flux, 3 energy bands (Jperp_e)

MEPED calculated omnidirectional proton flux,  5 energy bands from 0/81 and 3 from omni telescopes

MEPED calculated omnidirectional electron flux,  3 energy bands from 0/83 telescopes

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-06

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa06/1979/noaa06_meped1min_sem_19790628_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 97.5992% of the 935 timesteps. 

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-07

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa07/1981/noaa07_meped1min_sem_19810711_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.8347% of the 1208 timesteps. 

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-08

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa08/1983/noaa08_meped1min_sem_19830509_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 98.6755% of the 298 timesteps. 

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-10

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa10/1986/noaa10_meped1min_sem_19861011_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.8564% of the 1391 timesteps. 

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-12

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa12/1991/noaa12_meped1min_sem_19910601_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1438 timesteps. 

1 minute re-processed particle count rates, fluxes, and model fields, SEM-1 MEPED, NOAA-14

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa14/1995/noaa14_meped1min_sem_19950111_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1384 timesteps. 

MEPED Count Rates for 0 Deg. telescopes, 4 proton  and 2 electron energy bands (counts_0dg)

MEPED Count Rates for 81/83 Deg. telescopes, 2 electron energy bands (counts_90dg)

MEPED calculated perpendicular electron flux, 2 energy bands (Jperp_e)

MEPED calculated omnidirectional proton flux,  3 energy bands from omni telescopes

MEPED calculated omnidirectional electron flux,  2 energy bands from 0/83 telescopes

NOAA15 POES-SEM2 2-second Particle Precipitation Data [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa15/sem2_fluxes-2sec/2013/noaa15_poes-sem2_fluxes-2sec_20130101_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.9954% of the 43120 timesteps. 

NOAA16 POES-SEM2 2-second Particle Precipitation Data [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa16/sem2_fluxes-2sec/2013/noaa16_poes-sem2_fluxes-2sec_20130101_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.9977% of the 43162 timesteps. 

NOAA18 POES-SEM2 2-second Particle Precipitation Data [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa18/sem2_fluxes-2sec/2013/noaa18_poes-sem2_fluxes-2sec_20130101_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.9953% of the 42888 timesteps. 

NOAA19 POES-SEM2 2-second Particle Precipitation Data [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/noaa/noaa19/sem2_fluxes-2sec/2013/noaa19_poes-sem2_fluxes-2sec_20130101_v01.cdf. The most common cadence, 2000000000 [ns] = PT2S, occurred for 99.9954% of the 43170 timesteps. 

OMNI Combined, Definitive, Hourly IMF and Plasma Data, and Energetic Proton Fluxes, Time-Shifted to the Nose of the Earth's Bow Shock, plus Solar and Magnetic Indices

Hourly averaged definitive multispacecraft interplanetary parameters dataOMNI Data Documentation: https://omniweb.gsfc.nasa.gov/html/ow_data.htmlAdditional data access options available at  SPDF's OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow.htmlCOHOWeb-formatted OMNI_M merged magnetic field and plasma data http://cohoweb.gsfc.nasa.gov/Recent OMNI 1-HR Updates News: https://omniweb.gsfc.nasa.gov/html/ow_news.htmlData variables with 1800 in their names use time stamps on the half-hour (1800 seconds) to reflect the mid-point of the hourly data, and are tied to the EPOCH_1800 time variables

SPDF/CDAWeb. Please also acknowledge the data producer: J.H. King, N. Papitashvili at ADNET, NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J.H. King, N. Papitashvili at ADNET, NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.H. King, N. Papitashvili at ADNET, NASA GSFC

Merged 1 Hour Interplantary OMNI data (from all.xml/observatory/description/@short)

IMF, Plasma, Indices, Energetic Proton Flux (from all.xml/instrument/description/@short)

OMNI (1AU IP Data) (from Master/CDFglobalAttributes/Source_name)

Merged 1 Hour Interplantary OMNI data (from Master/CDFglobalAttributes/Source_name)

IMF, Plasma, Indices, Energetic Proton Flux (from all.xml/instrument/@ID)

OMNI ID code for the source spacecraft for time-shifted IMF values (see OMNI documentation link for codes) (half-hour midpoint)

OMNI ID code for the source spacecraft for time-shifted IP plasma values (see OMNI documentation link for codes) (half-hour midpoint)

1AU IP Average B Field Magnitude, nT, (last currently-available OMNI B-field data Dec 24, 2025) (half-hour midpoint)

1AU IP Magnitude of average field vector (nT) (half-hour midpoint)

1AU IP Latitude/Theta of average B vector (deg) (half-hour midpoint)

1AU IP Longitude/Phi of average B vector (deg) (half-hour midpoint)

RMS deviation of magnitude of the average vector field (nT) (half-hour midpoint)

1AU IP Plasma Temperature, deg K, (last currently-available OMNI plasma data Jan 07, 2026) (half-hour midpoint)

1AU IP plasma flow direction longitude (deg),  phi (half-hour midpoint)

1AU IP plasma flow direction latitude (deg), theta (half-hour midpoint)

RMS deviation of plasma temperature (deg k) (half-hour midpoint)

RMS deviation of ion number density (per cc) (half-hour midpoint)

RMS deviation in plasma flow velocity (km/s) (half-hour midpoint)

RMS deviation in plasma flow  direction longitude (deg), phi (half-hour midpoint)

RMS deviation in plasma flow direction latitude (deg), theta (half-hour midpoint)

1AU Proton flux > 1 MeV, 1/(SQcm-ster-s), (last currently-available OMNI proton fluxes Mar 04, 2020) (half-hour midpoint)

Magnetospheric Contamination of 1AU Proton Flux code (6=No,<=5 see OMNI documentation) (half-hour midpoint)

Daily sunspot number V2, from  http://sidc.oma.be/silso/datafiles/ (1963/001-2025/334) (half-hour midpoint)

F10.7 - Daily 10.7 cm solar radio flux, units: 10**(-22) Joules/second/square-meter/Hertz, from NGDC (1963/001-2026/012), (half-hour midpoint)

Kp - 3-hour Kp*10 (Kp=1-,1,1+ corresponds to 7,10,13), fromNGDC (1963/001-2026/012) (half-hour midpoint)

Dst - 1-hour Dst index (1963/001-2014/366), Provisional Dst (2021/001-2025/181), Quick-look Dst (2025/182-2026/012), from WDC Kyoto (half-hour midpoint)

AE - 1-hour AE-index,from WDC Kyoto (1963/001-1988/182), Provisional (1990/001-2020/365), from WDC Kyoto (half-hour midpoint)

ap - 3-hour ap-index (1963/001-2026/012), from NGDC (half-hour midpoint)

AL - 1-hour AL-index, from WDC Kyoto (1963/001-1988/182), Provisional (1990/001-2018/059), from WDC Kyoto (half-hour midpoint)

AU - 1-hour AU-index,from WDC Kyoto (1963/001-1988/182), Provisional (1990/001-2018/059), from WDC Kyoto (half-hour midpoint)

PC - 1-hour Polar Cap index (North, Thule station), from NGDC (Final 1975/001-2024/365) (half-hour midpoint)

Solar wind (magnetic energy density)/(kinetic energy density) (half-hour midpoint)

OMNI Combined merged hourly magnetic field, plasma and ephermis data

Hourly averaged definitive multispacecraft interplanetary parameters dataThe Heliographic Inertial (HGI) coordinates are Sun-centered and inertially fixed with respect to an X-axis directed along the intersection line of the ecliptic and solar equatorial  planes. The solar equator plane is inclined at 7.25 degrees from the ecliptic. This direction was towards ecliptic longitude of 74.367 degrees on 1 January 1900 at 1200 UT; because of precession of the celestial equator, this longitude increases by 1.4 degrees/century. The Z axis  is  directed perpendicular and northward from the solar equator, and the Y-axis completes the right-handed set. This system differs from the usual heliographic coordinates (e.g. Carrington longitudes) which are fixed in the frame of the rotating Sun.The RTN system is fixed at a spacecraft (or the planet). The R axis is directed radially away from the Sun, the T axis is the cross product of the solar rotation axis and the R axis, and the N axis is the cross product of the R and T axes.  At zero heliographic latitude, when the spacecraft is in the solar equatorial plane, the N and solar rotation axes are parallel.Latitude and longitude angles of solar wind plasma flow are generally measured  from the radius vector away from the Sun. In all cases, latitude angles are positive for north-going flow.  The flow longitude angles have been treated differently for the near-Earth data, i.e. the OMNI, and for the deep space data. The flow is positive for the  near-Earth data when coming from the right side of the Sun as viewed  from  the Earth, i.e. flowing toward +Y from -X GSE or opposite to the direction of planetary motion. On the other hand, the flow longitudes for the deep space spacecraft use the opposite sign convection, i.e. positive for flow in the +T direction in the RTN system.

SPDF/CDAWeb. Please also acknowledge the data producer: J.H. King, N. Papatashvilli at AdnetSystems, NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: J.H. King, N. Papatashvilli at AdnetSystems, NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.H. King, N. Papatashvilli at AdnetSystems, NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/omni/coho1hr_magplasma/1963/omni_coho1hr_merged_mag_plasma_19630101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Merged 1 Hour Interplantary OMNI data in RTN system (from all.xml/observatory/description/@short)

merged magnetic field and plasma data from cohoweb (from all.xml/instrument/description/@short)

Merged 1 Hour Interplantary OMNI data in RTN system (from Master/CDFglobalAttributes/Source_name)

Definitive Hourly data from cohoweb (from Master/CDFglobalAttributes/Data_type)

merged magnetic field and plasma data from cohoweb (from all.xml/instrument/@ID)

OMNI Combined, Definitive 1-minute IMF and Definitive Plasma Data Time-Shifted to the Nose of the Earth's Bow Shock, plus Magnetic Indices

1minute averaged definitive multispacecraft interplanetary parameters dataAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb.gsfc.nasa.gov/html/HROdocum.htmlAdditional data access options available at  SPDF's OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlRecent omni high resolution updates Release Notes: https://omniweb.gsfc.nasa.gov/html/hro_news.htmlTime stamps are for the beginning of each data averaging time bin.

OMNI Data Documnetation for 1 min and 5 min solar wind data sets at the Earth's bow shock nose

Goddard Space Flight Center, GSFC, Space Physics Data Facility, SPDF, OMNIWeb Service

Goddard Space Flight Center, GSFC, Space Physics Data Facility, SPDF, OMNIWeb Service. Additional data access options for high resolution (1 min and 5 min) OMNI solar wind magnetic field and plasma data at Earth's bow shock nose, geomagnetic activity indices, and energetic proton fluxes (5 min data only).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/omni/hro2_1min/1995/omni_hro2_1min_19950101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 44639 timesteps. 

Merged 1 minute Interplantary OMNI data (from all.xml/observatory/description/@short)

IMF and Plasma data (from all.xml/instrument/description/@short)

Merged 1 minute Interplantary OMNI data (from Master/CDFglobalAttributes/Source_name)

Definitive 1minute (modified) (from Master/CDFglobalAttributes/Data_type)

OMNI ID code for the source spacecraft for time-shifted IMF values (see OMNI documentation link for codes)

OMNI ID code for the source spacecraft  for time-shifted IP plasma values (see OMNI documentation link for codes)

Magnitude of avg. field vector (nT) (last currently-available OMNI B-field data Dec 09, 2025)

Proton density (n/cc) (last currently-available OMNI plasma data Dec 09, 2025)

AE - 1-minute AE-index, from WDC Kyoto (Final 1988/001-1988/182, Provisional 1990/001-2020/365)

AL - 1-minute AL-index, from WDC Kyoto (Final 1988/001-1988/182, Provisional 1990/001-2020/365)

AU - 1-minute AU-index,from WDC Kyoto  (Final 1988/001-1988/182, Provisional 1990/001-2020/365)

OMNI Combined, Definitive 5-minute IMF and Definitive Plasma, and Energetic Proton Fluxes, Time-Shifted to the Nose  of the Earth's Bow Shock, plus Magnetic Indices

5minute averaged definitive multispacecraft interplanetary parameters dataAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb.gsfc.nasa.gov/html/HROdocum.htmlAdditional data access options available at  SPDF's OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlRecent omni high resolution updates Release Notes: https://omniweb.gsfc.nasa.gov/html/hro_news.htmlTime stamps are for the beginning of each data averaging time bin.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/omni/hro2_5min/1995/omni_hro2_5min_19950101_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 8927 timesteps. 

Merged 5 minute Interplantary OMNI data (from all.xml/observatory/description/@short)

Merged 5 minute Interplantary OMNI data (from Master/CDFglobalAttributes/Source_name)

Definitive 5minute (modified) (from Master/CDFglobalAttributes/Data_type)

OMNI ID code for the source spacecraft for time-shifted IP plasma values (see OMNI documentation link for codes)

AE - 5-minute AE-index, from WDC Kyoto (Final 1988/001-1988/182, Provisional 1990/001-2020/365)

AL - 5-minute AL-index, from WDC Kyoto (Final 1988/001-1988/182, Provisional 1990/001-2020/365)

AU - 5-minute AU-index,from WDC Kyoto  (Final 1988/001-1988/182, Provisional 1990/001-2020/365)

Proton flux >10 MeV (1/(SQcm-ster-s)) (all fluxes from GOES 1986/001-2020/063)

OMNI Combined, Definitive, 1-minute IMF and Plasma Data Time-Shifted to the Nose of the Earth's Bow Shock, plus Magnetic Indices

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/omni/hro_1min/1981/omni_hro_1min_19810101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 44639 timesteps. 

Magnitude of avg. field vector (nT) (last currently-available OMNI B-field data Dec 24, 2025)

Proton density (n/cc) (last currently-available OMNI plasma data Dec 24, 2025)

PC - 1-minute Polar Cap index (North, Qaanaaq geomagnetic observatory), from DTU Space, Technical University of Denmark  (1981/001-2024/365)

OMNI Combined, Definitive, 5-minute IMF and Plasma, and Energetic Proton Fluxes, Time-Shifted to the Nose  of the Earth's Bow Shock, plus Magnetic Indices

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/omni/hro_5min/1981/omni_hro_5min_19810101_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 8927 timesteps. 

PC - 5-minute Polar Cap index (North, Qaanaaq geomagnetic observatory), from DTU Space, Technical University of Denmark (1981/001-2024/365)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/phobos/phobos2/helio1day/phobos2_helio1day_position_19880713_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 201 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/phobos/phobos2/helio1hr/phobos2_helio1hr_position_19880713_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4847 timesteps. 

Pioneer-10 merged hourly magnetic field, plasma, proton fluxes, and ephermis data

Pioneer10 COHOweb connectionThe main science objectives for the PIONEER interplanetary mission are as  follows:   search for the heliospheric boundary with interstellar space;    study the large-scale structure of the solar wind plasma and interplanetary magnetic field within the heliosphere;   investigate propagation of solar and galactic energetic particles in the heliosphere;   measure the radial gradient, spectra, and nuclear composition of the anomalous cosmic rays from the solar wind termination shock;   study acceleration of energetic particles by solar flare shocks and corotating interaction regions within the heliosphere.PI of magnetic field data: Dr. Edward J. Smith, NASA JPL.  PI of plasma data: Dr. Aaron Barnes, Ames Research Center, NASA;  plasma data were provided by Dr. P. Gazis, ARC. For the hourly resolution records, the PIONEER_10 directory contains hourly averages of parameters for the interplanetary  magnetic field (1972-Mar-3 (63) - 1975-Nov-17 (321)), solar wind plasma (1972-Apr-18 (109) - 1995-Sep-07 (250)), spacecraft trajectory coordinates (1972-Mar-3 (63) - 1995-Dec-31 (365)) and Proton Fluxes (1972-Mar-15 - 1994-Nov-18)Time Coverage of merged files: March 3, 1972 - December 31, 1995 Pioneer-10 data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions:   All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.   merging of trajectory coordinates, magnetic field data, and plasma data files into a single annual file P10_YR.DAT, where YR is the year;   Data gaps were filled with dummy numbers for the missing hours or entire days to make all files of equal length.  The character '9' is used to  fill all fields for missing data according to their format, e.g. (9999.9) for a field with the FORTRAN format F7.1. Note that format F7.1 below really means (1X,F6.1),etc.

SPDF/CDAWeb. Please also acknowledge the data producer: E.J. Smith (HVM) and A. Barnes (PLS) at NASA JPL/AMES

SPDF/SSCWeb. Please also acknowledge the data producer: E.J. Smith (HVM) and A. Barnes (PLS) at NASA JPL/AMES

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: E.J. Smith (HVM) and A. Barnes (PLS) at NASA JPL/AMES

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer10/merged/coho1hr_magplasma_cdaweb/1972/pioneer10_coho1hr_merged_mag_plasma_19720101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer10/helio1day/pioneer10_helio1day_position_19720304_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 28426 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer10/helio1hr/pioneer10_helio1hr_position_19720304_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 682247 timesteps. 

This data set from the Pioneer 10 Helium Vector Magnetometer (HVM) consists of one minute averages of vector components and scalar magnitudes of the interplanetary magnetic field. The three components (Br, Bt, Bn) are given in the RTN coordinate system and all magnetic fields are expressed in nanotelsa units. The scalar magnitudes (B) are averages of higher resolution scalar magnitudes. The time tag for each one-minute interval is the midpoint of the averaging interval in SCET-UT (Spacecraft Event Time - UT). The averages were originally calculated over one-minute intervals in Ground Received Time, and the midpoints have been converted to SCET-UT. The file P10_LIGHTTIME contains daily values for the one-way light-time delay. No records are written for data gaps. Most files cover 28 or 35 days, but there are a number of shorter files, particularly at year boundaries. Data for the Jupiter encounter, days 329-349 of 1973, are not included. The RTN system is fixed to the sun-spacecraft line and aligned with the solar heliographic equator. The R axis is the radial direction to the spacecraft, the T axis is the cross product of the solar rotation axis and the R axis, and N is the cross product of R and T.  The file P10HVM_15M.SFD provides a detailed description of the Pioneer spacecraft, the HVM experiment, and the data. This ASCII document is written in Standard Formatted Data Unit (SFDU) format as part of NSSDC data set 72-012A-01I for 15-minute averaged data covering 1972-03-03 to 1975-11-17. Data Set Files: P10HVMMN_FMT.txt     - this document (ASCII) P10HVM_15M.SFD       - SFDU metadata extract from Pioneer 10 HVM 15-min. data set Myyddd.asc           - 1-minute data files from Pioneer 10 HVM starting at date yyddd P10_LIGHTTIME.asc    - data file with one-way light-time delays (ASCII) Related Information and Data: Further details on the spacecraft, experiment, data sets at NSSDC, and related WWW sites can be found on the Pioneer 10/11 flight project page under  http://nssdc.gsfc.nasa.gov/space/ Hour averages of the interplanetary solar wind data from, and hourly heliocentric coordinates of, Pioneer 10/11 and other interplanetary spacecraft may be also be accessed and plotted on-line through the COHOWeb service based at the same WWW site as above. Pioneer data on NDADS (NASA"s Data Archive and Distribution Service) may be located on the WWW via the SPyCAT service at the above URL or an e-mail message to ARMS (Automated Retrieval Mail System) at archives@ndadsa.gsfc.nasa.gov with "HOLDINGS" on the subject line.   Acknowledgement: Use of these data in publications should be accompanied at minimum by acknowledgements of the National Space Science Data Center and the responsible Principal Investigator defined in the experiment documentation provided here. Citation of NSSDC"s Coordinated Heliospheric Observations (COHO) data base would also be appreciated, so that other potential users will be made aware of this service.   Data Set Coverage (yyyy-mm-dd): 1972-03-03 to 1975-11-17 Data Set Contact: Joyce Wolf, NASA JPL

Pioneer 10 Helium Vector Magnetometer, HVM, ASCII Data File Description

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_light_time.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_light_time.)

Helium Vector Magnetometer (from all.xml/instrument/description/@short)

Pioneer10 1-min averaged Magnetic Field (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer10/cdaweb/1min_mag/1972/pioneer10_mag_1min_magnetic_field_19720303_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 98.8447% of the 378751 timesteps. 

Counts based on variable 'Epoch_light_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer10/cdaweb/1min_mag/1972/pioneer10_mag_1min_magnetic_field_19720303_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 97.6974% of the 297 timesteps. 

Pioner-11 merged hourly magnetic field, plasma, proton fluxes,  and ephermis data

Pioneer11 COHOweb connectionThe main science objectives for the PIONEER interplanetary mission are as  follows:   search for the heliospheric boundary with interstellar space;    study the large-scale structure of the solar wind plasma and interplanetary magnetic field within the heliosphere;   investigate propagation of solar and galactic energetic particles in the heliosphere;   measure the radial gradient, spectra, and nuclear composition of the anomalous cosmic rays from the solar wind termination shock;   study acceleration of energetic particles by solar flare shocks and corotating interaction regions within the heliosphere.PI of magnetic field data: Dr. Edward J. Smith, NASA JPL.  PI of plasma data: Dr. Aaron Barnes, Ames Research Center, NASA;  plasma data were provided by Dr. P. Gazis, ARC. For the hourly resolution records, the PIONEER_11 directory contains hourly averages of parameters for the interplanetary  magnetic field (1973-Apr-6 - 1992-Aug-1, solar wind plasma (1973-Apr-21  - 1992-May-30), Proton Fluxes (1972-Mar-15 - 1994-Nov-18), and spacecraft trajectory coordinates (1973-Apr-6  - 1992-Aug-1). Time Coverage of merged files: April 6, 1973 - August 1, 1992 Pioneer-11 data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions:   All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.   merging of trajectory coordinates, magnetic field data, and plasma data files into a single annual file P11_YR.DAT, where YR is the year;   Data gaps were filled with dummy numbers for the missing hours or entire days to make all files of equal length.  The character '9' is used to  fill all fields for missing data according to their format, e.g. (9999.9) for a field with the FORTRAN format F7.1. Note that format F7.1 below really means (1X,F6.1),etc.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer11/merged/coho1hr_magplasma_cdaweb/1973/pioneer11_coho1hr_merged_mag_plasma_19730101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer11/helio1day/pioneer11_helio1day_position_19730407_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 28027 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer11/helio1hr/pioneer11_helio1hr_position_19730407_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 672671 timesteps. 

PioneerVenus merged hourly magnetic field, plasma and ephermis data

PIONEER VENUS ORBITER (PVO) was the first orbiter mission designed to conduct a comprehensive and long term investigation of the planet Venus.  PVO measured the detailed structure of the upper atmosphere and ionosphere of Venus and investigated the interaction of the solar wind magnetic field and plasma with the venusian ionosphere. Over the years 1978-1992 PVO provided nearly continuous measurements of the solar wind from its highly eccentric orbit around Venus.PI of magnetic field data: Dr. T. C. Russell, UCLA.PI of plasma data: Dr. Aaron Barnes, Ames Research Center, NASA. plasma data were provided by Dr. P. Gazis, Ames,NASA.For the hourly resolution records, thePVO directory contains files with hourly averages for selected parameters of the interplanetary magnetic field (1978-12-05 - 1988-08-07) solar wind plasma (1978-12-05 - 1992-10-08) and the spacecraft trajectory (1978-12-05 - 1992-12-31) in RTN, and in Venus-centered (1978-12-05 - 1988-08-07) coordinates.  These were data taken from time intervals when the spacecraft was outside the bow shock of the venusian ionosphere and in the solar wind.Time Coverage of merged files: 78-12-05 - 92-12-31.PVO data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions:- All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.- calculation of RTN components of interplanetary magnetic field from VSO coordinates.- merging of trajectory coordinates, magnetic field data, and plasma data files into a single annual file PVO_YR.ascii, where YR is the year;- Data gaps were filled with dummy numbers for the missing hours or entire days to make all files of equal length.  The character \'9\' is used to fill all fields for missing data according to their format, e.g. \' 9999.9\' for a field with the FORTRAN format F7.1. Note that format F7.1 below really means (1X,F6.1),etc.The Heliographic Inertial (HGI) coordinates are Sun-centered and inertially fixed with respect to an X-axis  directed along the intersection line of the ecliptic and solar equatorial planes.  The solar equator plane is inclined at 7.25 degrees from the ecliptic. This direction was towards ecliptic longitude of 74.36 degrees on 1 January 1900 at 1200 UT; because of precession of the celestial equator, this longitude increases by 1.4 degrees/century. The Z axis is directed perpendicular and northward from the solar equator, and the Y-axis completes the right-handed set.  This system differs from the usual heliographic coordinates  (e.g. Carrington longitudes) which are fixed in the frame of the rotating Sun.The RTN system is fixed at a spacecraft (or the planet). The R axis is directed radially away from  the Sun, the T axis is the cross product of the solar rotation axis and the R axis, and the N axis is the cross product of R and T.  At zero Heliographic Latitude when the spacecraft is in the solar equatorial plane the N and solar rotation axes are parallel.Venus Solar Orbital (VSO) coordinates are defined with respect to the orbital plane of Venus which is tilted about two degrees from the Ecliptic.  The VSO system is Venus-centered with the X axis towards the Sun, the Z axis northward and perpendicular to the orbital plane, and the Y axis completing the right hand system.Acknowledgement: Hour averages of the interplanetary solar wind data from, and hourly heliocentric coordinates of, PVO and other interplanetary spacecraft may be also be accessed and plotted on-line through the COHOWeb service http://cohoweb.gsfc.nasa.gov/

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. T. C. Russell (magnetic field), Dr. Aaron Barnes (plasma) at UCLA, NASA/Ames

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. T. C. Russell (magnetic field), Dr. Aaron Barnes (plasma) at UCLA, NASA/Ames

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. T. C. Russell (magnetic field), Dr. Aaron Barnes (plasma) at UCLA, NASA/Ames

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer_venus/merged/coho1hr_magplasma_cdaweb/1978/pioneervenus_coho1hr_merged_mag_plasma_19781205_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 647 timesteps. 

Merged Trajectory, Magnetic Field, and Plasma (from all.xml/instrument/description/@short)

Pioneer Venus Orbiter (PVO) was the first orbiter mission designed to conduct a comprehensive and long term investigation of the planet Venus.  PVO measured the detailed structure of the upper atmosphere and ionosphere of Venus and investigated the interaction of the solar wind with the Venusian ionosphere. Over the years 1978-1992 PVO provided nearly continuous measurements of the solar wind from its highly eccentric orbit around Venus.PI of magnetic field data: Dr. C.T. Russell, UCLA.PI of plasma data: Dr. Aaron Barnes, Ames Research Center, NASA.The 10-min data include 10-minute averages for selected parameters of the interplanetary magnetic field, solar wind plasma, and spacecraft trajectory. The data were taken when the spacecraft was outside the bow shock of the Venusian ionosphere and was in the solar wind.Time coverage of merged data: 78-12-06 - 88-08-07.PVO data were converted to CDF based on the  flatfiles from UCLA.Venus Solar Orbital (VSO) coordinates are defined with respect to the orbital plane of Venus which is tilted about two degrees from the Ecliptic.  The VSO system is Venus-centered with the X axis towards the Sun, the Z axis northward and perpendicular to the orbital plane, and the Y axis completing the right hand system.

General information and Documentation concerning the Pioneer Venus Orbiter spacecraft

General information concerning the Pioneer Venus Orbiter, Magnetometer, OMAG, instrument

General information concerning the Pioneer Venus Orbiter, Solar Wind Plasma Analyzer, OPA, instrument

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. C.T. Russell (magnetic field), Dr. Aaron Barnes (plasma) at UCLA, NASA/Ames

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. C.T. Russell (magnetic field), Dr. Aaron Barnes (plasma) at UCLA, NASA/Ames

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. C.T. Russell (magnetic field), Dr. Aaron Barnes (plasma) at UCLA, NASA/Ames

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/pioneer/pioneer_venus/merged/10m_magplasma_cdf/pioneervenus_merged_solar-wind_10m_19781206_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 98.6132% of the 297242 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/pluto_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/pluto_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

Instrument description in https://doi.org/10.5194/amt-13-5681-2020

Users are encouraged to contact the PI for early discussion of analysis projects and to offer co-authorship when publishing results derived from BOLIDE data

SPDF/CDAWeb. Please also acknowledge the data producer: Bernd Kaifler, bernd.kaifler@dlr.de at DLR, IPA

SPDF/SSCWeb. Please also acknowledge the data producer: Bernd Kaifler, bernd.kaifler@dlr.de at DLR, IPA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Bernd Kaifler, bernd.kaifler@dlr.de at DLR, IPA

Polar Mesospheric Cloud Turbulence (from all.xml/observatory/description/@short)

Balloon lidar experiment (from all.xml/instrument/description/@short)

Mesosphere and Thermosphere Dynamics (from Master/CDFglobalAttributes/Discipline)

Polar Mesospheric Cloud Turbulence (from Master/CDFglobalAttributes/Source_name)

Volume backscatter coefficients (from Master/CDFglobalAttributes/Data_type)

Beam pointing clockwise from north, from gondola yaw angle + 90 deg of CSBFs TDRSS log

Latitude of lidar beam at 82 km altitude, given azimuth, floating altitude and 28 deg off-zenith beam angle

Longitude of lidar beam at 82 km altitude, given azimuth, floating altitude and 28 deg off-zenith beam angle

volume backscatter coefficient beta derived from Rayleigh lidar data at a threshold of 2.5 sigma above background

Reference: HYDRA is a 3-Dimensional Electron and Ion Hot Plasma Instrumentfor the Polar Spacecraft of the GGS Mission, J. Scudder et al., Space Sci. Rev., 71,459-495, Feb. 1995. http://www-st.physics.uiowa.edu This data set contains survey electron and proton moments for density, bulk velocity (GSM), temperature: parallel, perpendicular, at 13.8-second resolution as determined (0-20keV). Higher quality data products may be available from the P.I.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Scudder at U of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: J. Scudder at U of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Scudder at U of Iowa

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/hydra/moments-14sec/1996/polar_hydra_moments-14sec_19960320_v02.cdf. The most common cadence, 13800 [ms] = PT13.8S, occurred for 96.8852% of the 2364 timesteps. 

Polar Plasma Laboratory (from all.xml/observatory/description/@short)

Fast Plasma Analyzer (from all.xml/instrument/description/@short)

Polar Plasma Laboratory (from Master/CDFglobalAttributes/Source_name)

Important Warning: The data described below is meant for archival purposes.  It should not be considered as highly accurate data.  For example, accurate data requires a correction in the form of an offset to the Sunward component of the electric field.  A constant offset of 1.2 mV/m has been used for all the data, this being an approximate average value.  In fact, however, the offset varies with time, and must be determined by analysis of the particular time of interest.  Users of this data desiring more information should get in touch with Dr. Forrest Mozer, at the Space Sciences Laboratory, University of California, Berkeley.The electric field data is at spin period time resolution. This means that there is 1 data point about every 6 seconds. However, it should be noted that there can be longer intervals between data points, due to missing data.  Data gaps are not filled in.The components of the electric field are given in a coordinate system designated as Despun Spacecraft Coordinates , or DSC.  This is a coordinate system for a rotating spacecraft that is in an orbit near the Earth.  DSC is defined by the spacecraft's spin plane and spin axis. However, as the Despun part of the name suggests, the coordinate axes do not participate of the spacecraft's rotation. The X and Y axes are on the spacecraft's spin plane; the Z axis is along the spacecraft's spin axis.  The positive X, Y, and Z axes form an orthogonal, right-handed coordinate system.  The positive Z axis points in the same direction as the spacecraft's angular momentum (or spin or attitude) vector.  The positive X axis points in the direction on the spin plane that is closest to the direction towards the Sun.  In other words, the positive X axis points in the direction of the projection on the spin plane of the vector from the spacecraft to the Sun.  The positive Y axis is determined by the requirement that the DSC system (X, Y, Z) be an orthogonal right-handed system. It follows that the positive Y axis points in the direction on the spin plane that is 90 degrees ahead of the positive X axis (in the sense of the spacecraft's rotation). The electric field data included in these files consists of 2 electric field components on the spin plane.  The original data used is V34L, which typically has a time resolution of about 40 data points per second.  A least-squares spin fit of V34L is performed, and the spin fit coefficients provide the spin plane components of the spin period electric field. Time is a real double-precision quantity.  The units for the time are seconds.  The time is time elapsed since the FAST Mission Epoch, which is May 24, 1968 (1968/05/24) at 00:00:00 UT.  Each time tag indicates the mid-point of the time interval for the corresponding spin period.  Data gaps are not filled; each time tag corresponds to an actual data point.  X, Y, and Z are the 3 components of the attitude vector in the GSE coordinate system (note that all 3 X, Y, and Z components are present, despite the X in the file name). 

SPDF/CDAWeb. Please also acknowledge the data producer: Mozer at UC Berkeley

SPDF/SSCWeb. Please also acknowledge the data producer: Mozer at UC Berkeley

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Mozer at UC Berkeley

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/efi/efi_10minatt/1996/po_10minatt_efi_19960316_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

Electric Field Instrument (from all.xml/instrument/description/@short)

10 minute spacecraft attitude data (from Master/CDFglobalAttributes/Data_type)

Important Warning: The data described below is meant for archival purposes.  It should not be considered as highly accurate data.  For example, accurate data requires a correction in the form of an offset to the Sunward component of the electric field.  A constant offset of 1.2 mV/m has been used for all the data, this being an approximate average value.  In fact, however, the offset varies with time, and must be determined by analysis of the particular time of interest.  Users of this data desiring more information should get in touch with Dr. Forrest Mozer, at the Space Sciences Laboratory, University of California, Berkeley.The electric field data is at spin period time resolution. This means that there is 1 data point about every 6 seconds. However, it should be noted that there can be longer intervals between data points, due to missing data.  Data gaps are not filled in.The components of the electric field are given in a coordinate system designated as Despun Spacecraft Coordinates , or DSC.  This is a coordinate system for a rotating spacecraft that is in an orbit near the Earth.  DSC is defined by the spacecraft's spin plane and spin axis. However, as the Despun part of the name suggests, the coordinate axes do not participate of the spacecraft's rotation. The X and Y axes are on the spacecraft's spin plane; the Z axis is along the spacecraft's spin axis.  The positive X, Y, and Z axes form an orthogonal, right-handed coordinate system.  The positive Z axis points in the same direction as the spacecraft's angular momentum (or spin or attitude) vector.  The positive X axis points in the direction on the spin plane that is closest to the direction towards the Sun.  In other words, the positive X axis points in the direction of the projection on the spin plane of the vector from the spacecraft to the Sun.  The positive Y axis is determined by the requirement that the DSC system (X, Y, Z) be an orthogonal right-handed system. It follows that the positive Y axis points in the direction on the spin plane that is 90 degrees ahead of the positive X axis (in the sense of the spacecraft's rotation). The electric field data included in these files consists of 2 electric field components on the spin plane.  The original data used is V34L, which typically has a time resolution of about 40 data points per second.  A least-squares spin fit of V34L is performed, and the spin fit coefficients provide the spin plane components of the spin period electric field. Time is a real double-precision quantity.  The units for the time are seconds.  The time is time elapsed since the FAST Mission Epoch, which is May 24, 1968 (1968/05/24) at 00:00:00 UT.  Each time tag indicates the mid-point of the time interval for the corresponding spin period.  Data gaps are not filled; each time tag corresponds to an actual data point.  E_X and E_Y are the X and Y components of the electric field in the DSC coordinate system (note that both the X and the Y component are present, despite the X in the file name).  E_X and E_Y are real single-precision quantities. The units for the electric field components are mV/m.  There are no missing data values; each data point value corresponds to an actual data point. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/efi/efi_6secedsc/1996/po_6secEdsc_efi_19960316_v01.cdf. The most common cadence, 5978 [ms] = PT5.978S, occurred for 65.5579% of the 9441 timesteps. 

6 second Electric Field components Despun Spacecraft Coordinates (DSC) (from Master/CDFglobalAttributes/Data_type)

Important Warning: The data described below is meant for archival purposes.  It should not be considered as highly accurate data.  For example, accurate data requires a correction in the form of an offset to the Sunward component of the electric field.  A constant offset of 1.2 mV/m has been used for all the data, this being an approximate average value.  In fact, however, the offset varies with time, and must be determined by analysis of the particular time of interest.  Users of this data desiring more information should get in touch with Dr. Forrest Mozer, at the Space Sciences Laboratory, University of California, Berkeley.The electric field data is at spin period time resolution. This means that there is 1 data point about every 6 seconds. However, it should be noted that there can be longer intervals between data points, due to missing data.  Data gaps are not filled in.The components of the electric field are given in a coordinate system designated as Despun Spacecraft Coordinates , or DSC.  This is a coordinate system for a rotating spacecraft that is in an orbit near the Earth.  DSC is defined by the spacecraft's spin plane and spin axis. However, as the Despun part of the name suggests, the coordinate axes do not participate of the spacecraft's rotation. The X and Y axes are on the spacecraft's spin plane; the Z axis is along the spacecraft's spin axis.  The positive X, Y, and Z axes form an orthogonal, right-handed coordinate system.  The positive Z axis points in the same direction as the spacecraft's angular momentum (or spin or attitude) vector.  The positive X axis points in the direction on the spin plane that is closest to the direction towards the Sun.  In other words, the positive X axis points in the direction of the projection on the spin plane of the vector from the spacecraft to the Sun.  The positive Y axis is determined by the requirement that the DSC system (X, Y, Z) be an orthogonal right-handed system. It follows that the positive Y axis points in the direction on the spin plane that is 90 degrees ahead of the positive X axis (in the sense of the spacecraft's rotation). The electric field data included in these files consists of 2 electric field components on the spin plane.  The original data used is V34L, which typically has a time resolution of about 40 data points per second.  A least-squares spin fit of V34L is performed, and the spin fit coefficients provide the spin plane components of the spin period electric field. Time is a real double-precision quantity.  The units for the time are seconds.  The time is time elapsed since the FAST Mission Epoch, which is May 24, 1968 (1968/05/24) at 00:00:00 UT.  Each time tag indicates the mid-point of the time interval for the corresponding spin period.  Data gaps are not filled; each time tag corresponds to an actual data point.  The original data used is V1L, V2L, etc., which typically have a time resolution of about 1 data point per 0.4 seconds. The spacecraft potentials come from spin period averages of the voltages V1L, V2L, etc.  The spacecraft potential S_C_Pot12 is defined as follows: S_C_Pot12 = (V1 + V2) / 2  The spacecraft potential S_C_Pot34 is defined analogously.  V1, V2, etc. stand for V1L, V2L, etc., respectively.  One additional spacecraft potential, S_C_Pot1234, is defined as follows: S_C_Pot1234 = (S_C_Pot12 + S_C_Pot34) / 2The plasma density n is obtained as a function of the spacecraft potential. The function is a power function, provided by Dr. Jack Scudder (University of Iowa).  It comes from a fit to the POLAR Hydra particle data.  The function was determined using data for 2001/04/01. The validity of the function for dates far from the date above has not been checked.  Values above 75 are regarded as unphysical and re-assigned a NULL value. n will be in units of cm^(-3), i.e., number of charges per cubic centimeter. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/efi/efi_6secpotldens/1996/po_6secpotldens_efi_19960316_v01.cdf. The most common cadence, 5978 [ms] = PT5.978S, occurred for 65.5897% of the 9460 timesteps. 

6 second Spacecraft potential/plasma density (from Master/CDFglobalAttributes/Data_type)

Polar Satellite Attitude and Orbit Information, Archived Website. Disclaimer: The following material is being kept online for archival purposes. Although accurate at the Time Of publication, it is no longer being updated. The Page may contain Broken Links or outdated Information, and parts may not function in Current Web Browsers.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/orbit/def_at/1996/po_at_def_19960224_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

POLAR PLASMA LABORATORY (from all.xml/observatory/description/@short)

POLAR PLASMA LABORATORY (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/orbit/pre_at/1996/po_at_pre_19960308_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

Instrument functional description:   The VIS is a set of three low-light-level cameras.  Two of these   cameras share primary and some secondary optics and are designed to   provide images of the nighttime auroral oval at visible wavelengths.   A third camera is used to monitor the directions of the fields-of-view   of the auroral cameras with respect to the sunlit Earth and return   global images of the auroral oval at ultraviolet wavelengths.  The   VIS instrumentation produces an auroral image of 256 x 256 pixels   approximately every 24 seconds dependent on the integration time and   filter selected.  The fields-of-view of the two nighttime auroral   cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and   medium resolution cameras, respectively.  One or more Earth camera   images of 256 x 256 pixels are produced every five minutes, depending   on the commanded mode.  The field-of-view of the Earth camera is   approximately 20 x 20 degrees. Reference:   Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan,       M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller,       'The Visible Imaging System (VIS) for the Polar Spacecraft',       Space Science Review, vol. 71, pp. 297-328, 1995. [Note to first-time users:  The first four variables are of primaryinterest.  The displayable 256 x 256 image array is in variable 3.  Thecorrect orien- tation of a displayed image is explained in thedescription of variable 3 below.] Data set description:   The VIS Earth camera data set comprises all Earth camera images forthe selected time period.  EJ-ER type files have images that have beenprocessed to remove the effects of penetrating radiation.  In addition,the images have been flat-fielded and fixed pattern noise has beenremoved.  Image pixels are median filtered with the images immediatelybefore and after in time.  The displayable image counts are in variable3.  Some coordinate information is included for viewer orientation.Coordinates are calculated for a grid of 18 x 18 points corresponding toone pixel out of every 15 x 15 pixel block.  In addition, a rotationmatrix and a table of distortion-correcting look direction unit vectorsare provided for the purpose of calculating coordinates for every pixel.See the description of variables 14 and 15 below.  To facilitate viewingof the images, a mapping of pixel value to a recommended color tablebased on the characteristics of the selected filter will be included witheach image.  See the description of variables 19, 20, and 21 below.  Arelative intensity scale is provided by the uncompressed count table ofvariable 24.  Approximate intensity levels in kiloRayleighs are given inthe intensity table of variable 25.  Information on the availability ofmore precisely calibrated intensities can be found on the VIS website atURL http://eiger.physics.uiowa.edu/~vis/software/. Variable descriptions:    1,2. Center time       The time assigned to an image is the center time of the integration       period within a resolution of 50 milliseconds.    3. Image counts       Image pixel counts range from 0 to 255.  They are stored in a two-       dimensional 256 x 256 byte array.  Images from the Earth camera       (sensor 0) are conventionally displayed with row 1 at the top, row 256       at the bottom, column 1 on the left, and column 256 on the right.  The       conventional image display for the low resolution camera (sensor 1) is       rotated 180 degrees so that the row 1-column 1 pixel is at the lower       right corner and the row 256-column 256 pixel is at the upper left       corner.  When displayed in this manner, the spacecraft spin axis is       oriented to the right in the display, the X component is defined as       the center of the image look direction, and the Y component is the   4. Sensor number        0 = Earth camera,       1 = low resolution camera,       2 = medium resolution camera.    5. Half integration time       This is half the length of the integration period for the image,       measured in milliseconds.    6. Filter       Twelve filters are available for visible imaging; the filter number,       1-12, is given here.  Ultra-violet imaging is done with one filter       only, designated here as filter number 0.  In addition, the peak       wavelength in Angstroms is given for the selected filter.    7. Presumed altitude of emissions       The presumed altitude of the emissions seen in the image varies       with the characteristics of the filter used.    8. Platform pitch angle       This is the platform pointing angle of rotation around the spin       axis, measured from nadir.  9,10. Geographic coordinates       Geographic north latitude and east longitude are provided for the       pixels at these image array locations: every 15th row starting       with row 1 and ending with row 256, and every 15th column starting       with column 1 and ending with column 256, for a total of       18 x 18 coordinate pairs. 11,12. Spacecraft position and velocity vectors, GCI       The spacecraft position vector and velocity vector in GCI       coordinates are for the image center time as given in variables       1 and 2.   13. Spacecraft spin axis unit vector, GCI 14,15. Image-to-GCI rotation matrix and look direction vector table       The rotation matrix may be used with the look direction vector table to       obtain pointing vectors in GCI coordinates for each pixel.  The       resulting vectors may be used to calculate coordinates for the observed       positions of the pixels.  Software for this purpose is available at URL       http://eiger.physics.uiowa.edu/~vis/software/.  The general method       used is described below.        In the image coordinate system, the X axis is the center line-of-sight       or look direction; the Y axis is the cross product of the spin axis an       the X axis; and the Z axis is the cross product of the X axis and the       Y axis.  When the display orientation conventions in the variable 3       description are applied, the low resolution camera image is rotated so       that both Earth camera and low resolution camera images are displayed       with Y axis pointing up and Z axis pointing toward the right.        To obtain the coordinates of the observed position of a pixel,       calculate the intersection of the line-of-sight with the surface       of an oblately spheroidal Earth at the altitude given as       variable 7.  The equation of the spheroid is           X**2/(A+ALT)**2 + Y**2/(A+ALT)**2 + Z**2/(B+ALT)**2 = 1           where A is the Earth radius at the equator,                 B is the Earth radius at the pole, and                 ALT is the given altitude.       The line-of-sight equations are           (X-SCX)/DX = (Y-SCY)/DY = (Z-SCZ)/DZ           where (SCX,SCY,SCZ) is the spacecraft position vector GCI, and                   (DX,DY,DZ)  is the look direction unit vector GCI.       Solve the line-of-sight equations for two variables in terms       of the third; substitute into the spheroid equation; and use the       quadratic formula to solve for the third variable.  Select       the solution point closer to the spacecraft.   16. Zenith angle of center line-of-sight at presumed altitude       This is the angle between the geocentric vector through the       observed point, assuming the altitude given as variable 7,       and the reverse of the image center line-of-sight vector.   17. Sun position unit vector, GCI   18. Solar zenith angle at observed point of center line-of-sight       This is the angle of the sun from zenith at the observed point       of the center line-of-sight, assuming the altitude given as       variable 7.   19. RGB color table       This is the recommended color table to be used with the       limits given in variables 20 and 21. 20,21. Low and high color mapping limits       The low and high color limits are recommended for remapping       the color table entries, as follows:           For pixel values less than the low limit, use the color               at table position 1.       assignments:               and less than or equal to the high limit, use the color               at table position (pix-low)/(high-low) x 255 + 1.           For pixel values greater than the high limit, use the color               at table position 256.   22. Data quality flag       The data quality word has bits set to 1 when the listed       conditions are true.  Bit #31 is the most significant bit in the       word, and it will not be used as a flag.  These are the bit           bit 0 - image data frame sync error           bit 1 - image data frame counters error           bit 2 - image data fill frame flag.   23. Post gap flag       The post gap flag has these possible values:           0 - no gap occurred immediately prior to this record,           1 - the gap occurred because the instrument was not in                 a mode that allowed for the production of images for the                 selected sensor,           2 - the gap occurred because level zero data were missing,           3 - the gap occurred because level zero data were too                 noisy to extract images.   24. Expanded count table       The image pixel counts are quasi-logarithmically compressed to the       range 0-255.  This table gives the average of the uncompressed range       for each compressed count value.  Table entries 1-256 correspond to       compressed counts 0-255 respectively.   25. Intensity table       Approximate intensity levels in kiloRayleighs are given for each       compressed count value.  Table entries 1-256 correspond to compressed       counts 0-255 respectively.  Information on the availability of more       precisely calibrated intensities can be found on the VIS website at       URL http://eiger.physics.uiowa.edu/~vis/software/. Supporting software:   Supporting software is available on the VIS website at the URL   http://eiger.physics.uiowa.edu/~vis/software/.  Included is an IDL   program that displays the images with the recommended color bar and   provides approximate intensities and coordinate data for each pixel.

VIS Summary PNG Collection (combined Visible and Earth Camera images at U. Iowa

SPDF/CDAWeb. Please also acknowledge the data producer: Louis A. Frank at The University of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: Louis A. Frank at The University of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Louis A. Frank at The University of Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/vis/vis_ej/1996/po_ej_vis_19960526_v02.cdf. The most common cadence, 53550 [ms] = PT53.55S, occurred for 26.3309% of the 366 timesteps. 

Visible Imaging System (from all.xml/instrument/description/@short)

Earth Camera Images, processed (from Master/CDFglobalAttributes/Data_type)

Presumed emission altitude (also quickly shows times when images are available). 

Earth Camera UV Images (quasi-log cnts), small format display with click-expand (~1 min. res.)

 --> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)

 --> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat

Earth Camera UV Images (kRay), small format display with click-expand (~1 min. res.)

 --> Larger format display with click-expand, no geographic registration.

(USE SHORT TIME SPANS) Movie display of images, no geographic registration.

SPDF/CDAWeb. Please also acknowledge the data producer: R. Friedel at Lanl

SPDF/SSCWeb. Please also acknowledge the data producer: R. Friedel at Lanl

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Friedel at Lanl

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/cammice/cam_h0/1996/po_h0_cam_19960318_v01.cdf. The most common cadence, 203283 [ms] = PT3M23.283S, occurred for 9.2857% of the 39 timesteps. 

Charge And Mass Magnetospheric Ion Composition (from all.xml/instrument/description/@short)

Ion Fluxes at 32-Spin/3-Minute Resolution (from Master/CDFglobalAttributes/Data_type)

Ion (mainly H+) flux (from DC rate) at 25 energies 1-200 keV/Q, 32-spin/3-minute averages

H+ Flux (usually)at 19 energies 5-200 keV/Q, 32-spin/3-minute averages

He+ flux (usually) at 14 energies 20-200 keV/Q, 32-spin/3-minute averages

He+2 flux (usually) at 24 energies 1-200 keV/Q, 32-spin/3-minute averages

O<+3 flux (usually) at 12 energies 35-200 keV/Q, 32-spin/3-minute averages

O>+2 flux (usually) at 19 energies 1.5-100 keV/Q, 32-spin/3-minute averages

Reference: HYDRA is a 3-Dimensional Electron and Ion Hot Plasma Instrumentfor the Polar Spacecraft of the GGS Mission, J. Scudder et al., Space Sci. Rev., 71,459-495, Feb. 1995. http://www-st.physics.uiowa.edu This data set contains the differential electron and proton omnidirectional fluxes per unit solid angle vs energy, at 13.8-second resolution.  Multiply the given value by 4 pi to obtain the total omnidirectional differential energy flux.There are 29 energy channels from 12.5 ev to 18.3 keV.HYDRA is composed of two boxes, each housing 6 detectors.A separate stepping power supply is used for each box.The values of these steps are designed to be interlaced.Therefore, the energies designated in this file are interpolated between the values of the two power supplies.Stepping modes may also vary the number and range of steps during the mission.  To accommodate these changes an interpolation is done from the steps for a particular mode to the common energy values listed in ENERGY_ELE and ENERGY_ION.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/hydra/hyd_h0/1996/po_h0_hyd_19960320_v01.cdf. The most common cadence, 13800 [ms] = PT13.8S, occurred for 75.4874% of the 4724 timesteps. 

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduNote:..The electron cyclotron frequencies are derived from the following:  Fce = 0.028 kHz*B, where B is the magnitude of the ambient magnetic field measured in nT.  All frequencies are converted to Hz.There are 20 MCA E frequency bands, logarithmically spaced and 14 MCA B frequency bands, logarithmically spaced.

A Polar PWI page is maintained at the University of Iowa with descriptions of interpretation issues, user's guides, data availability tables, a form for creating summary plots and access to pregenerated dynamic spectrograms.

SPDF/CDAWeb. Please also acknowledge the data producer: D. Gurnett at U. Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: D. Gurnett at U. Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Gurnett at U. Iowa

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => EpochB.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => EpochB.)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h0/1996/po_h0_pwi_19960325_v02.cdf. The most common cadence, 1325 [ms] = PT1.325S, occurred for 71.4284% of the 46927 timesteps. 

Counts based on variable 'EpochB' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h0/1996/po_h0_pwi_19960325_v02.cdf. The most common cadence, 1325 [ms] = PT1.325S, occurred for 71.4284% of the 46927 timesteps. 

Polar TIDE H+,O+,He+ High Time Resolution Data (before 10/01/96) 

TIDE data for dates 28-Mar-1996 to 30-Sep-1996 are mass resolved. TIDE data between 01-Oct-1996 and 07-Dec-1996 are not valid.

SPDF/CDAWeb. Please also acknowledge the data producer: Thomas E. Moore at Goddard Space Flight Center

SPDF/SSCWeb. Please also acknowledge the data producer: Thomas E. Moore at Goddard Space Flight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Thomas E. Moore at Goddard Space Flight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/tide/tide_h0/1996/po_h0_tid_19960327_v04.cdf. The most common cadence, 5980 [ms] = PT5.98S, occurred for 63.1523% of the 8943 timesteps. 

Thermal Ion Dynamics Experiment (from all.xml/instrument/description/@short)

H+ Ion Plasma Velocity, Field Aligned, available before 01-Oct-1996

H+ Ion Temperature, Parallel and Perendicular to the Magnetic Field, available before 01-Oct-1996.

O+ Ion Plasma Velocity, Field Aligned, available before 01-Oct-1996

O+ Ion Temperature, Parallel and Perendicular to the Magnetic Field, available before 01-Oct-1996.

He+ Ion Plasma Velocity, Field Aligned, available before 01-Oct-1996

He+ Ion Temperature, Parallel and Perendicular to Magnetic Field, available before 01-Oct-1996.

He+ Polar Angle Spectrogram.  Only available before 01-Oct-1996.

Polar Toroidal Imaging Mass-Angle Spectrograph, High Time Resolution data

H+, O+, He+ and He++ number fluxes and statistical uncertainties processed by  the TIMAS science team.  Data acquired   with various anglular and energy resolutions are combined here.  Data Quality and other indicators are provided  to allow selection of high  resolution data (PA_status(ion)=0 and   Energy_status(ion)=0 )  and   High Quality data (Quality=0).  See the VAR_NOTES for the following   variables for more detailed information.  Quality, PA_status, Energy_status Bcr, Fec, Even_odd,  Energy_Range_ID and Spins. A PAPCO module exists that reads and displays these data and data From other POLAR instruments.  Seehttp://www.mpae.gwdg.de/mpae_projects/CCR/software/papco/papco.html and the pointer to a description of the TIMAS PAPCO module on the TIMAS home page.Reference:E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.ftp://sierra.spasci.com/DATA/timas/TIMAS_description.html

access via PAPCO modules and appropriate use of high-resolution (H0) data

A PAPCO module for reading and displaying TIMAS (and other POLAR) data.

PaPCo is IDL software for data visualization and analysis. It is modular, PaPCo modules built by various institutions and individuals plug into PaPCo core to provide data products. These modules provide graphic panels that are stacked on a time axis. About 60 modules exist, and 30 are supported as core modules that come with PaPCo. There are modules from 15+ spacecraft, including CRRES, Polar, Cassini and Cluster. Data from CDAWeb is plottable as well. The software is open-source, making it very flexible and well-suited for science use.

SPDF/CDAWeb. Please also acknowledge the data producer: W.K. Peterson at Lockheed Martin

SPDF/SSCWeb. Please also acknowledge the data producer: W.K. Peterson at Lockheed Martin

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: W.K. Peterson at Lockheed Martin

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_H, @1 => Epoch_O, @2 => Epoch_He_1, @3 => Epoch_He_2.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_H, @1 => Epoch_O, @2 => Epoch_He_1, @3 => Epoch_He_2.)

Toroidal Imaging Mass-Angle Spectrograph (from all.xml/instrument/description/@short)

NSSDC standard-reference time value at the center of the accumulation interval.

H+ number flux for 28 energy and 3 selected angle bins - quality flag applied.

Counts based on variable 'Epoch_H' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/timas/timas_h0/1996/po_h0_tim_19960317_v03.cdf. The most common cadence, 11957 [ms] = PT11.957S, occurred for 61.0376% of the 3459 timesteps. 

H+ number flux for 6 selected energies and 12 angle bins - quality flag applied.

[DO NOT USE] H+ number flux for all energies and all angle bins - quality flag applied.

% Sigma for H+ number flux for 28 energies and 3 selected angle bins - quality flag applied

% Sigma for H+ number flux for 6 selected energies and 12 angle bins - quality flag applied.

Energy Range Identification:  0: Full energy range;  1: Reduced energy range;  2: Low energy range

Pitch Angle Resolution Flags (0=best; >3=smeared PAs; 99=invalid PAs with omnidirec flux in 0-15 deg)

Quality flags for H+, O+, He+, He++ (values 0,1,2=good; 3=adequate; >3 bad/do not use)

O+ number flux for 28 energy and 3 selected angle bins - quality flag applied.

Counts based on variable 'Epoch_O' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/timas/timas_h0/1996/po_h0_tim_19960317_v03.cdf. The most common cadence, 11957 [ms] = PT11.957S, occurred for 61.1788% of the 3467 timesteps. 

O+ number flux for 6 selected energies and 12 angle bins - quality flag applied.

% Sigma for O+ number flux for 28 energies and 3 selected angle bins - quality flag applied.

% Sigma for O+ number flux for 6 selected energies and 12 angle bins  - quality flag applied.

He+ number flux for 28 energies and 3 selected angle bins - quality flag applied.

Counts based on variable 'Epoch_He_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/timas/timas_h0/1996/po_h0_tim_19960317_v03.cdf. The most common cadence, 10 [ms] = PT0.01S, occurred for 34.0039% of the 1927 timesteps. 

He+ number flux for 6 selected energies and 12 angle bins  - quality flag applied.

% Sigma for He+ number flux for 28 energies and 3 selected angle bins - quality flag applied.

% Sigma for He+ number flux for 6 selected energies and 12 angle bins - quality flag applied

He++ number flux for 28 energies and 3 selected angle bins - quality flag applied.

Counts based on variable 'Epoch_He_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/timas/timas_h0/1996/po_h0_tim_19960317_v03.cdf. The most common cadence, 11957 [ms] = PT11.957S, occurred for 58.2848% of the 3303 timesteps. 

He++ number flux for for 28 energy and 12 angle bins - quality flag applied.

% Sigma for He++ number flux for 28 energy and 3 angle bins - quality flag applied.

% Sigma for He++ number flux for 6 selected energies and 12 angle bins - quality flag applied. 

References --------------------1. M. R. Torr, et al., A far ultraviolet imager for the International Solar-Terrestrial Physics mission, Space Sci. Rev., v71, pp329 - 383, 1995Notes ------------------------ 1. The UVI field of view is circular with an 8 degree full width.  The circular image is stored in IMAGE_DATA as a rectangular array of 228 rows and 200 columns.2.  Time information is contained in EPOCH, Time_PB5, IMG_MINUS_MSEC, and IMG_PLUS_MSEC.  3. Pointing information is given in GCI_LOOK_DIR, GEODETIC_LAT, and GEODETIC_LONG. 

SPDF/CDAWeb. Please also acknowledge the data producer: G. Parks at U. Washington

SPDF/SSCWeb. Please also acknowledge the data producer: G. Parks at U. Washington

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Parks at U. Washington

Key Parameter (segment 0) (from Master/CDFglobalAttributes/Data_type)

Polar Plasma Wave Instrument, Step Frequency Receivers A & B, ~2 sec resolution fields

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduThere are 224 SFR frequency bands, logarithmically spaced.  When SFR_MODE is Linear, the 448 linear frequency bands are mapped to 224 logarithmic bands.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch4, @1 => Epoch3, @2 => Epoch2, @3 => Epoch, @4 => Epochfc.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch4, @1 => Epoch3, @2 => Epoch2, @3 => Epoch, @4 => Epochfc.)

Counts based on variable 'Epoch4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h1/1996/po_h1_pwi_19960325_v04.cdf. The most common cadence, 4710 [ms] = PT4.71S, occurred for 76.8816% of the 15384 timesteps. 

Counts based on variable 'Epoch3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h1/1996/po_h1_pwi_19960325_v04.cdf. The most common cadence, 16486 [ms] = PT16.486S, occurred for 62.0147% of the 3546 timesteps. 

Counts based on variable 'Epoch2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h1/1996/po_h1_pwi_19960325_v04.cdf. The most common cadence, 32972 [ms] = PT32.972S, occurred for 41.3287% of the 1182 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h1/1996/po_h1_pwi_19960325_v04.cdf. The most common cadence, 65912 [ms] = PT1M5.912S, occurred for 68.1564% of the 976 timesteps. 

Counts based on variable 'Epochfc' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h1/1996/po_h1_pwi_19960325_v04.cdf. The most common cadence, 5980 [ms] = PT5.98S, occurred for 53.9880% of the 7581 timesteps. 

TIDE data after 07-Dec-1996 are non-mass total ion contribution below 411 ev

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/tide/tide_h1/1996/po_h1_tid_19961208_v02.cdf. The most common cadence, 6013 [ms] = PT6.013S, occurred for 81.3201% of the 11680 timesteps. 

Magnetoshperic Science (from Master/CDFglobalAttributes/Discipline)

Total Ion Plasma Velocity, Field Aligned, available after 07-Dec-1996

Total Ion Temperature, Parallel and Perpendicular to the Magnetic Field. Available after 07-Dec-1996

Polar Plasma Wave Instrument, Low Frequency Waveform Receiver, ~0.01 sec resolution fields

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduAn FFT on 256 or 464 values, depending on the snapshot size, was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series.Coordinate System Used:  local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward.  The X- and Z-axes are contained in the north-south plane.The three orthogonal magnetic field components are given in units of nT/Sec rather than nT because the response of the searchcoils across the passband is not flat.  In order to obtain units of nT, the data would need to be digitally filtered to the frequency of interest and then integrated over time.  Integrating over the entire passband could possibly destroy the resolution of the higher frequency components since the low frequency noise, if present, will dominate.Data are bandpass filtered.  The valid range of data in the frequency domain is from 0.5 to 22.5 Hz.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h2/1996/po_h2_pwi_19960325_v04.cdf. The most common cadence, 10 [ms] = PT0.01S, occurred for 99.6095% of the 797385 timesteps. 

LFWR Elec. Field, Antenna Ex (perp & outward in Local-Field-Aligned/LFA coords)

LFWR Elec. Field, Antenna Ey (perp & eastward in Local-Field-Aligned/LFA coords)

LFWR Elec. Field, Antenna Ez (parallel in Local-Field-Aligned/LFA coords)

LFWR Mag. Field, Antenna Bx (perp & outward in Local-Field-Aligned/LFA coords)

LFWR Mag. Field, Antenna By (perp & eastward in Local-Field-Aligned/LFA coords)

LFWR Mag. Field, Antenna Bz (parallel in Local-Field-Aligned/LFA coords)

H+, O+, He+ and He++ upflowing fluxes and statistical .uncertainties processed by . the TIMAS science team..These data were used as in  .preparing the following papers .1: Peterson et al., JGR 2008 .2: Peterson et al., JGR 2006 .3: Lennartson et al. JGR, 2004  .References:.O.W. Lennartsson et al., .Solar wind control of Earth's H+ and O+ outflow .rates in the 15-eV to 33-keV energy range,.J. Geophys. Res., Vol. 109, A12212 10.1029/2004JA010690, 2004..W.K. Peterson et al., .Quiet time solar illumination effects on the fluxes and .characteristic energies of ionospheric outflow, .J. Geophys. Res., 111, A11S05, doi:10.1029/2005JA011596, 2006. .W.K. Peterson et al., .Solar-minimum quiet-time ion energization and outflow in dynamic .boundary related coordinates,  .To appear in J. Geophys. Res., 2008 .E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995..http://lasp.colorado.edu/timas/TIMAS_description.html. .uncertainties processed by . the TIMAS science team..These data were used as in  .preparing the following papers .1: Peterson et al., JGR 2008 .2: Peterson et al., JGR 2006 .3: Lennartson et al. JGR, 2004  .References:.O.W. Lennartsson et al., .Solar wind control of Earth's H+ and O+ outflow .rates in the 15-eV to 33-keV energy range,.J. Geophys. Res., Vol. 109, A12212 10.1029/2004JA010690, 2004..W.K. Peterson et al., .Quiet time solar illumination effects on the fluxes and .characteristic energies of ionospheric outflow, .J. Geophys. Res., 111, A11S05, doi:10.1029/2005JA011596, 2006. .W.K. Peterson et al., .Solar-minimum quiet-time ion energization and outflow in dynamic .boundary related coordinates,  .To appear in J. Geophys. Res., 2008 .E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995..http://lasp.colorado.edu/timas/TIMAS_description.html. .uncertainties processed by . the TIMAS science team..These data were used as in  .preparing the following papers .1: Peterson et al., JGR 2008 .2: Peterson et al., JGR 2006 .3: Lennartson et al. JGR, 2004  .References:.O.W. Lennartsson et al., .Solar wind control of Earth's H+ and O+ outflow .rates in the 15-eV to 33-keV energy range,.J. Geophys. Res., Vol. 109, A12212 10.1029/2004JA010690, 2004..W.K. Peterson et al., .Quiet time solar illumination effects on the fluxes and .characteristic energies of ionospheric outflow, .J. Geophys. Res., 111, A11S05, doi:10.1029/2005JA011596, 2006. .W.K. Peterson et al., .Solar-minimum quiet-time ion energization and outflow in dynamic .boundary related coordinates,  .To appear in J. Geophys. Res., 2008 .E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995..http://lasp.colorado.edu/timas/TIMAS_description.html. .uncertainties processed by . the TIMAS science team..These data were used as in  .preparing the following papers .1: Peterson et al., JGR 2008 .2: Peterson et al., JGR 2006 .3: Lennartson et al. JGR, 2004  .References:.O.W. Lennartsson et al., .Solar wind control of Earth's H+ and O+ outflow .rates in the 15-eV to 33-keV energy range,.J. Geophys. Res., Vol. 109, A12212 10.1029/2004JA010690, 2004..W.K. Peterson et al., .Quiet time solar illumination effects on the fluxes and .characteristic energies of ionospheric outflow, .J. Geophys. Res., 111, A11S05, doi:10.1029/2005JA011596, 2006. .W.K. Peterson et al., .Solar-minimum quiet-time ion energization and outflow in dynamic .boundary related coordinates,  .To appear in J. Geophys. Res., 2008 .E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995..http://lasp.colorado.edu/timas/TIMAS_description.html. .uncertainties processed by . the TIMAS science team..These data were used as in  .preparing the following papers .1: Peterson et al., JGR 2008 .2: Peterson et al., JGR 2006 .3: Lennartson et al. JGR, 2004  .References:.O.W. Lennartsson et al., .Solar wind control of Earth's H+ and O+ outflow .rates in the 15-eV to 33-keV energy range,.J. Geophys. Res., Vol. 109, A12212 10.1029/2004JA010690, 2004..W.K. Peterson et al., .Quiet time solar illumination effects on the fluxes and .characteristic energies of ionospheric outflow, .J. Geophys. Res., 111, A11S05, doi:10.1029/2005JA011596, 2006. .W.K. Peterson et al., .Solar-minimum quiet-time ion energization and outflow in dynamic .boundary related coordinates,  .To appear in J. Geophys. Res., 2008 .E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995..http://lasp.colorado.edu/timas/TIMAS_description.html. uncertainties processed by  the TIMAS science team.These data were used as in  preparing the following papers 1: Peterson et al., JGR 2008 2: Peterson et al., JGR 2006 3: Lennartson et al. JGR, 2004  References:O.W. Lennartsson et al., Solar wind control of Earth's H+ and O+ outflow rates in the 15-eV to 33-keV energy range,J. Geophys. Res., Vol. 109, A12212 10.1029/2004JA010690, 2004.W.K. Peterson et al., Quiet time solar illumination effects on the fluxes and characteristic energies of ionospheric outflow, J. Geophys. Res., 111, A11S05, doi:10.1029/2005JA011596, 2006. W.K. Peterson et al., Solar-minimum quiet-time ion energization and outflow in dynamic boundary related coordinates,  To appear in J. Geophys. Res., 2008 E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.http://lasp.colorado.edu/timas/TIMAS_description.html 

Solar-minimum quiet-time ion energization and outflow in dynamic boundary related coordinates, W.K. Peterson, L. Andersson, B.C. Callahan, H.L. Collin, J.D. Scudder, and A.W. Yau, To appear in J. Geophys. Res., 2008.

Polar/TIMAS Observations of Suprathermal Ion Outflow During Solar Minimum Conditions, W.K. Peterson, H.L. Collin, A.W. Yau, and O.W. Lennartsson, J. Geophys. Res., 106, 6059, 2001.

The Seasonal Variation of Auroral Ion Beams, H.L. Collin, W.K. Peterson, O.W. Lennartsson, and J.F. Drake, Geophysical Research Letters, 25, 4071, 1998.

SPDF/CDAWeb. Please also acknowledge the data producer: W.K. Peterson at LASP/University of Colorado

SPDF/SSCWeb. Please also acknowledge the data producer: W.K. Peterson at LASP/University of Colorado

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: W.K. Peterson at LASP/University of Colorado

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => H_Epoch, @1 => O_Epoch, @2 => He1_Epoch, @3 => He2_Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => H_Epoch, @1 => O_Epoch, @2 => He1_Epoch, @3 => He2_Epoch.)

Time delayed Wind IFM Magnetic Field from WIND in GSM Coordinates

 --> O+ Quality Flag (0 indicates OK, See Var_notes for other codes)

 --> He+ Quality Flag (0 indicates OK, See Var_notes for other codes)

 --> He++ Quality Flag (0 indicates OK, See Var_notes for other codes)

Polar Plasma Wave Instrument, Low-rate High Frequency Waveform Receiver, 16K (6-channel, ~0.00003 sec resolution) fields

A Polar PWI page is maintained at the University of Iowa with descriptions of receivers, interpretation issues, user's guides, and data availability tables.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch0.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch0.)

HFWR16K Time Domain Fields (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h3/1996/po_h3_pwi_19960325_v03.cdf. The most common cadence, 28002 [ns] = PT0.000028002S, occurred for 79.1510% of the 102123 timesteps. 

HFWR 16 kHz Elec Field, Antenna Ex (perp and outward in Local-Field-Aligned/LFA coords)

HFWR 16 kHz Elec Field, Antenna Ey (perp and eastward in Local-Field-Aligned/LFA coords)

HFWR 16 kHz Elec Field, Antenna Ez (parallel in Local-Field-Aligned/LFA coords)

HFWR 16 kHz Mag. Field, Antenna Bx (perp and outward in Local-Field-Aligned/LFA coords)

HFWR 16 kHz Mag. Field, Antenna By (perp and eastward in Local-Field-Aligned/LFA coords)

HFWR 16 kHz Mag. Field, Antenna Bz (parallel in Local-Field-Aligned/LFA coords)

Counts based on variable 'Epoch0' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h3/1996/po_h3_pwi_19960325_v03.cdf. The most common cadence, 128799800000 [ns] = PT2M8.7998S, occurred for 77.4194% of the 48 timesteps. 

Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 2 kHz (6-channel, ~0.0002 sec resolution) fields

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch0, @1 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch0, @1 => Epoch.)

Counts based on variable 'Epoch0' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h4/1996/po_h4_pwi_19960326_v03.cdf. The most common cadence, 128799800000 [ns] = PT2M8.7998S, occurred for 80.0000% of the 20 timesteps. 

HFWR 2 kHz Elec Field Antenna Ex (perp and outward in Local-Field-Aligned/LFA coords)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h4/1996/po_h4_pwi_19960326_v03.cdf. The most common cadence, 224014 [ns] = PT0.000224014S, occurred for 66.3098% of the 35308 timesteps. 

HFWR 2 kHz Elec Field Antenna Ey (perp and eastward in Local-Field-Aligned/LFA coords)

HFWR 2 kHz Elec Field Antenna Ez (parallel in Local-Field-Aligned/LFA coords)

HFWR 2 kHz Mag Field Antenna Bx (perp and outward in Local-Field-Aligned/LFA coords)

HFWR 2 kHz Mag Field Antenna By (perp and eastward in Local-Field-Aligned/LFA coords)

HFWR 2 kHz Mag Field Antenna Bz (parallel in Local-Field-Aligned/LFA coords)

Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 16 kHz/30 usec (interferometry) fields

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduAn FFT on 2048 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series.Data are lowpass filtered so that the data are valid only up to 16 kHz.Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t.

A Polar PWI page is maintained at the University of Iowa with descriptions of receivers, interpretation issues, user's guides, data availability tables, a form for creating summary plots and access to pregenerated dynamic spectrograms.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h5/1996/po_h5_pwi_19960325_v01.cdf. The most common cadence, 45936 [ms] = PT45.936S, occurred for 0.0485% of the 1689 timesteps. 

Counts based on variable 'Epoch0' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h5/1996/po_h5_pwi_19960325_v01.cdf. The most common cadence, 46000 [ms] = PT46S, occurred for 70.2591% of the 1193 timesteps. 

Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 6-channel (~1.5 usec resolution) fields

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduAn FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series.Coordinate System Used:  local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward.  The X- and Z-axes are contained in the north-south plane.Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t.This data comes is in snapshots of 31816 points per channel, every 9.2 seconds, where the duration of each snapshot is 0.045 seconds.  Since Epoch time is in milliseconds, the times for the data points will not be unique unless the Delta_T in milliseconds is added to the Epoch time for the snapshot.The data in this file will be in sets of 31744 (31*1024) points per channel because the FFT size does not come out even within the number of points per snapshot.  To obtain the time for each point in the snapshot, increment each Epoch time after the first with Delta_T (in ms).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h7/1996/po_h7_pwi_1996032615_v02.cdf. The most common cadence, 9200 [ms] = PT9.2S, occurred for 98.5294% of the 67 timesteps. 

[NO LIST] HFWR Elec Field Antenna Ex (perp and outward in Local-Field Aligned/LFA coords)

[NO LIST] HFWR Elec Field Antenna Ey (perp and eastward in Local-Field Aligned/LFA coords)

[NO LIST] HFWR Elec Field Antenna Ez (parallel in Local-Field Aligned/LFA coords)

[NO LIST] HFWR Mag Field Antenna Bx (perp and outward in Local-Field Aligned/LFA coords)

[NO LIST] HFWR Mag Field Antenna By (perp and eastward in Local-Field Aligned/LFA coords)

[NO LIST] HFWR Mag Field Antenna Bz (parallel in Local-Field Aligned/LFA coords)

[NO LIST] Data Quality for Ex components(0 = OK, 1 = clipped or questionable)

[NO LIST] Data Quality for Ey components(0 = OK, 1 = clipped or questionable)

[NO LIST] Data Quality for Ez components(0 = OK, 1 = clipped or questionable)

[NO LIST] Data Quality for Bx components(0 = OK, 1 = clipped or questionable)

[NO LIST] Data Quality for By components(0 = OK, 1 = clipped or questionable)

[NO LIST] Data Quality for Bz components(0 = OK, 1 = clipped or questionable)

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduAn FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series.Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t.Coordinate system used:  antenna coordinate system, where the u-axis is offset by -45 degrees from the spacecraft x-axis, the v-axis is offset by -45 degrees from the spacecraft y-axis, and the z-axis is identical to the spacecraft z-axis.This data comes in snapshots of 190902 points distributed among 2 to 6 channels every 9.2 seconds, where the duration of the snapshot is 0.045 seconds.  Since Epoch time is in milliseconds, the times for the data points will not be unique unless the Delta_T (in milliseconds) is added to  the Epoch time for the snapshot.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h8/1996/po_h8_pwi_1996040400_v01.cdf. The most common cadence, 9200 [ms] = PT9.2S, occurred for all 116 timesteps. 

Number of FFTs of size 1024 that were processed for this snapshot

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduAn FFT on 1992 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series.Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t.Coordinate system used:  antenna coordinate system, where the u-axis is offset by -45 degrees from the spacecraft x-axis, the v-axis is offset by -45 degrees from the spacecraft y-axis, and the z-axis is identical to the spacecraft z-axis.This data comes in snapshots of 1992 or 3984 points every 0.064 seconds.  Duration of a snapshot is less when the instrument is in duty cycle modes.  Since Epoch time is in milliseconds, the times for the data points will not be unique unless the fmsec (fraction of milliseconds) is appended to the Epoch0 time for that point.The frequency filters used for the wideband receiver have a range that limits the calibration.  The following table specifies the range of frequencies for which the calibration is certified.  Outside this range the amplitude values may be in error and should not be used.  (Translation, Filter, Freq Range) (0 kHz, 90 kHz, 7.5 kHz-90.0 kHz) (125 kHz, 90 kHz, 131.9 kHz-214.8 kHz) (250 kHz, 90 kHz, 254.3 kHz-341.2 kHz) (500 kHz, 90 kHz, 504.79 kHz-591.1 kHz) (0 kHz, 10 kHz, 0.035 kHz-11.64 kHz) (0 kHz, 22 kHz, 0.065 kHz-21.59 kHz) (0 kHz, 1-3 kHz, 1.0 kHz-3.0 kHz) (0 kHz, 3-6 kHz, 3.0 kHz-6.0 kHz) 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_h9/1996/po_h9_pwi_1996032510_v01.cdf. The most common cadence, 64 [ms] = PT0.064S, occurred for 99.9715% of the 7015 timesteps. 

Sample rate: the rate at which the data is telemetered to the ground.

Filter Mode: 0-2 = 90 kHz, 3 = 1-3 kHz, 4 = 20 kHz, 5 = 3-6 kHz, 6 = 10-16 kHz, 7 = 10 kHz

Reference: HYDRA is a 3-Dimensional Electron and Ion Hot Plasma Instrument for the Polar Spacecraft of the GGS Mission, J. Scudder et al., Space Sci. Rev., 71,459-495, Feb. 1995. http://www-st.physics.uiowa.edu This data set contains survey electron and proton moments for the energy flux (parallel), at 13.8-second resolution as determined (0-20keV). Higher quality data products may be available from the P.I.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/hydra/energy-flux/1997/po_hyd_energy_flux_19970429_v01.cdf. The most common cadence, 13800 [ms] = PT13.8S, occurred for 99.4881% of the 6219 timesteps. 

~2.3-minute Key Parameters, CAMMICE/Polar Charge And Mass Magnetospheric Ion Composition Experiment

This data set contains 96-second averaged counting rates for H+, He++, (O+, O++ together), (O>2+), all from the MICS part of the instrument, with a +/- 1 degree field of view perpendicular to the spin axis, segmented into bins of size 1/32 of a spin.T.A. Fritz et.al, CAMMICE:The POLAR CAMMICE instrumentsIt also contains 96-second averaged counting rates from two proton channels (0.5-1.7 MeV and 1.7-5.8 MeV), two He channels (1.4-4.3 MeV and 4.3-9.6 MeV), and six CNO channels (5-10, 6-11, 7-13, 17-92, 18-92, 21-92 MeV), from the HIT part of the instrument, with a +/- 6 degree field of view perpendicular to the spin axis, segmented into bins  of 1/32 of a spin.A. Fritz et.al, CAMMICE:The POLAR CAMMICE instruments

SPDF/CDAWeb. Please also acknowledge the data producer: T. A. Fritz at Boston University

SPDF/SSCWeb. Please also acknowledge the data producer: T. A. Fritz at Boston University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. A. Fritz at Boston University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/cammice/cammice_k0/1996/po_k0_cam_19960226_v01.cdf. The most common cadence, 202400 [ms] = PT3M22.4S, occurred for all 9 timesteps. 

Charge and Mass Magnetospheric Ion Composition (from all.xml/instrument/description/@short)

CEPPAD Energetic particles & angular distribution, Key parameters

Data: 96 second averagesJ. B. Blake et.al, Comprehensive Energetic Particle & Pitch Angle Distribution

SPDF/CDAWeb. Please also acknowledge the data producer: J. B.Blake at Aerospace Corp.

SPDF/SSCWeb. Please also acknowledge the data producer: J. B.Blake at Aerospace Corp.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. B.Blake at Aerospace Corp.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/ceppad/ceppad_k0/1996/po_k0_cep_19960226_v01.cdf. The most common cadence, 101200 [ms] = PT1M41.2S, occurred for all 19 timesteps. 

Comprehensive Energetic Particle Pitch Angle (from all.xml/instrument/description/@short)

Reference: DATA FORMAT CONTROL DOCUMENT (DFCD) BETWEEN THE INTERNATIONAL SOLAR-TERRESTRIAL PHYSICS (ISTP) PROGRAM INFORMATION PROCESSING DIVISION (IPD) GROUND DATA PROCESSING SYSTEM AND THE ISTP MISSION INVESTIGATORS SEPTEMBER 1993 Pages 3-57 through 3-60.GGS Instrument papers (DRAFT)December 1992 pages B.2.1 thru B.2.14 inclusive.The Polar Electric Field Instrument KPS will record data from two sets of Langmuir probes.The first set V12, are 130m apart, the second set V34, are 100m apart.

SPDF/CDAWeb. Please also acknowledge the data producer: F. Mozer at UC Berkeley

SPDF/SSCWeb. Please also acknowledge the data producer: F. Mozer at UC Berkeley

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: F. Mozer at UC Berkeley

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/efi/efi_k0/1996/po_k0_efi_19960315_v01.cdf. The most common cadence, 5979 [ms] = PT5.979S, occurred for 87.9370% of the 1786 timesteps. 

Reference: HYDRA is a 3-Dimensional Electron and Ion Hot  plasma Instrument for the Polar Spacecraft of the GGS Mission, J. Scudder et al., Space Sci. Rev., 71, 459-495, Feb. 1995.This data set contains the electron density and average energy, and the maximum and minimum Debye energies, at 1-minute resolution.J. Scudder, et.al, Space Sci. Rev., 71, 459-495, 1995, http://www-st.physics.uiowa.eduJ. Scudder, et.al, Space Sci. Rev., 71, 459-495, 1995, http://www-st.physics.uiowa.edu

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/hydra/hydra_k0/1996/po_k0_hyd_19960320_v04.cdf. The most common cadence, 55200 [ms] = PT55.2S, occurred for 95.0000% of the 494 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: C.T. Russell at UCLA

SPDF/SSCWeb. Please also acknowledge the data producer: C.T. Russell at UCLA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C.T. Russell at UCLA

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch6.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch6.)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/mfe/mfe_k0/1996/po_k0_mfe_19960316_v08.cdf. The most common cadence, 55199 [ms] = PT55.199S, occurred for 32.1611% of the 503 timesteps. 

Dipole tilt angle (deg) using dipole moment of data, scalar (IGRF with secular correction (0.92 min res.)

Observed compressional standard dev. of magnetic field (0.92 min res.)

IGRF95&T95 vector magnetic field in cartesian GSE (0.92 min res.)

IGRF95&T95 vector magnetic field in cartesian GSM (0.92 min res.)

IGRF95&T95 vector magnetic field in cartesian SM (0.92 min res.)

North magnetic footprint, latitude and longitude in cartesian GEO (0.92 min res.)

South magnetic footprint, latitude and longitude in cartesian GEO (0.92 min res.)

Vector sampling interval deviation : dt-120000 (microsec)(0.92 min res.)

Counts based on variable 'Epoch6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/mfe/mfe_k0/1996/po_k0_mfe_19960316_v08.cdf. The most common cadence, 6000 [ms] = PT6S, occurred for all 14399 timesteps. 

Observed vector magnetic field in cartesian S/C coord. (6 sec res.)

INSTRUMENT DESCRIPTION:              The PIXIE instrument remotely images bremsstrahlung X-rays which are emitted from the earth's atmosphere. PIXIE measures the bremsstrahlung X-ray flux in two spatial dimensions and as a function of energy from 2 keV to 60 keV in 64 energy channels.  The spatial resolution and sensitivity of the instrument are a function of orbital altitude.  Sensitivity is optimized by the use of a variable configuration of the instrument's adjustable aperture plate.    Continuous imagery will be provided, since PIXIE is mounted on the despun platform.  Each X-ray photon is identified individually by the time and location at which it is detected within the focal plane. INSTRUMENT REFERENCES:               1.  Instrument Description Document for the Polar Ionospheric X-ray Imaging Experiment (PIXIE) on the ISTP/GGS POLAR Satellite (submitted to Project as a PIXIE deliverable). Document number LMSC F254274 (Lockheed Space and Missiles Co.)                                   2.  McKenzie, D. L., D. J. Gorney, and W. L. Imhof, Auroral X-ray Imaging from High- and Low-Earth Orbit, Proc. SPIE, 1745, 39, 1992.                                   3.  McKenzie, D. L., D. J. Gorney, and W. L. Imhof, Auroral X-ray Imaging from High- and Low-Earth Orbit, Opt. Eng. (to be published in the February 1994 issue).                                   4.  Imhof, W. L., et al., The Polar Ionospheric X-ray Imaging Experiment (PIXIE), Space Science Reviews (to be published as part of a special issue on the GGS instruments). KEY PARAMETERS DESCRIPTION:          The Primary Key Parameter data consists of two 64x64 pixel X-ray image arrays and two Mean Intensity measures. The images and intensities are associated with two variable integrated energy channel ranges.  The Secondary Key Parameter data contains information necessary to the appropriate interpretation of the images.  This information includes geographic and geomagnetic spatial registration references, integrated energy range definitions, data quality flags, and various mode/state indicators.  The spatial references include full pixel maps (providing the value of a particular coordinate, e.g., magnetic latitude, at each of the 4096 pixels) as well as simple pixel markers locating specific features (such as the geographic and geomagnetic poles).

SPDF/CDAWeb. Please also acknowledge the data producer: D. Chenette at Lockheed

SPDF/SSCWeb. Please also acknowledge the data producer: D. Chenette at Lockheed

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Chenette at Lockheed

Polar Ionospheric X-ray Imaging Experiment (from all.xml/instrument/description/@short)

Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.eduNote:..The electron ion and cyclotron frequencies are derived from the following:  Fce = 0.028 kHz*B, where B is the magnitude of the ambient magnetic field measured in nT.  Fcp = Fce/1837 in kHz.  FcO+ = Fcp/16 in kHz.  All frequencies in the key parameters are converted to Hz.Since the SFR frequency steps vary with the mode, the measured SFR frequencies will be mapped to a fixed array of 160 approximately logarithmically spaced frequency values, 32 frequency values for each of the five SFR channels.  In the log mode, the 64 frequency steps of the fourth and fifth frequency channels will be mapped to 32 frequency steps each, using geometric averaging.  In the linear mode, the 448 linearly spaced frequency steps of the five frequency channels will be mapped to the fixed array of 160 logarithmically spaced frequency values using a windowing technique.  The magnetic and electric field values corresponding to each SFR frequency step will be similarly mapped to 160-point fixed arrays corresponding to the mapped frequency array.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/pwi/pwi_k0/1996/po_k0_pwi_19960227_v02.cdf. The most common cadence, 299000 [ms] = PT4M59S, occurred for 99.2857% of the 139 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/orbit/spha_k0/1996/po_k0_spha_19960125_v01.cdf. The most common cadence, 55200 [ms] = PT55.2S, occurred for 99.5620% of the 682 timesteps. 

Quality indicator (also quickly shows times when images are available)

Far UV Images (kRay), small format display with click-expand (~10 min res)

 --> (USE SHORT TIME SPANS) Azimuthal projection to geographic (with fixed sun orientation)

 --> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat, using eccentric dipole model

 --> (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (with fixed sun orientation)

 --> (USE SHORT TIME SPAN) Movie, azimuthal projection to magnetic LT and invariant lat, using eccentric dipole model

 Instrument functional description:    The VIS is a set of three low-light-level cameras.  Two of these    cameras share primary and some secondary optics and are designed to    provide images of the nighttime auroral oval at visible wavelengths.    A third camera is used to monitor the directions of the fields-of-view    of the auroral cameras with respect to the sunlit Earth and return    global images of the auroral oval at ultraviolet wavelengths.  The    VIS instrumentation produces an auroral image of 256 x 256 pixels    approximately every 24 seconds dependent on the integration time and    filter selected.  The fields-of-view of the two nighttime auroral    cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and    medium resolution cameras, respectively.  One or more Earth camera    images of 256 x 256 pixels are produced every five minutes, depending    on the commanded mode.  The field-of-view of the Earth camera is    approximately 20 x 20 degrees.  Reference:    Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan,        M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller,        'The Visible Imaging System (VIS) for the Polar Spacecraft',        Space Science Review, vol. 71, pp. 297-328, 1995. [Note to first-time users:  The first four variables are of primary interest.    The displayable 256 x 256 image array is in variable 3.  The correct orien-    tation of a displayed image is explained in the description of variable 3    below.]  Data set description:         The VIS key parameter data set is a survey of auroral activity    provided by a series of single images showing a significant area of the    auroral zone.  The displayable image counts are in variable 3.         Some coordinate information is included for viewer orientation.    Coordinates are calculated for a grid of 18 x 18 points corresponding    to one pixel out of every 15 x 15 pixel block.  In addition, a rotation    matrix and a table of distortion-correcting look direction unit vectors    are provided for the purpose of calculating coordinates for every pixel.    See the description of variables 17 and 18 below.         To facilitate viewing of the images, a mapping of pixel value to a    recommended color table based on the characteristics of the selected    filter will be included with each image.  See the description of variables    22, 23, and 24 below.         A relative intensity scale is provided by the uncompressed count table    of variable 27.  Approximate intensity levels in kiloRayleighs are given in    the intensity table of variable 28.  Information on the availability of    more precisely calibrated intensities can be found on the VIS website at    URL http://eiger.physics.uiowa.edu/~vis/software/.  Variable descriptions:     1,2. Center time        The time assigned to an image is the center time of the integration        period within a resolution of 50 milliseconds.     3. Image counts        Image pixel counts range from 0 to 255.  They are stored in a two-        dimensional 256 x 256 byte array.  Images from the Earth camera        (sensor 0) are conventionally displayed with row 1 at the top, row 256        at the bottom, column 1 on the left, and column 256 on the right.  The        conventional image display for the low resolution camera (sensor 1) is        rotated 180 degrees so that the row 1-column 1 pixel is at the lower        right corner and the row 256-column 256 pixel is at the upper left        corner.  When displayed in this manner, the spacecraft spin axis is        oriented to the right in the display, the X component is defined as        the center of the image look direction, and the Y component is the        cross product of the spin axis and the look direction.     4. Sensor number        0 = Earth camera,        1 = low resolution camera,        2 = medium resolution camera.     5. Half integration time        This is half the length of the integration period for the image,        measured in milliseconds.     6. Filter        Twelve filters are available for visible imaging; the filter number,        1-12, is given here.  Ultra-violet imaging is done with one filter only,        designated here as filter number 0.  In addition, the peak wavelength        in Angstroms is given for the selected filter.     7. Presumed altitude of emissions        The presumed altitude of the emissions seen in the image varies        with the characteristics of the filter used.     8. Field stop position        The field stop may partially occlude the field of view of the low        or medium resolution cameras.  The position is given in 1.5 degree        steps.     9. Platform pitch angle        This is the platform pointing angle of rotation around the spin        axis, measured from nadir.  10,11. Mirror elevation and azimuth angles        For the low or medium resolution camera, the two-axis mirror        position is given in steps measured from the instrument calibration        switches.  The boresight of the instrument is located at step 68 in        azimuth and step 118 in elevation.  12,13. Geographic coordinates        Geographic north latitude and east longitude are provided for the        pixels at these image array locations: every 15th row starting        with row 1 and ending with row 256, and every 15th column starting        with column 1 and ending with column 256, for a total of        18 x 18 coordinate pairs.  14,15. Spacecraft position and velocity vectors, GCI        The spacecraft position vector and velocity vector in GCI        coordinates are for the image center time as given in variables        1 and 2.    16. Spacecraft spin axis unit vector, GCI  17,18. Image-to-GCI rotation matrix and look direction vector table        The rotation matrix may be used with the look direction vector table to        obtain pointing vectors in GCI coordinates for each pixel.  The        resulting vectors may be used to calculate coordinates for the observed        positions of the pixels.  Software for this purpose is available at URL         http://eiger.physics.uiowa.edu/~vis/software/.  The general method         used is described below.         In the image coordinate system, the X axis is the center line-of-sight        or look direction; the Y axis is the cross product of the spin axis an        the X axis; and the Z axis is the cross product of the X axis and the        Y axis.  When the display orientation conventions in the variable 3        description are applied, the low resolution camera image is rotated so        that both Earth camera and low resolution camera images are displayed        with Y axis pointing up and Z axis pointing toward the right.         To obtain the coordinates of the observed position of a pixel,        calculate the intersection of the line-of-sight with the surface        of an oblately spheroidal Earth at the altitude given as        variable 7.  The equation of the spheroid is            X**2/(A+ALT)**2 + Y**2/(A+ALT)**2 + Z**2/(B+ALT)**2 = 1            where A is the Earth radius at the equator,                  B is the Earth radius at the pole, and                  ALT is the given altitude.        The line-of-sight equations are            (X-SCX)/DX = (Y-SCY)/DY = (Z-SCZ)/DZ            where (SCX,SCY,SCZ) is the spacecraft position vector GCI, and                    (DX,DY,DZ)  is the look direction unit vector GCI.        Solve the line-of-sight equations for two variables in terms        of the third; substitute into the spheroid equation; and use the        quadratic formula to solve for the third variable.  Select        the solution point closer to the spacecraft.    19. Zenith angle of center line-of-sight at presumed altitude        This is the angle between the geocentric vector through the        observed point, assuming the altitude given as variable 7,        and the reverse of the image center line-of-sight vector.    20. Sun position unit vector, GCI    21. Solar zenith angle at observed point of center line-of-sight        This is the angle of the sun from zenith at the observed point        of the center line-of-sight, assuming the altitude given as        variable 7.    22. RGB color table        This is the recommended color table to be used with the        limits given in variables 23 and 24.  23,24. Low and high color mapping limits        The low and high color limits are recommended for remapping        the color table entries, as follows:            For pixel values less than the low limit, use the color                at table position 1.            For pixel values greater than or equal to the low limit                and less than or equal to the high limit, use the color                at table position (pix-low)/(high-low) x 255 + 1.            For pixel values greater than the high limit, use the color                at table position 256.    25. Data quality flag        The data quality word has bits set to 1 when the listed        conditions are true.  Bit #31 is the most significant bit in the        word, and it will not be used as a flag.  These are the bit        assignments:            bit 0 - image data frame sync error            bit 1 - image data frame counters error            bit 2 - image data fill frame flag.    26. Post gap flag        The post gap flag has these possible values:            0 - no gap occurred immediately prior to this record,            1 - the gap occurred because the instrument was not in                  a mode that allowed for the production of images for the                  selected sensor,            2 - the gap occurred because level zero data were missing,            3 - the gap occurred because level zero data were too                  noisy to extract images.    27. Expanded count table        The image pixel counts are quasi-logarithmically compressed to the        range 0-255.  This table gives the average of the uncompressed range        for each compressed count value.  Table entries 1-256 correspond to        compressed counts 0-255 respectively.    28. Intensity table        Approximate intensity levels in kiloRayleighs are given for each        compressed count value.  Table entries 1-256 correspond to compressed        counts 0-255 respectively.  Information on the availability of more        precisely calibrated intensities can be found on the VIS website at        URL http://eiger.physics.uiowa.edu/~vis/software/.  Supporting software:    Supporting software is available on the VIS website at the URL    http://eiger.physics.uiowa.edu/~vis/software/.  Included is an IDL program    that displays the images with the recommended color bar and provides    approximate intensities and coordinate data for each pixel.

Visible Key Parameter (from Master/CDFglobalAttributes/Data_type)

Presumed emission altitude (also quickly shows time periods when images are available)

Visible Image (quasi-log cnts), small format display with click-expand (~4 min. res.)

 --> (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (fixed sun orientation)

 --> (USE SHORT TIME SPANS) Movie, azimuthal projection to magnetic LT and invariant lat

Visible Image (kRay), small format display with click-expand (~4 min. res.)

 --> Larger format display with click-expand, no geographic registration

 --> (USE SHORT TIME SPANS) Movie display of images, no geographic registration

Polar Toroidal Imaging Mass-Angle Spectrograph, Supplemental Key Parameters

H+, O+, He+ and He++ number fluxes for survey  purposes only E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.ftp://sierra.spasci.com/DATA/timas/TIMAS_description.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/timas/timas_k1/1999/po_k1_tim_19990607_v01.cdf. The most common cadence, 193000 [ms] = PT3M13S, occurred for 50.1176% of the 213 timesteps. 

 Instrument functional description:    The VIS is a set of three low-light-level cameras.  Two of these    cameras share primary and some secondary optics and are designed to    provide images of the nighttime auroral oval at visible wavelengths.    A third camera is used to monitor the directions of the fields-of-view    of the auroral cameras with respect to the sunlit Earth and return    global images of the auroral oval at ultraviolet wavelengths.  The    VIS instrumentation produces an auroral image of 256 x 256 pixels    approximately every 24 seconds dependent on the integration time and    filter selected.  The fields-of-view of the two nighttime auroral    cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and    medium resolution cameras, respectively.  One or more Earth camera    images of 256 x 256 pixels are produced every five minutes, depending    on the commanded mode.  The field-of-view of the Earth camera is    approximately 20 x 20 degrees.  Reference:    Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan,        M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller,        'The Visible Imaging System (VIS) for the Polar Spacecraft',        Space Science Review, vol. 71, pp. 297-328, 1995. [Note to first-time users:  The first four variables are of primary interest.    The displayable 256 x 256 image array is in variable 3.  The correct orien-    tation of a displayed image is explained in the description of variable 3    below.]  Data set description:         The VIS Earth camera key parameter data set is a survey of global    auroral activity providedby a series of piled images produced by the median-    filtering of up to five consecutive images.  The displayable image counts    are in variable 3.         Some coordinate information is included for viewer orientation.    Coordinates are calculated for a grid of 18 x 18 points corresponding    to one pixel out of every 15 x 15 pixel block.  In addition, a rotation    matrix and a table of distortion-correcting look direction unit vectors    are provided for the purpose of calculating coordinates for every pixel.    See the description of variables 14 and 15 below.         To facilitate viewing of the images, a mapping of pixel value to a    recommended color table based on the characteristics of the selected    filter will be included with each image.  See the description of variables    19, 20, and 21 below.         A relative intensity scale is provided by the uncompressed count table    of variable 24.  Approximate intensity levels in kiloRayleighs are given in    the intensity table of variable 25.  Information on the availability of    more precisely calibrated intensities can be found on the VIS website at    URL http://eiger.physics.uiowa.edu/~vis/software/.  Variable descriptions:     1,2. Center time        The time assigned to an image is the center time of the integration        period within a resolution of 50 milliseconds.     3. Image counts        Image pixel counts range from 0 to 255.  They are stored in a two-        dimensional 256 x 256 byte array.  Images from the Earth camera        (sensor 0) are conventionally displayed with row 1 at the top, row 256        at the bottom, column 1 on the left, and column 256 on the right.  The        conventional image display for the low resolution camera (sensor 1) is        rotated 180 degrees so that the row 1-column 1 pixel is at the lower        right corner and the row 256-column 256 pixel is at the upper left        corner.  When displayed in this manner, the spacecraft spin axis is        oriented to the right in the display, the X component is defined as        the center of the image look direction, and the Y component is the        cross product of the spin axis and the look direction.     4. Sensor number        0 = Earth camera,        1 = low resolution camera,        2 = medium resolution camera.     5. Half integration time        This is half the length of the integration period for the image,        measured in milliseconds.     6. Filter        Twelve filters are available for visible imaging; the filter number,        1-12, is given here.  Ultra-violet imaging is done with one filter only,        designated here as filter number 0.  In addition, the peak wavelength        in Angstroms is given for the selected filter.     7. Presumed altitude of emissions        The presumed altitude of the emissions seen in the image varies        with the characteristics of the filter used.     8. Platform pitch angle        This is the platform pointing angle of rotation around the spin        axis, measured from nadir.   9,10. Geographic coordinates        Geographic north latitude and east longitude are provided for the        pixels at these image array locations: every 15th row starting        with row 1 and ending with row 256, and every 15th column starting        with column 1 and ending with column 256, for a total of        18 x 18 coordinate pairs.  11,12. Spacecraft position and velocity vectors, GCI        The spacecraft position vector and velocity vector in GCI        coordinates are for the image center time as given in variables        1 and 2.    13. Spacecraft spin axis unit vector, GCI  14,15. Image-to-GCI rotation matrix and look direction vector table        The rotation matrix may be used with the look direction vector table to        obtain pointing vectors in GCI coordinates for each pixel.  The        resulting vectors may be used to calculate coordinates for the observed        positions of the pixels.  Software for this purpose is available at URL         http://eiger.physics.uiowa.edu/~vis/software/.  The general method         used is described below.         In the image coordinate system, the X axis is the center line-of-sight        or look direction; the Y axis is the cross product of the spin axis an        the X axis; and the Z axis is the cross product of the X axis and the        Y axis.  When the display orientation conventions in the variable 3        description are applied, the low resolution camera image is rotated so        that both Earth camera and low resolution camera images are displayed        with Y axis pointing up and Z axis pointing toward the right.         To obtain the coordinates of the observed position of a pixel,        calculate the intersection of the line-of-sight with the surface        of an oblately spheroidal Earth at the altitude given as        variable 7.  The equation of the spheroid is            X**2/(A+ALT)**2 + Y**2/(A+ALT)**2 + Z**2/(B+ALT)**2 = 1            where A is the Earth radius at the equator,                  B is the Earth radius at the pole, and                  ALT is the given altitude.        The line-of-sight equations are            (X-SCX)/DX = (Y-SCY)/DY = (Z-SCZ)/DZ            where (SCX,SCY,SCZ) is the spacecraft position vector GCI, and                    (DX,DY,DZ)  is the look direction unit vector GCI.        Solve the line-of-sight equations for two variables in terms        of the third; substitute into the spheroid equation; and use the        quadratic formula to solve for the third variable.  Select        the solution point closer to the spacecraft.    16. Zenith angle of center line-of-sight at presumed altitude        This is the angle between the geocentric vector through the        observed point, assuming the altitude given as variable 7,        and the reverse of the image center line-of-sight vector.    17. Sun position unit vector, GCI    18. Solar zenith angle at observed point of center line-of-sight        This is the angle of the sun from zenith at the observed point        of the center line-of-sight, assuming the altitude given as        variable 7.    19. RGB color table        This is the recommended color table to be used with the        limits given in variables 20 and 21.  20,21. Low and high color mapping limits        The low and high color limits are recommended for remapping        the color table entries, as follows:            For pixel values less than the low limit, use the color                at table position 1.            For pixel values greater than or equal to the low limit                and less than or equal to the high limit, use the color                at table position (pix-low)/(high-low) x 255 + 1.            For pixel values greater than the high limit, use the color                at table position 256.    22. Data quality flag        The data quality word has bits set to 1 when the listed        conditions are true.  Bit #31 is the most significant bit in the        word, and it will not be used as a flag.  These are the bit        assignments:            bit 0 - image data frame sync error            bit 1 - image data frame counters error            bit 2 - image data fill frame flag.    23. Post gap flag        The post gap flag has these possible values:            0 - no gap occurred immediately prior to this record,            1 - the gap occurred because the instrument was not in                  a mode that allowed for the production of images for the                  selected sensor,            2 - the gap occurred because level zero data were missing,            3 - the gap occurred because level zero data were too                  noisy to extract images.    24. Expanded count table        The image pixel counts are quasi-logarithmically compressed to the        range 0-255.  This table gives the average of the uncompressed range        for each compressed count value.  Table entries 1-256 correspond to        compressed counts 0-255 respectively.    25. Intensity table        Approximate intensity levels in kiloRayleighs are given for each        compressed count value.  Table entries 1-256 correspond to compressed        counts 0-255 respectively.  Information on the availability of more        precisely calibrated intensities can be found on the VIS website at        URL http://eiger.physics.uiowa.edu/~vis/software/.  Supporting software:    Supporting software is available on the VIS website at the URL    http://eiger.physics.uiowa.edu/~vis/software/.  Included is an IDL program    that displays the images with the recommended color bar and provides    approximate intensities and coordinate data for each pixel.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/vis/vis_k1/1996/po_k1_vis_19960430_v03.cdf. The most common cadence, 267500 [ms] = PT4M27.5S, occurred for 9.5785% of the 25 timesteps. 

Earth Camera Key Parameter (from Master/CDFglobalAttributes/Data_type)

Presumed altitude of emissions (also quickly shows times when images are available)

Earth Camera UV Images (quasi-log cnts), small format display with click-expand (~4 min. res.)

Earth Camera UV Images (kRay), small format display with click-expand (~4 min. res.)

Primary UVI team data productsCDAWeb displayed images have time-tags shifted 51 seconds back from nominal EpochThis corrects that H2 Epochs are telemetry times, not centered collection time51 seconds is an approximate, typical correction.  Exact values depend on modes and transition status.

The Polar Ultraviolet Imager (UVI) Home Page contains links that describe the instrument, its operation, allow the user to view 36 second images and key parameter mosaics from the mission and download software, plus links to the UVI data archive, to lists of UVI publications and presentations, and several miscellaneous mission sites.

Level-1 Full Resolution Images (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/orbit/def_or/1997/po_or_def_19970715_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/orbit/pre_or/1996/po_or_pre_19960227_v06.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/orbit/def_pa/1996/po_pa_def_19960315_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 92.8289% of the 1411 timesteps. 

Polar Visible Imaging System (VIS) Earth Camera Images at ~4 minute cadence

Instrument functional description:The VIS is a set of three low-light-level cameras. Two of these cameras share primary and some secondary optics and are designed to provide images of the nighttime auroral oval at visible wavelengths. A third camera is used to monitor the directions of the fields-of-view of the auroral cameras with respect to the sunlit Earth and return global images of the auroral oval at ultraviolet wavelengths. The VIS instrumentation produces an auroral image of 256 x 256 pixels approximately every 24 seconds dependent on the integration time and filter selected.The fields-of-view of the two nighttime auroral cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and medium resolution cameras, respectively. The medium resolution camera was never activated. One or more Earth camera images of 256 x 256 pixels are produced every five minutes, depending on the commanded mode. The field-of-view of the Earth camera is approximately 20 x 20 degrees. Reference: Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan, M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller, 'The Visible Imaging System (VIS) for the Polar Spacecraft', Space Science Review, vol. 71, pp. 297-328, 1995. http://vis.physics.uiowa.edu/vis/vis_description/vis_description.htmlx [Note to first-time users:  The first six variables are of primary interest. The displayable 256 x 256 raw image data is in variable 3. The displayable 256 x 256 processed image datais in variable 4. The correct orientation of a displayed image is explained in the description of variable 3 below.] Data set description:The VIS Earth camera data set comprises all Earth camera images for the selected time period. The raw displayable image counts are in variable 3 while the processed displayable image counts are in variable 4. Full coordinate information is included for viewer orientation.  In addition, a rotation matrix and a table of distortion-correcting look direction unit vectors are provided for the purpose of calculating coordinates for every pixel. See the description of variables 20 and 21 below. To facilitate viewing of the images, a mapping of pixel value to a recommended color table based on the characteristics of the selected filter will be included with each image. See the description of variables 25, 26, and 27 below. A relative intensity scale is provided by the uncompressed count table of variable 30. Approximate intensity levels in kiloRayleighs are given in the intensity table of variable 31.For detailed information on intensities, see Sensitivities_and_Intensities.txt https://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/SENSITIVITIES_AND_INTENSITIES.TXT Variable descriptions: 1,2. Center timeThe time assigned to an image is the center time of the integration period within a resolution of 50 milliseconds. 3. Raw (unprocessed) image countsImage pixel counts range from 0 to 255. They are stored in a two-dimensional 256 x 256 byte array. Images from the Earth camera (sensor 0) are conventionally displayed with row 1 at the top, row 256 at the bottom,column 1 on the left, and column 256 on the right. The conventional image display for the low resolution camera (sensor 1) is rotated 180 degrees so that the row 1-column 1 pixel is at the lower right corner and the row 256-column 256 pixel is at the upper left corner. When displayed in this manner, the spacecraft spin axis is oriented to the right in the display, the X component is defined as the center of the image look direction, and the Y component is the cross product of the spin axis and the look direction. 4. Cleaned image countsThese are image pixel counts that have been calibrated using the following routines. For the earth camera: Horizontal Smooth EC 4 if Modified Julian Date (MJD) > 3429 (correction required after an event in 2005)Horizontal Smooth EC 6 if MJD > 4307 (correction required after an event in 2007)Subtract Cosmic RaysSubtract Slopes (adjusts for biases across the CCD)Remove Weave (corrects for interference from low resolution camera)Flat Field (corrects for other characteristics of the CCD) [Note: depending on viewing geometry, not all irregularities can be fixed completely;  in particular, a wide diagonal stripe may still be visible]Dayglow SubtractNightglow Minimum For the low resolution camera: Subtract Cosmic RaysSubtract SlopesFlat FieldSmooth Filter The data structure is the same as the Raw image counts. See the description of variable 3 for details. 5. Cleaned image data in kiloRayleighs.Same data as in variable 4, only in kiloRayleighs. 6. Sensor number0 = Earth camera1 = low resolution camera2 = medium resolution camera (never activated). 7. Half integration timeThis is half the length of the integration period for the image, measured in milliseconds. 8. Filter Twelve filters are available for visible imaging; the filter number, 1-12, is given here. Ultra-violet imaging is done with one filter only, designated here as filter number 0. In addition, the peak wavelength in Angstroms is given for the selected filter.For detailed information on filter characteristics, see Sensitivities_and_Intensities.txt https://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/SENSITIVITIES_AND_INTENSITIES.TXT 9. Presumed altitude of emissionsThe presumed altitude of the emissions seen in the image varies with the characteristics of the filter used. 10. Platform pitch angleThis is the platform pointing angle of rotation around the spin axis, measured from  nadir. 11,12. Geographic coordinatesGeographic north latitude and east longitude are provided for all pixels. 13,14. Right Ascension and Declination of each pixel These values are given in degrees. 15. Altitude along tangent to line-of-sight for each pixel. 16. Flag to indicate if each pixel is pointed at the earth.(0/False 1/True) 17,18. Spacecraft position and velocity vectors, GCIThe spacecraft position vector and velocity vector in GCI coordinates are for the image center time as given in variables 1 and 2. 19. Spacecraft spin axis unit vector, GCI 20,21. Image-to-GCI rotation matrix and look direction vector tableThe rotation matrix may be used with the look direction vector table to obtain pointing vectors in GCI coordinates for each pixel. The resulting vectors may be used to calculate coordinates for the observed positions of the pixels.The general method used is described below in Coordinate_Calculation.txt https://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/Coordinate_Calculation.txt 22. Zenith angle of center line-of-sight at presumed altitude This is the angle between the geocentric vector through the observed point, assuming the altitude given as variable 8, and the  reverse of the image center line-of-sight vector. 23. Sun position unit vector, GCI 24. Solar zenith angle at observed point of center line-of-sight.This is the angle of the sun from zenith at the observed point of the center line-of-sight, assuming the altitude given as variable 8. 25. RGB color tableThis is the recommended color table to be used with the limits given in variables 26 and 27.  26,27. Low and high color mapping limitsThe low and high color limits are recommended for remapping the color table entries, as follows:For pixel values less than the low limit, use the color at table position 1.For pixel values greater than or equal to the low limit and less than or equal to the high limit, use the color at table position (pix-low)/(high-low) x 255 + 1.For pixel values greater than the high limit, use the color at table position 256. 28. Data quality flag The data quality word has bits set to 1 when the listed conditions are true. Bit #31 is the most significant bit in the word, and it will not be used as a flag. These are the bit assignments:bit 0 - image data frame sync errorbit 1 - image data frame counters errorbit 2 - image data fill frame flag. 29. Post gap flagThe post gap flag has these possible values: 0 - no gap occurred immediately prior to this record.1 - the gap occurred because the instrument wasnot in a mode that allowed for the production of images for the selected sensor2 - the gap occurred because level zero data were missing3 - the gap occurred because level zero data were too noisy to extract images. 30. Expanded count tableThe image pixel counts are quasi-logarithmically compressed to the range 0-255. This table gives the average of the uncompressed range for each compressed count value. Table entries 1-256 correspond to compressed counts 0-255 respectively. 31. Intensity tableApproximate intensity levels in kiloRayleighs are given for each compressed count value. Table entries 1-256 correspond to compressed counts 0-255 respectively. Intensity calculation is described in Sensitivities_and_Intensities.txt. https://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/SENSITIVITIES_AND_INTENSITIES.TXT Supporting software:Supporting software is available at http://vis.physics.uiowa.edu/vis/software/ Included is an IDL program that displays the images with the recommended color bar, provides approximate intensities and coordinate data for each pixel, and and includes multiple options for image manipulation.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/vis/vis_earth-camera-calibrated/1996/po_vis_earth-camera-calibrated_1996043000_v01.cdf. The most common cadence, 53500 [ms] = PT53.5S, occurred for 35.0000% of the 21 timesteps. 

Uncleaned 256 x 256 Ultra-Violet Image (quasi-logarithmically compressed counts)

Cleaned and Filtered 256 x 256 Ultra-Violet Image (quasi-logarithmically compressed counts)

Instrument functional description:The VIS is a set of three low-light-level cameras. Two of these cameras share primary and some secondary optics and are designed to provide images of the nighttime auroral oval at visible wavelengths. A third camera is used to monitor the directions of the fields-of-view of the auroral cameras with respect to the sunlit Earth and return global images of the auroral oval at ultraviolet wavelengths. The VIS instrumentation produces an auroral image of 256 x 256 pixels approximately every 24 seconds dependent on the integration time and filter selected.The fields-of-view of the two nighttime auroral cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and medium resolution cameras, respectively. The medium resolution camera was never activated. One or more Earth camera images of 256 x 256 pixels are produced every five minutes, depending on the commanded mode. The field-of-view of the Earth camera is approximately 20 x 20 degrees. Reference: Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan, M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller, 'The Visible Imaging System (VIS) for the Polar Spacecraft', Space Science Review, vol. 71, pp. 297-328, 1995. http://vis.physics.uiowa.edu/vis/vis_description/vis_description.htmlx [Note to first-time users:  The first six variables are of primary interest. The displayable 256 x 256 raw image data is in variable 3. The displayable 256 x 256 processed image datais in variable 4. The correct orientation of a displayed image is explained in the description of variable 3 below.] Data set description:The VIS imaging data set comprises all Earth camera and Low Resolution camera images for the selected time period. The raw displayable image counts are in variable 3 while the processed displayable image counts are in variable 4. Full coordinate information is included for viewer orientation.  In addition, a rotation matrix and a table of distortion-correcting look direction unit vectors are provided for the purpose of calculating coordinates for every pixel. See the description of variables 20 and 21 below. To facilitate viewing of the images, a mapping of pixel value to a recommended color table based on the characteristics of the selected filter will be included with each image. See the description of variables 25, 26, and 27 below. A relative intensity scale is provided by the uncompressed count table of variable 30. Approximate intensity levels in kiloRayleighs are given in the intensity table of variable 31.For detailed information on intensities, see Sensitivities_and_Intensities.txt http://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/SENSITIVITIES_AND_INTENSITIES.TXT Variable descriptions: 1,2. Center timeThe time assigned to an image is the center time of the integration period within a resolution of 50 milliseconds. 3. Raw (unprocessed) image countsImage pixel counts range from 0 to 255. They are stored in a two-dimensional 256 x 256 byte array. Images from the Earth camera (sensor 0) are conventionally displayed with row 1 at the top, row 256 at the bottom,column 1 on the left, and column 256 on the right.  The conventional image display for the low resolution camera (sensor 1) is rotated 180 degrees so that the row 1-column 1 pixel is at the lower right corner and the row 256-column 256 pixel is at the upper left corner. When displayed in this manner, the spacecraft spin axis is oriented to the right in the display, the X component is defined as the center of the image look direction, and the Y component is the cross product of the spin axis and the look direction. 4. Cleaned image countsThese are image pixel counts that have been calibrated using the following routines. For the earth camera: Horizontal Smooth EC 4 if Modified Julian Date (MJD) > 3429 (correction required after an event in 2005)Horizontal Smooth EC 6 if MJD > 4307 (correction required after an event in 2007)Subtract Cosmic RaysSubtract Slopes (adjusts for biases across the CCD)Remove Weave (corrects for interference from low resolution camera)Flat Field (corrects for other characteristics of the CCD) [Note: depending on viewing geometry, not all irregularities can be fixed completely;  in particular, a wide diagonal stripe may still be visible]Dayglow SubtractNightglow Minimum For the low resolution camera: Subtract Cosmic RaysSubtract SlopesFlat FieldSmooth Filter The data structure is the same as the Raw image counts. See the description of variable 3 for details. 5. Cleaned image data in kiloRayleighs.Same data as in variable 4, only in kiloRayleighs. 6. Sensor number0 = Earth camera1 = low resolution camera2 = medium resolution camera (never activated). 7. Half integration timeThis is half the length of the integration period for the image, measured in milliseconds. 8. Filter Twelve filters are available for visible imaging; the filter number, 1-12, is given here. Ultra-violet imaging is done with one filter only, designated here as filter number 0. In addition, the peak wavelength in Angstroms is given for the selected filter.For detailed information on filter characteristics, see Sensitivities_and_Intensities.txt http://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/SENSITIVITIES_AND_INTENSITIES.TXT 9. Presumed altitude of emissionsThe presumed altitude of the emissions seen in the image varies with the characteristics of the filter used. 10. Field stop positionThe field stop may partially occlude the field of view of the low or medium resolution cameras.  The position is given in 1.5 degree steps. 11. Platform pitch angleThis is the platform pointing angle of rotation around the spin axis, measured from  nadir. 12,13. Mirror elevation and azimuth anglesFor the low or medium resolution camera, the two-axis mirror position is given in steps measured from the instrument calibration switches.The low resolution boresight is located at step 68 in azimuth and step 118 in elevation. 14,15. Geographic coordinatesGeographic north latitude and east longitude are provided for all pixels. 16,17. Right Ascension and Declination of each pixel These values are given in degrees. 18. Altitude along tangent to line-of-sight for each pixel. 19. Flag to indicate if each pixel is pointed at the earth.(0/False 1/True) 20,21. Spacecraft position and velocity vectors, GCIThe spacecraft position vector and velocity vector in GCI coordinates are for the image center time as given in variables 1 and 2. 22. Spacecraft spin axis unit vector, GCI 23,24. Image-to-GCI rotation matrix and look direction vector tableThe rotation matrix may be used with the look direction vector table to obtain pointing vectors in GCI coordinates for each pixel. The resulting vectors may be used to calculate coordinates for the observed positions of the pixels.The general method used is described below in Coordinate_Calculation.txt http://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/Coordinate_Calculation.txt 25. Zenith angle of center line-of-sight at presumed altitude This is the angle between the geocentric vector through the observed point, assuming the altitude given as variable 8, and the  reverse of the image center line-of-sight vector. 26. Sun position unit vector, GCI 27. Solar zenith angle at observed point of center line-of-sight.This is the angle of the sun from zenith at the observed point of the center line-of-sight, assuming the altitude given as variable 8. 28. RGB color tableThis is the recommended color table to be used with the limits given in variables 26 and 27. 29,30. Low and high color mapping limitsThe low and high color limits are recommended for remapping the color table entries, as follows:For pixel values less than the low limit, use the color at table position 1.For pixel values greater than or equal to the low limit and less than or equal to the high limit, use the color at table position (pix-low)/(high-low) x 255 + 1.For pixel values greater than the high limit, use the color at table position 256. 31. Data quality flag The data quality word has bits set to 1 when the listed conditions are true. Bit #31 is the most significant bit in the word, and it will not be used as a flag. These are the bit assignments:bit 0 - image data frame sync errorbit 1 - image data frame counters errorbit 2 - image data fill frame flag. 32. Post gap flagThe post gap flag has these possible values: 0 - no gap occurred immediately prior to this record.1 - the gap occurred because the instrument wasnot in a mode that allowed for the production of images for the selected sensor2 - the gap occurred because level zero data were missing3 - the gap occurred because level zero data were too noisy to extract images. 33. Expanded count tableThe image pixel counts are quasi-logarithmically compressed to the range 0-255. This table gives the average of the uncompressed range for each compressed count value. Table entries 1-256 correspond to compressed counts 0-255 respectively. 34. Intensity tableApproximate intensity levels in kiloRayleighs are given for each compressed count value. Table entries 1-256 correspond to compressed counts 0-255 respectively. Intensity calculation is described in Sensitivities_and_Intensities.txt. http://cdaweb.gsfc.nasa.gov/Polar_VIS_docs/SENSITIVITIES_AND_INTENSITIES.TXT Supporting software:Supporting software is available at http://vis.physics.uiowa.edu/vis/software/ Included is an IDL program that displays the images with the recommended color bar, provides approximate intensities and coordinate data for each pixel, and and includes multiple options for image manipulation.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/polar/vis/vis_visible-imager-calibrated/1996/po_vis_visible-imager-calibrated_1996111222_v01.cdf. The most common cadence, 24250 [ms] = PT24.25S, occurred for 20.0000% of the 1 timesteps. 

Low Resolution Images (from Master/CDFglobalAttributes/Data_type)

256 x 256 Visible Image (quasi-logarithmically compressed counts)

256 x 256 Cleaned and Filtered Visible Image (quasi-logarithmically compressed counts)

Merged hourly magnetic field, plasma, proton fluxes, and ephermis data of PSP 

COHO hourly and daily PSP data were made using PSP high res data from from CDAWeb at https://cdaweb.gsfc.nasa.gov/The name of the original  plasma data - '\PSP_SWP_SPC_L3I\', [ parameter names - Proton bulk velocity from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (Only Good Quality); [Total] proton density, from 1-dimensional Maxwellian fitting. (Only Good Quality); Proton radial [most probable] thermal speed component from 1-dimensional Maxwellian fitting. (Only Good Quality).] The name of  the original magnetic field data: \'PSP_FLD_L2_MAG_RTN_1MIN\'.and heliocentric trajectory from HELIOWeb at https://omniweb.gsfc.nasa.gov/coho/helios/heli.htmlThis file includes the PSP FIELDS Fluxgate Magnetometer data.and densities, vector velocities, and scalar (radial component) temperatures of the solar wind protons measured by the Solar Probe Cup (SPC). About PSP data in COHOWEB PSP https://omniweb.gsfc.nasa.gov/coho and https://cdaweb.gsfc.nasa.gov/.

This web site provides a overview description of the data and services provided by the COHOWeb interface and includes spacecraft mission specific notes, the data format specification, and coordinate system descriptions.

COHOWeb Deep Space Hourly and Daily Data and Service web site, GSFC, SPDF

Data access and services for hourly and daily merged interplanetary magnetic field, plasma, proton fluxes, and ephemerides data from deep space satellite missions. The services include: 1) Graphical browse and listing, 2) Listing, and plotting with filtering, 3) Distribution functions, medians, averages, standard deviations, 4) Scatter plotting, linear regression fitting, 5) FTPS access to hourly data, and 6) FTPS access to high resolution data.

The OMNIWeb Plus integrated interface provides access to the many interplanetary magnetic field, plasma, and energetic particle data sets hosted by the Goddard Space Flight Center, GSFC, Space Physics Data Facility, SPDF. OMNIWeb Plus services are available via several underlying interfaces including: OMNIWeb, COHOWeb, FTPBrowser, CDAWeb, HelioWeb, and direct HTTPS access that offering various functionalities.

SPDF/CDAWeb. Please also acknowledge the data producer: Natalia Papitashvili at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Natalia Papitashvili at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Natalia Papitashvili at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/coho1hr_magplasma/cdf/2018/psp_coho1hr_merged_mag_plasma_20180101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Parker Solar Probe (from all.xml/observatory/description/@short)

Parker Solar Probe (from Master/CDFglobalAttributes/Source_name)

HelioGraphic Inertial (HGI) latitude of the spacecraft position 

HelioGraphic Inertial (HGI) longitude of the spacecraft position

Parker Solar Probe, PSP, FIELDS Instrument Suite Description: Bale, S.D., Goetz, K., Harvey, P.R. et al., The FIELDS Instrument Suite for Solar Probe Plus, Space Sci Rev 204, 49-82 (2016)

PSP FIELDS Instrument Suite, Digital Fields Board, JGR Space Physics Publication

Parker Solar Probe, PSP, FIELDS Instrument Suite, Digital Fields Board, DFB, Description: Malaspina, D.M., Ergun, R.E., Bolton, M. et al., The Digital Fields Board for the FIELDS Instrument Suite on the Solar Probe Plus Mission: Analog and Digital signal Processing, JGR Space Physics, 121, 5088-5096 (2016)

PSP FIELDS Instrument Suite, Data Description, SOC Web Site, UC Berkeley

Parker Solar Probe, PSP, FIELDS Instrument Suite, Data Description and Access, Spacecraft Operations Center, SOC, Web Site, UC Berkeley

PSP FIELDS Instrument Suite, Rules of the Road, SOC Web Site, UC Berkeley

Parker Solar Probe, PSP, FIELDS Instrument Suite, Rules of the Road, Spacecraft Operations Center, SOC, Web Site, UC Berkeley

SPDF/CDAWeb. Please also acknowledge the data producer: Stuart D. Bale (bale@ssl.berkeley.edu) at UC Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Stuart D. Bale (bale@ssl.berkeley.edu) at UC Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Stuart D. Bale (bale@ssl.berkeley.edu) at UC Berkeley Space Sciences Laboratory

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_aeb1, @1 => epoch_aeb2.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_aeb1, @1 => epoch_aeb2.)

Parker Solar Probe FIELDS (from all.xml/observatory/description/@short)

Antenna Electronics Board (from all.xml/instrument/description/@short)

Parker Solar Probe FIELDS (from Master/CDFglobalAttributes/Source_name)

Commanded raw bias voltage (in DAC counts) applied to the V1 shield.

Commanded raw bias voltage (in DAC counts) applied to the V1 stub.

Bias current applied to the V1 whip, derived from measured bias voltage.

Bias current applied to the V1 whip, derived from commanded bias voltage.

Commanded raw bias voltage (in DAC counts) applied to the V1 whip.

Commanded raw bias voltage (in DAC counts) applied to the V2 shield.

Commanded raw bias voltage (in DAC counts) applied to the V2 stub.

Bias current applied to the V2 whip, derived from measured bias voltage.

Bias current applied to the V2 whip, derived from commanded bias voltage.

Commanded raw bias voltage (in DAC counts) applied to the V2 whip.

Commanded raw bias voltage (in DAC counts) applied to the V5 box.

Bias current applied to the V5 sensor, derived from measured bias voltage.

Bias current applied to the V5 sensor, derived from commanded bias voltage.

Commanded raw bias voltage (in DAC counts) applied to the V5 sensor.

Current draw of the floating power supply for the V1 and V2 antennas.

Measured temperature of the floating power supply for the V1 and V2 antennas.

Measured temperature of the floating power supply for the V5 sensor.

Commanded raw bias voltage (in DAC counts) applied to the V3 shield.

Commanded raw bias voltage (in DAC counts) applied to the V3 stub.

Bias current applied to the V3 whip, derived from measured bias voltage.

Bias current applied to the V3 whip, derived from commanded bias voltage.

Commanded raw bias voltage (in DAC counts) applied to the V3 whip.

Commanded raw bias voltage (in DAC counts) applied to the V4 shield.

Commanded raw bias voltage (in DAC counts) applied to the V4 stub.

Bias current applied to the V4 whip, derived from measured bias voltage.

Bias current applied to the V4 whip, derived from commanded bias voltage.

Commanded raw bias voltage (in DAC counts) applied to the V4 whip.

Current draw of the floating power supply for the V3 and V4 antennas.

Measured temperature of the floating power supply for the V3 and V4 antennas.

PSP FIELDS Level 2 Digital Fields Board (DFB) AC Bandpass Filter (BPF) of dV12 High Gain (HG) Channel (dV12hg)

PSP FIELDS Digital Fields Board (DFB), dV12hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The AC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, and (iii) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filters and analog filters have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB AC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC bandpass cadence is typically 1/8 of a NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Parker Solar Probe, PSP, Mission Overview, hosted by the Applied Physics Laboratory, Johns Hopkins University

PSP/FIELDS data release 5.1, on October 19, 2020, updates the dfb_dbm_scm and dfb_wf_dvdc data types to version 3. The new data versions contain significant corrections to the previously released data.

PSP/FIELDS data release 7, on April 4, 2021, includes data from PSP Encounter 6 (September 2020). All data up to and including December 2020 are now publicly available. For this data release, all DFB cross spectra have been reprocessed (with a new version number), and a subset of MAG data has also been reprocessed (with a new version number).

PSP/FIELDS data release 8, on June 28, 2021, includes survey data from PSP Encounter 7 and Venus Gravity assist 4. Several data sets have been updated in release 8.

PSP/FIELDS Data Release 9, on October 29, 2021, includes select data from Encounter 7 (perihelion January 2021), and survey and select data from Encounter 8 (perihelion April 2021).

PSP/FIELDS Data Release 10, on February 7, 2022, includes survey and select data from Encounter 9 (perihelion August 2021).

PSP/FIELDS Data Release 11, on April 25, 2022, includes survey and select data from Encounter 10 (perihelion November 2021), and survey and select data from Venus Gravity Assist 5 (October 2021).

Digital Fields Board AC Bandpass Filter dV12hg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), dV34hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The AC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, and (iii) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filters and analog filters have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB AC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC bandpass cadence is typically 1/8 of a NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Bandpass Filter dV34hg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMulfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The AC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, and (iii) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filters and analog filters have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB AC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC bandpass cadence is typically 1/8 of a NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Bandpass Filter SCMulfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMumfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The AC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, and (iii) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filters and analog filters have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB AC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC bandpass cadence is typically 1/8 of a NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Bandpass Filter SCMumfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), dV12hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra dV12hg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of dV34 High Gain (HG) Channel (DV34HG)

PSP FIELDS Digital Fields Board (DFB), dV34hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra dV34hg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of Search Coil Magnetometer (SCM) D Low Frequency (LF) High Gain (HG) Channel (SCMDLFHG)

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra SCMdlfhg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of Search Coil Magnetometer (SCM) E Low Frequency (LF) High Gain (HG) Channel (SCMELFHG)

PSP FIELDS Digital Fields Board (DFB), SCMelfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra SCMelfhg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of Search Coil Magnetometer (SCM) F Low Frequency (LF) High Gain (HG) Channel (SCMFLFHG)

PSP FIELDS Digital Fields Board (DFB), SCMflfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra SCMflfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMmf data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra SCMmf (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of Search Coil Magnetometer (SCM) U Low Frequency (LF) Low Gain (LG) Channel (SCMULFLG)

PSP FIELDS Digital Fields Board (DFB), SCMulflg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra SCMulflg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of Search Coil Magnetometer (SCM) V Low Frequency (LF) High Gain (HG) Channel (SCMVLFHG)

PSP FIELDS Digital Fields Board (DFB), SCMvlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra SCMvlfhg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Spectra of V5 High Gain (HG) Channel (V5HG)

PSP FIELDS Digital Fields Board (DFB), V5hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.  The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features at the highest frequencies.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_3vector = R ## spectra_def_3vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB AC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), the DFB AC spectra data is typically reported each 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board AC Spectra V5hg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Cross Spectra (XSPEC) between DV12HG and DV34HG Channels

PSP FIELDS Digital Fields Board (DFB), dV12hg x dV34hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

Digital Fields Board AC Cross Spectra dV34hg (from all.xml/instrument/description/@short)

L2 XSpectra Real Part of Crossterm (FT_1 x FT_2^*) for channel DV12HG and DV34HG

L2 XSpectra Imag Part of Crossterm (FT_1 x FT_2^*) for channel DV12HG and DV34HG

PSP FIELDS Level 2 DFB AC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) D and E Low Frequency (LF) High Gain (HG) Channels 

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg x SCMelfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg x SCMelfhg data. 

Digital Fields Board AC Cross Spectra SCMelfhg (from all.xml/instrument/description/@short)

L2 XSpectra Coherence between channel SCMDLFHG and channel SCMELFHG

L2 XSpectra Phase of channel SCMELFHG relative to channel SCMDLFHG

L2 XSpectra Real Part of Crossterm (FT_1 x FT_2^*) for channel SCMDLFHG and SCMELFHG

L2 XSpectra Imag Part of Crossterm (FT_1 x FT_2^*) for channel SCMDLFHG and SCMELFHG

PSP FIELDS Level 2 DFB AC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) D and F Low Frequency (LF) High Gain (HG) Channels 

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg x SCMflfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg x SCMflfhg data. 

Digital Fields Board AC Cross Spectra SCMflfhg (from all.xml/instrument/description/@short)

L2 XSpectra Coherence between channel SCMDLFHG and channel SCMFLFHG

L2 XSpectra Phase of channel SCMFLFHG relative to channel SCMDLFHG

L2 XSpectra Real Part of Crossterm (FT_1 x FT_2^*) for channel SCMDLFHG and SCMFLFHG

L2 XSpectra Imag Part of Crossterm (FT_1 x FT_2^*) for channel SCMDLFHG and SCMFLFHG

PSP FIELDS Level 2 DFB AC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) E and F Low Frequency (LF) High Gain (HG) Channels 

PSP FIELDS Digital Fields Board (DFB), SCMelfhg x SCMflfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB AC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence).  Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N.  For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

PSP FIELDS Digital Fields Board (DFB), SCMelfhg x SCMflfhg data. 

L2 XSpectra Coherence between channel SCMELFHG and channel SCMFLFHG

L2 XSpectra Phase of channel SCMFLFHG relative to channel SCMELFHG

L2 XSpectra Real Part of Crossterm (FT_1 x FT_2^*) for channel SCMELFHG and SCMFLFHG

L2 XSpectra Imag Part of Crossterm (FT_1 x FT_2^*) for channel SCMELFHG and SCMFLFHG

PSP FIELDS Level 2 DFB AC Differential Voltage (DV) Burst Waveform (DBM) Data

PSP FIELDS Digital Fields Board (DFB), Differential Voltage data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB burst waveform data consist of short bursts of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. These data are pre-sorted by on-board competitive selection algorithms described in [3] before storage by FIELDS. A sub-set of this stored burst data is telemetered to Earth for scientist-selected regions of interest.  The Level 2 data products contained in this data file have been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter phase response, and (iv) the search coil preamplifier gain/phase response (when applicable). Calibrations for the FIELDS voltage sensor preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution for the DFB burst waveform data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB burst waveform data is typically 150,000 samples/second.  This rate is the sample rate of the ADC, and data taken at this rate do not pass through a digital filter.References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_dvac, @1 => psp_fld_l2_dfb_dbm_dvac_time_series_TT2000_f.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_dvac, @1 => psp_fld_l2_dfb_dbm_dvac_time_series_TT2000_f.)

Digital Fields Board Differential Voltage Burst Waveform (from all.xml/instrument/description/@short)

L2 AC Burst Differential Voltage from Sensors 1 and 2 median value

L2 AC Burst Differential Voltage from Sensors 3 and 4 median value

PSP FIELDS Level 2 DFB DC Burst Differential Voltage Waveform Data

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_dvdc, @1 => psp_fld_l2_dfb_dbm_dvdc_time_series_TT2000_f.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_dvdc, @1 => psp_fld_l2_dfb_dbm_dvdc_time_series_TT2000_f.)

L2 DC Burst Differential Voltage from Sensors 1 and 2 median value

L2 DC Burst Differential Voltage from Sensors 3 and 4 median value

PSP FIELDS Digital Fields Board (DFB), Search Coil data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB burst waveform data consist of short bursts of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. These data are pre-sorted by on-board competitive selection algorithms described in [3] before storage by FIELDS. A sub-set of this stored burst data is telemetered to Earth for scientist-selected regions of interest.  The Level 2 data products contained in this data file have been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter phase response, and (iv) the search coil preamplifier gain/phase response (when applicable). Calibrations for the FIELDS voltage sensor preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution for the DFB burst waveform data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB burst waveform data is typically 150,000 samples/second.  This rate is the sample rate of the ADC, and data taken at this rate do not pass through a digital filter.References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => psp_fld_l2_dfb_dbm_scmlg_time_series_TT2000_f, @1 => epoch_psp_fld_l2_dfb_dbm_scmhg, @2 => psp_fld_l2_dfb_dbm_scmhg_time_series_TT2000_f.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => psp_fld_l2_dfb_dbm_scmlg_time_series_TT2000_f, @1 => epoch_psp_fld_l2_dfb_dbm_scmhg, @2 => psp_fld_l2_dfb_dbm_scmhg_time_series_TT2000_f.)

Digital Fields Board Search Coil Burst Waveform (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB AC Burst Single Ended Voltage Waveform Data

PSP FIELDS Digital Fields Board (DFB), Single Ended Voltage data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB burst waveform data consist of short bursts of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. These data are pre-sorted by on-board competitive selection algorithms described in [3] before storage by FIELDS. A sub-set of this stored burst data is telemetered to Earth for scientist-selected regions of interest.  The Level 2 data products contained in this data file have been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter phase response, and (iv) the search coil preamplifier gain/phase response (when applicable). Calibrations for the FIELDS voltage sensor preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution for the DFB burst waveform data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB burst waveform data is typically 150,000 samples/second.  This rate is the sample rate of the ADC, and data taken at this rate do not pass through a digital filter.References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_vac, @1 => psp_fld_l2_dfb_dbm_vac_time_series_TT2000_f.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_vac, @1 => psp_fld_l2_dfb_dbm_vac_time_series_TT2000_f.)

Digital Fields Board Single Ended Voltage Burst Waveform (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB DC Burst Single Ended Voltage Waveform Data

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_vdc, @1 => psp_fld_l2_dfb_dbm_vdc_time_series_TT2000_f.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_psp_fld_l2_dfb_dbm_vdc, @1 => psp_fld_l2_dfb_dbm_vdc_time_series_TT2000_f.)

PSP FIELDS Level 2 DFB DC Bandpass Filter (BPF) of dV12hg Channel

PSP FIELDS Digital Fields Board (DFB), dV12hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, (iii) DFB digital filter time delays, which become significant in the lowest frequency DC bandpass bins, and (iv) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filter and analog filter gains have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB DC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), DFB AC bandpass cadence is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Bandpass Filter dV12hg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB DC Bandpass Filter (BPF) of dV34 High Gain (HG) Channel (DV34HG)

PSP FIELDS Digital Fields Board (DFB), dV34hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, (iii) DFB digital filter time delays, which become significant in the lowest frequency DC bandpass bins, and (iv) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filter and analog filter gains have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB DC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), DFB AC bandpass cadence is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Bandpass Filter dV34hg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMulfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, (iii) DFB digital filter time delays, which become significant in the lowest frequency DC bandpass bins, and (iv) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filter and analog filter gains have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB DC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), DFB AC bandpass cadence is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Bandpass Filter SCMulfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMvlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC bandpass data consist of peak and average values of the absolute value of band-passed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3]. The Level 2 data products contained in this data file have been calibrated for (i) the ~6.3 dB loss associated with forming the bandpass signal [3], (ii) DFB in-band gain, (iii) DFB digital filter time delays, which become significant in the lowest frequency DC bandpass bins, and (iv) the search coil preamplifier response (when applicable). Calibrations for the DFB digital filter and analog filter gains have not been implemented, as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response, and because all bins except the highest frequency bin have a flat gain response equal to 1 due to these filters.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied voltage sensor signals (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution of the DFB DC bandpass data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), DFB AC bandpass cadence is typically 1 NYsecond [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Bandpass Filter SCMvlfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), dV12hg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra dV12hg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra SCMdlfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMelfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra SCMelfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMflfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra SCMflfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMulfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra SCMulfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMvlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra SCMvlfhg (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), SCMwlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time.  These spectra are averaged in both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins, with the bin central frequencies reported in the metadata. The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz.The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]Time resolution of the DFB DC spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board DC Spectra SCMwlfhg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB DC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) D and E Low Frequency (LF) High Gain (HG) Channels 

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg x SCMelfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.    The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the search coil auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

Digital Fields Board DC Cross Spectra SCMelfhg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB DC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) D and F Low Frequency (LF) High Gain (HG) Channels 

PSP FIELDS Digital Fields Board (DFB), SCMdlfhg x SCMflfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.    The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the search coil auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

Digital Fields Board DC Cross Spectra SCMflfhg (from all.xml/instrument/description/@short)

PSP FIELDS Level 2 DFB DC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) E and F Low Frequency (LF) High Gain (HG) Channels 

PSP FIELDS Digital Fields Board (DFB), SCMelfhg x SCMflfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.    The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the search coil auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

PSP FIELDS Level 2 Digital Fields Board (DFB) DC Cross Spectra (XSPEC) between Search Coil Magnetometer (SCM) V and W Low Frequency (LH) High Gain (HG) Sensors

PSP FIELDS Digital Fields Board (DFB), SCMvlfhg x SCMwlfhg data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB DC cross spectra data consist of, for a pair of input channels, (i) power spectral densities (auto spectra, e.g. FT1 x FT1*), (ii) real and imaginary parts of the spectral cross term (FT1 x FT2*), (iii) coherence, and (iv) phase, all as a function of frequency and time.  Coherence and phase are defined in [3].  These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.    The Level 2 data products contained in this data file have been calibrated for (i) the Hanning window used in the spectral calculation, (ii) DFB in-band gain, (iii) DFB analog filter gain response, (iv) DFB digital filter gain response, (v) the search coil preamplifier response (when applicable), (vi) the bandwidth of each spectral bin.  Note that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise.  This effect should be examined carefully when determining spectral slopes and features.  Calibrations for the FIELDS preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts^2/Hz.  Units for all magnetic field quantities are nT^2/Hz. Coherence is unitless.  Units for phase are degrees. The Level 2 voltage data products contained in this data file are in sensor coordinates (e.g. dV12, dV34 for voltage measurements). For solar orbits 1 and 2, the search coil magnetometer cross spectral data is rotated into a non-intuitive coordinate system (d,e,f). For solar orbits 3 and beyond, magnetic field data products are in the u,v,w search coil magnetometer sensor coordinates.  To rotate from d,e,f into u,v,w search coil sensor coordinates, use the following matrix as (IDL notation) spectra_uvw_vector = R ## spectra_def_vector.  R =  [ [ 0.46834856  , -0.81336422    ,  0.34509170]       [-0.66921924  , -0.071546954   ,  0.73961249]       [-0.57688408  , -0.57733845    , -0.57782790]  ]For some orbits, sufficient spectral information exists in the search coil auto- and cross-spectra to determine wave ellipticity, planarity, and wave normal angles.  One method for accomplishing this is presented in [4]. Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [2].  Timestamps correspond to the center time of each window. References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Santolik, O., Parrot, M., Lefeuvre, F. (2003) Radio Science, 38, 1010. https://doi.org/10.1029/2000RS002523 

PSP FIELDS Digital Fields Board (DFB), SCMvlfhg x SCMwlfhg data. 

Digital Fields Board DC Cross Spectra SCMwlfhg (from all.xml/instrument/description/@short)

L2 XSpectra Coherence between channel SCMVLFHG and channel SCMWLFHG

L2 XSpectra Phase of channel SCMWLFHG relative to channel SCMVLFHG

L2 XSpectra Real Part of Crossterm (FT_1 x FT_2^*) for channel SCMVLFHG and SCMWLFHG

L2 XSpectra Imag Part of Crossterm (FT_1 x FT_2^*) for channel SCMVLFHG and SCMWLFHG

PSP FIELDS Digital Fields Board (DFB), Differential Voltage data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB continuous waveform data consist of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. The Level 2 data products contained in this data file have been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter phase response, and (iv) the search coil preamplifier gain/phase response (when applicable). Calibrations for the FIELDS digital filter gain response have not been implemented, but the required convolution kernel is provided in this file.  It was decided not to apply the FIELDS digital filter gain response to the L2 data because this can introduce non-physical power at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS voltage sensor preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in spacecraft coordinates (e.g. x,y,z) and in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution for the DFB continuous waveform data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB continuous waveform data is typically 256 samples/NYsecond [2].  References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Digital Fields Board Differential Voltage Waveform (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), Search Coil Magnetometer data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB continuous waveform data consist of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. The Level 2 data products contained in this data file have been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter phase response, and (iv) the search coil preamplifier gain/phase response (when applicable). Calibrations for the FIELDS digital filter gain response have not been implemented, but the required convolution kernel is provided in this file.  It was decided not to apply the FIELDS digital filter gain response to the L2 data because this can introduce non-physical power at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS voltage sensor preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in spacecraft coordinates (e.g. x,y,z) and in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution for the DFB continuous waveform data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB continuous waveform data is typically 256 samples/NYsecond [2].  References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => hg_epoch, @1 => lg_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => hg_epoch, @1 => lg_epoch.)

Digital Fields Board Search Coil Magnetometer Waveform (from all.xml/instrument/description/@short)

PSP FIELDS Digital Fields Board (DFB), Single Ended Voltage data. The DFB is the low frequency (< 75 kHz) component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the DFB, see [3].DFB continuous waveform data consist of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. The Level 2 data products contained in this data file have been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter phase response, and (iv) the search coil preamplifier gain/phase response (when applicable). Calibrations for the FIELDS digital filter gain response have not been implemented, but the required convolution kernel is provided in this file.  It was decided not to apply the FIELDS digital filter gain response to the L2 data because this can introduce non-physical power at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS voltage sensor preamplifiers have not been implemented, as the preamplifier response is flat and equal to 1 through the DFB frequency range.  Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data (these corrections will be applied in Level 3 DFB data), therefore units for all voltage sensor quantities are Volts.  Units for all magnetic field quantities are nT.The Level 2 data products contained in this data file are in spacecraft coordinates (e.g. x,y,z) and in sensor coordinates (e.g. dV12, dV34 for voltage measurements, and u,v,w for the search coil magnetometer). Time resolution for the DFB continuous waveform data can vary by multiples of 2^N.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB continuous waveform data is typically 256 samples/NYsecond [2].  References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => v1_epoch, @1 => v2_epoch, @2 => v3_epoch, @3 => v4_epoch, @4 => v5_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => v1_epoch, @1 => v2_epoch, @2 => v3_epoch, @3 => v4_epoch, @4 => v5_epoch.)

Digital Fields Board Single Ended Voltage Waveform (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: Stuart D. Bale (bale@berkeley.edu) at UC Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Stuart D. Bale (bale@berkeley.edu) at UC Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Stuart D. Bale (bale@berkeley.edu) at UC Berkeley Space Sciences Laboratory

Parker Solar Probe - FIELDS Instrument Suite (from all.xml/observatory/description/@short)

FIELDS2-100bps Time Domain Sampler Moments (from all.xml/instrument/description/@short)

Parker Solar Probe - FIELDS Instrument Suite (from Master/CDFglobalAttributes/Source_name)

Summary Telemetry Data (from Master/CDFglobalAttributes/Data_type)

Corrected UTC time of the center of the collected data stripe (TT2000)

FIELDS2 100bps flight software telemetry format version number. Note: CDF_UINT4 data was converted to HAPI double.

The RMS of the magnitude of the 3-axis B field vector observed during this sample period on the inner magnetometer (nT RMS)

The average value observed during this sample period on the three inner magnetometer axes in S/C coordinates (nT)

The average value observed during this sample period on the three inner magnetometer axes in RTN coordinates (nT)

The number of TDS bursts obtained during this sample period (count). Note: CDF_UINT4 data was converted to HAPI double.

The quality value of the best TDS burst obtained during this sample period (arbitrary units - bigger is better). Note: CDF_UINT4 data was converted to HAPI double.

The frequency (or zero crossings) value observed from the best TDS burst obtained during this sample period (Hz)

The normalized peak value observed on the V1 high-gain full-speed TDS channel (Ch1) during this sample period (+1 to -1)

The normalized peak value observed on the V2 high-gain full-speed TDS channel (Ch2) during this sample period (+1 to -1)

The normalized peak value observed on the V3 high-gain full-speed TDS channel (Ch3) during this sample period (+1 to -1)

The normalized peak value observed on the V4 high-gain full-speed TDS channel (Ch4) during this sample period (+1 to -1)

The normalized peak value observed on the V5 high-gain full-speed TDS channel (Ch5) during this sample period (+1 to -1)

The normalized peak value observed on the V1-V2 difference full-speed TDS channel (Ch3) during this sample period (+1 to -1)

The normalized peak value observed on the V3-V4 difference full-speed TDS channel (Ch1) during this sample period (+1 to -1)

The normalized peak value observed on the V1234 summation full-speed TDS channel (Ch2) during this sample period (+1 to -1)

The normalized peak value observed on the MF SCM high-gain full-speed TDS channel (Ch4) during this sample period (+1 to -1)

The normalized peak value observed on the MF SCM high-gain full-speed TDS channel (Ch5) during this sample period (+1 to -1)

The normalized peak value observed on the MF SCM low-gain full-speed TDS channel (Ch4) during this sample period (+1 to -1)

The normalized peak value observed on the V1 low-gain full-speed TDS channel (Ch3) during this sample period (+1 to -1)

The normalized peak value observed on the V2 low-gain full-speed TDS channel (Ch5) during this sample period (+1 to -1)

The normalized peak value observed on the V3 low-gain full-speed TDS channel (Ch1) during this sample period (+1 to -1)

The normalized peak value observed on the V4 low-gain full-speed TDS channel (Ch2) during this sample period (+1 to -1)

The normalized peak value observed on the V5 low-gain full-speed TDS channel (Ch4) during this sample period (+1 to -1)

The peak value observed on the V1 high-gain full-speed TDS channel (Ch1) during this sample period (mV)

The peak value observed on the V2 high-gain full-speed TDS channel (Ch2) during this sample period (mV)

The peak value observed on the V3 high-gain full-speed TDS channel (Ch3) during this sample period (mV)

The peak value observed on the V4 high-gain full-speed TDS channel (Ch4) during this sample period (mV)

The peak value observed on the V5 high-gain full-speed TDS channel (Ch5) during this sample period (mV)

The peak value observed on the V1-V2 difference full-speed TDS channel (Ch3) during this sample period (mV)

The peak value observed on the V3-V4 difference full-speed TDS channel (Ch1) during this sample period (mV)

The peak value observed on the V1+V2+V3+V4 summation full-speed TDS channel (Ch2) during this sample period (mV)

The peak value observed on the MF SCM high-gain full-speed TDS channel (Ch4) during this sample period (nT)

The peak value observed on the MF SCM high-gain full-speed TDS channel (Ch5) during this sample period (nT)

The peak value observed on the MF SCM low-gain full-speed TDS channel (Ch4) during this sample period (nT)

The peak value observed on the V1 low-gain full-speed TDS channel (Ch3) during this sample period (mV)

The peak value observed on the V2 low-gain full-speed TDS channel (Ch5) during this sample period (mV)

The peak value observed on the V3 low-gain full-speed TDS channel (Ch1) during this sample period (mV)

The peak value observed on the V4 low-gain full-speed TDS channel (Ch2) during this sample period (mV)

The peak value observed on the V5 low-gain full-speed TDS channel (Ch4) during this sample period (mV)

The RMS value observed on the V1 high-gain possibly down-sampled TDS channel (Ch1) during this sample period (mV)

The RMS value observed on the V2 high-gain possibly down-sampled TDS channel (Ch2) during this sample period (mV)

The RMS value observed on the V3 high-gain possibly down-sampled TDS channel (Ch3) during this sample period (mV)

The RMS value observed on the V4 high-gain possibly down-sampled TDS channel (Ch4) during this sample period (mV)

The RMS value observed on the V5 high-gain possibly down-sampled TDS channel (Ch5) during this sample period (mV)

The RMS value observed on the V1-V2 difference possibly down-sampled TDS channel (Ch3) during this sample period (mV)

The RMS value observed on the V3-V4 difference possibly down-sampled TDS channel (Ch1) during this sample period (mV)

The RMS value observed on the V1+V2+V3+V4 summation possibly down-sampled TDS channel (Ch2) during this sample period (mV)

The RMS value observed on the MF SCM high-gain possibly down-sampled TDS channel (Ch4) during this sample period (nT)

The RMS value observed on the MF SCM high-gain possibly down-sampled TDS channel (Ch5) during this sample period (nT)

The RMS value observed on the MF SCM low-gain possibly down-sampled TDS channel (Ch4) during this sample period (nT)

The RMS value observed on the V1 low-gain possibly down-sampled TDS channel (Ch3) during this sample period (mV)

The RMS value observed on the V2 low-gain possibly down-sampled TDS channel (Ch5) during this sample period (mV)

The RMS value observed on the V3 low-gain possibly down-sampled TDS channel (Ch1) during this sample period (mV)

The RMS value observed on the V4 low-gain possibly down-sampled TDS channel (Ch2) during this sample period (mV)

The RMS value observed on the V5 low-gain possibly down-sampled TDS channel (Ch4) during this sample period (mV)

The banded frequency (or zero crossings) observed on the V1 high-gain TDS channel (Ch1) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V2 high-gain TDS channel (Ch2) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V3 high-gain TDS channel (Ch3) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V4 high-gain TDS channel (Ch4) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V5 high-gain TDS channel (Ch5) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V1-V2 difference TDS channel (Ch3) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V3-V4 difference TDS channel (Ch1) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V1+V2+V3+V4 summation TDS channel (Ch2) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the MF SCM high-gain TDS channel (Ch4) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the MF SCM high-gain TDS channel (Ch5) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the MF SCM low-gain TDS channel (Ch4) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V1 low-gain TDS channel (Ch3) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V2 low-gain TDS channel (Ch5) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V3 low-gain TDS channel (Ch1) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V4 low-gain TDS channel (Ch2) during this sample period (Hz)

The banded frequency (or zero crossings) observed on the V5 low-gain TDS channel (Ch4) during this sample period (Hz)

The wave-particle correlator particle counting frequency observed during this sample period (particle counts per second)

The wave-particle correlator skew observed during this sample period (dimensionless)

Gives the average DC voltage from one of the four V1234 electric field sensors during the event/packet (Volts)

Indicates the average rotational speed of one of the four reaction wheels during the event/packet (revolutions per second)

PSP FIELDS full cadence Fluxgate Magnetometer (MAG) data in RTN coordinates

PSP FIELDS Fluxgate Magnetometer data. Time resolution varies with instrument mode, ranging from 2.3-292.9 samples/sec, corresponding to 2-256 samples per 0.874 seconds (0.874 = 2^25 / 38.4 MHz, see reference [2]).The Magnetometer has 4 ranges - +/-1024, +/-4096, +/-16,384, +/-65,536 nT, selected by the ranging algorithm, based on the ambient magnetic field. Precision is +/- 15 bits, based on the 16-bit ADC.References:1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-62. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-5

PSP/FIELDS Rules of the Road available at http://fields.ssl.berkeley.edu/rules/

Counts based on variable 'epoch_mag_RTN' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_rtn/2018/psp_fld_l2_mag_rtn_2018100200_v02.cdf. The most common cadence occurred for 58.7296% of the 336342 timesteps. Cadence = 13653248 [ns] = PT0.013653S.

Fluxgate Magnetometer data in RTN coordinates (from all.xml/instrument/description/@short)

PSP FIELDS 1 minute cadence Fluxgate Magnetometer (MAG) data in RTN coordinates

Counts based on variable 'epoch_mag_RTN_1min' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_rtn_1min/2018/psp_fld_l2_mag_rtn_1min_20181002_v02.cdf. The most common cadence occurred for 100.0000% of the 790 timesteps. Cadence = 60000000000 [ns] = PT1M.

PSP FIELDS 4 samples per cycle cadence Fluxgate Magnetometer (MAG) data in RTN coordinates

Counts based on variable 'epoch_mag_RTN_4_Sa_per_Cyc' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_rtn_4_per_cycle/2018/psp_fld_l2_mag_rtn_4_sa_per_cyc_20181002_v02.cdf. The most common cadence occurred for 51.4527% of the 111483 timesteps. Cadence = 218453376 [ns] = PT0.218453S.

Time in TT2000 for 4 samples per cycle cadence MAG waveform data

PSP FIELDS full cadence Fluxgate Magnetometer (MAG) data in SC coordinates

Counts based on variable 'epoch_mag_SC' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_sc/2018/psp_fld_l2_mag_sc_2018100200_v02.cdf. The most common cadence occurred for 58.7296% of the 336342 timesteps. Cadence = 13653248 [ns] = PT0.013653S.

Fluxgate Magnetometer data in SC coordinates (from all.xml/instrument/description/@short)

PSP FIELDS 1 minute cadence Fluxgate Magnetometer (MAG) data in SC coordinates

Counts based on variable 'epoch_mag_SC_1min' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_sc_1min/2018/psp_fld_l2_mag_sc_1min_20181002_v02.cdf. The most common cadence occurred for 100.0000% of the 790 timesteps. Cadence = 60000000000 [ns] = PT1M.

PSP FIELDS 4 samples per cycle cadence Fluxgate Magnetometer (MAG) data in SC coordinates

Counts based on variable 'epoch_mag_SC_4_Sa_per_Cyc' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_sc_4_per_cycle/2018/psp_fld_l2_mag_sc_4_sa_per_cyc_20181002_v02.cdf. The most common cadence occurred for 51.4527% of the 111483 timesteps. Cadence = 218453376 [ns] = PT0.218453S.

PSP FIELDS full cadence Fluxgate Magnetometer (MAG) data in VSO coordinates

Counts based on variable 'epoch_mag_VSO' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/mag_vso/2018/psp_fld_l2_mag_vso_2018100200_v02.cdf. The most common cadence occurred for 58.7296% of the 336342 timesteps. Cadence = 13653248 [ns] = PT0.013653S.

Fluxgate Magnetometer data in VSO coordinates (from all.xml/instrument/description/@short)

PSP FIELDS Radio Frequency Spectrometer (RFS), BURST data.The RFS is the high frequency component  of the FIELDS experiment on the  Parker Solar Probe spacecraft [1].  For a full description of the FIELDS  experiment, see [2].  For a description  of the RFS, see [3].The RFS produces auto and cross spectral data products in two frequency ranges, the LFR (Low Frequency Reciever) range and the HFR (High Frequency Receiver) range.  Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR HiRes spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, and the polyphase filter bank (PFB) and the FFT spectral processing as described in [3].  Corrections for base capacitance and antenna effective length have not been applied (these corrections will be applied in Level 3 RFS data.) Therefore, units for all spectral quantities are given in V^2/Hz.Time resolution of the RFS varies with instrument mode.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for RFS HFR and LFR spectra is typically about 7 seconds.  During cruise mode, which is the default mode for operations outside of 0.25 AU, cadence for HFR and LFR spectra is about 56 seconds.References:1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-62. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-53. Pulupa, M., Bale, S. D., Bonnell, J.W. et al. (2017) JGR Space Physics, 122, 2836-2854. https://doi.org/10.1002/2016JA023345

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_burst_auto_ch0_V1V2, @1 => epoch_burst_auto_ch1_V3V4, @2 => epoch_burst_cross_im_V1V2_V3V4, @3 => epoch_burst_cross_re_V1V2_V3V4, @4 => epoch_burst.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_burst_auto_ch0_V1V2, @1 => epoch_burst_auto_ch1_V3V4, @2 => epoch_burst_cross_im_V1V2_V3V4, @3 => epoch_burst_cross_re_V1V2_V3V4, @4 => epoch_burst.)

Radio Frequency Spectrometer BURST (from all.xml/instrument/description/@short)

Counts based on variable 'epoch_burst_auto_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/rfs_burst/2019/psp_fld_l2_rfs_burst_20191226_v02.cdf. The most common cadence occurred for 75.4220% of the 4155 timesteps. Cadence = 218505856 [ns] = PT0.218506S.

Counts based on variable 'epoch_burst_auto_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/rfs_burst/2019/psp_fld_l2_rfs_burst_20191226_v02.cdf. The most common cadence occurred for 75.4220% of the 4155 timesteps. Cadence = 218505856 [ns] = PT0.218506S.

Counts based on variable 'epoch_burst_cross_im_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/rfs_burst/2019/psp_fld_l2_rfs_burst_20191226_v02.cdf. The most common cadence occurred for 75.4220% of the 4155 timesteps. Cadence = 218505856 [ns] = PT0.218506S.

Gain flag for BURST Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

N summed spectra for BURST Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

Overrange flag for BURST Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

Counts based on variable 'epoch_burst_cross_re_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/rfs_burst/2019/psp_fld_l2_rfs_burst_20191226_v02.cdf. The most common cadence occurred for 75.4220% of the 4155 timesteps. Cadence = 218505856 [ns] = PT0.218506S.

Gain flag for BURST Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

N summed spectra for BURST Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

Overrange flag for BURST Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

Counts based on variable 'epoch_burst' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l2/rfs_burst/2019/psp_fld_l2_rfs_burst_20191226_v02.cdf. The most common cadence occurred for 75.4220% of the 4155 timesteps. Cadence = 218505856 [ns] = PT0.218506S.

PSP FIELDS Level 2 Radio Frequency Spectrometer (RFS) High Frequency Receiver (HFR) Data

PSP FIELDS Radio Frequency Spectrometer (RFS), HFR data.The RFS is the high frequency component  of the FIELDS experiment on the  Parker Solar Probe spacecraft [1].  For a full description of the FIELDS  experiment, see [2].  For a description  of the RFS, see [3].The RFS produces auto and cross spectral data products in two frequency ranges, the LFR (Low Frequency Reciever) range and the HFR (High Frequency Receiver) range.  Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR HiRes spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, and the polyphase filter bank (PFB) and the FFT spectral processing as described in [3].  Corrections for base capacitance and antenna effective length have not been applied (these corrections will be applied in Level 3 RFS data.) Therefore, units for all spectral quantities are given in V^2/Hz.Time resolution of the RFS varies with instrument mode.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for RFS HFR and LFR spectra is typically about 7 seconds.  During cruise mode, which is the default mode for operations outside of 0.25 AU, cadence for HFR and LFR spectra is about 56 seconds.References:1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-62. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-53. Pulupa, M., Bale, S. D., Bonnell, J.W. et al. (2017) JGR Space Physics, 122, 2836-2854. https://doi.org/10.1002/2016JA023345

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_hfr_auto_averages_ch0_V1V2, @1 => epoch_hfr_auto_averages_ch1_V3V4, @2 => epoch_hfr_auto_peaks_ch0_V1V2, @3 => epoch_hfr_auto_peaks_ch1_V3V4, @4 => epoch_hfr_cross_im_V1V2_V3V4, @5 => epoch_hfr_cross_re_V1V2_V3V4, @6 => epoch_hfr_coher_V1V2_V3V4, @7 => epoch_hfr_phase_V1V2_V3V4, @8 => epoch_hfr.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_hfr_auto_averages_ch0_V1V2, @1 => epoch_hfr_auto_averages_ch1_V3V4, @2 => epoch_hfr_auto_peaks_ch0_V1V2, @3 => epoch_hfr_auto_peaks_ch1_V3V4, @4 => epoch_hfr_cross_im_V1V2_V3V4, @5 => epoch_hfr_cross_re_V1V2_V3V4, @6 => epoch_hfr_coher_V1V2_V3V4, @7 => epoch_hfr_phase_V1V2_V3V4, @8 => epoch_hfr.)

Radio Frequency Spectrometer HFR (from all.xml/instrument/description/@short)

N summed spectra for HFR Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

Overrange flag for HFR Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

N summed spectra for HFR Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

Overrange flag for HFR Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

PSP FIELDS Level 2 Radio Frequency Spectrometer (RFS) Low Frequency Receiver (LFR) Data

PSP FIELDS Radio Frequency Spectrometer (RFS), LFR data.The RFS is the high frequency component  of the FIELDS experiment on the  Parker Solar Probe spacecraft [1].  For a full description of the FIELDS  experiment, see [2].  For a description  of the RFS, see [3].The RFS produces auto and cross spectral data products in two frequency ranges, the LFR (Low Frequency Reciever) range and the HFR (High Frequency Receiver) range.  Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR HiRes spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, and the polyphase filter bank (PFB) and the FFT spectral processing as described in [3].  Corrections for base capacitance and antenna effective length have not been applied (these corrections will be applied in Level 3 RFS data.) Therefore, units for all spectral quantities are given in V^2/Hz.Time resolution of the RFS varies with instrument mode.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for RFS HFR and LFR spectra is typically about 7 seconds.  During cruise mode, which is the default mode for operations outside of 0.25 AU, cadence for HFR and LFR spectra is about 56 seconds.References:1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-62. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-53. Pulupa, M., Bale, S. D., Bonnell, J.W. et al. (2017) JGR Space Physics, 122, 2836-2854. https://doi.org/10.1002/2016JA023345

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 13 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_lfr_auto_averages_ch0_V1V2, @1 => epoch_lfr_auto_averages_ch1_V3V4, @2 => epoch_lfr_auto_peaks_ch0_V1V2, @3 => epoch_lfr_auto_peaks_ch1_V3V4, @4 => epoch_lfr_hires_averages_ch0_V1V2, @5 => epoch_lfr_hires_averages_ch1_V3V4, @6 => epoch_lfr_hires_peaks_ch0_V1V2, @7 => epoch_lfr_hires_peaks_ch1_V3V4, @8 => epoch_lfr_cross_im_V1V2_V3V4, @9 => epoch_lfr_cross_re_V1V2_V3V4, @10 => epoch_lfr_coher_V1V2_V3V4, @11 => epoch_lfr_phase_V1V2_V3V4, @12 => epoch_lfr.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 13 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_lfr_auto_averages_ch0_V1V2, @1 => epoch_lfr_auto_averages_ch1_V3V4, @2 => epoch_lfr_auto_peaks_ch0_V1V2, @3 => epoch_lfr_auto_peaks_ch1_V3V4, @4 => epoch_lfr_hires_averages_ch0_V1V2, @5 => epoch_lfr_hires_averages_ch1_V3V4, @6 => epoch_lfr_hires_peaks_ch0_V1V2, @7 => epoch_lfr_hires_peaks_ch1_V3V4, @8 => epoch_lfr_cross_im_V1V2_V3V4, @9 => epoch_lfr_cross_re_V1V2_V3V4, @10 => epoch_lfr_coher_V1V2_V3V4, @11 => epoch_lfr_phase_V1V2_V3V4, @12 => epoch_lfr.)

Radio Frequency Spectrometer LFR (from all.xml/instrument/description/@short)

N summed spectra for LFR Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

Overrange flag for LFR Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4

N summed spectra for LFR Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

Overrange flag for LFR Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => PSP_FLD_L2_TDS_WF_Burst_Time_Series_Times_TT2000_f, @1 => epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => PSP_FLD_L2_TDS_WF_Burst_Time_Series_Times_TT2000_f, @1 => epoch.)

Time Domain Sampler Waveform Bursts (from all.xml/instrument/description/@short)

Science Telemetry Data (from Master/CDFglobalAttributes/Data_type)

Flattened Corrected (UTC-based) absolute time for each of the time series samples (ns)

TDS wave-form burst time series for the high-gain V1 sensor (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain V2 sensor (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain V3 sensor (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain V4 sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain V5 sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain difference of V1-V2 (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain difference of V3-V4 (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain sum of V1+V2+V3+V4 (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series for the high-gain SCM MF sensor (Ch5) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series for the high-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series for the high-gain SCM MF sensor (Ch5) NOT corrected for frequency response (engineering mV)

The TDS wave-form burst time series for SWEAP (Ch0) - the values are positive integers (GE 0) returned as a real from the SWEAP particle count channel (counts)

Corrected UTC time of the start of the collected wave-form burst in TT2000

TDS wave-form burst telemetry format version number. Note: CDF_UINT4 data was converted to HAPI double.

Event number for this burst. Note: CDF_UINT4 data was converted to HAPI double.

Overall quality for this burst (arbitrary units - used for burst selection). Note: CDF_UINT4 data was converted to HAPI double.

Number of samples per channel. Note: CDF_UINT4 data was converted to HAPI double.

Maximum number of samples allowed per channel (always 262,144). Note: CDF_UINT4 data was converted to HAPI double.

The total number of SWEAP particle counts in this TDS wave-form burst time series (Ch0) - the value is a positive integer (GE 0) returned as a real8 from the SWEAP particle counting channel (counts)

The observed SWEAP particle counting rate (Ch0) during this burst (counts per second)

The desired time/location of the burst trigger after the start of the burst (s)

Possibly down-sampled sample period of the TDS samples (seconds/sample)

Indicates the rotational speed of the 1st reaction wheel (revolutions per second)

Indicates the rotational speed of the 2nd reaction wheel (revolutions per second)

Indicates the rotational speed of the 3rd reaction wheel (revolutions per second)

Indicates the rotational speed of the 4th reaction wheel (revolutions per second)

TDS wave-form burst time series peak for the high-gain V1 sensor (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain V2 sensor (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain V3 sensor (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain V4 sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain V5 sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain difference of V1-V2 (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain difference of V3-V4 (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain sum of V1+V2+V3+V4 (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series peak for the high-gain SCM MF sensor (Ch5) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series peak for the low-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series peak for the high-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the high-gain SCM MF sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the low-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the low-gain V1 sensor (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the low-gain V2 sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the low-gain V3 sensor (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the low-gain V4 sensor (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series peak for the low-gain V5 sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain V1 sensor (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain V2 sensor (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain V3 sensor (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain V4 sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain V5 sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain difference of V1-V2 (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain difference of V3-V4 (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain sum of V1+V2+V3+V4 (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series RMS for the high-gain SCM MF sensor (Ch5) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series RMS for the low-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering nT)

TDS wave-form burst time series RMS for the high-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the high-gain SCM MF sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the low-gain SCM MF sensor (Ch4) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the low-gain V1 sensor (Ch3) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the low-gain V2 sensor (Ch5) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the low-gain V3 sensor (Ch1) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the low-gain V4 sensor (Ch2) NOT corrected for frequency response (engineering mV)

TDS wave-form burst time series RMS for the low-gain V5 sensor (Ch4) NOT corrected for frequency response (engineering mV)

Value is the S/C provided distance to the sun at the time of this burst

Database of dust impact detections on Parker Solar Probe via impact plasma clouds detected by the FIELDS instrument, TDS receiver. Each file contains data relevant to (i) individual dust impacts (events), (ii) impact rates (rates), and (ii) ancillary information important for interpreting the dust impact data (spacecraft pointing, position).References:[1] Bale, S.D. et al. "The FIELDS Instrument Suite for Solar Probe Plus. Measuring the Coronal Plasma and Magnetic Field, Plasma Waves and Turbulence, and Radio Signatures of Solar Transients" Space Science Reviews, Volume 204, Issue 1-4, pp. 49-82, December 2016, https://doi.org/10.1007/s11214-016-0244-5[2] Malaspina, D.M. et al. "A dust detection database for the inner heliosphere using the Parker Solar Probe spacecraft", The Astrophysical Journal Supplement Series, Volume 266, Number 2, May 2023, https://doi.org/10.3847/1538-4365/acca75

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => psp_fld_l3_dust_V2_rate_epoch, @1 => psp_fld_l3_dust_V2_event_epoch, @2 => psp_fld_l3_dust_ej2000_pointing_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => psp_fld_l3_dust_V2_rate_epoch, @1 => psp_fld_l3_dust_V2_event_epoch, @2 => psp_fld_l3_dust_ej2000_pointing_epoch.)

Counts based on variable 'psp_fld_l3_dust_V2_rate_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/dust/2018/psp_fld_l3_dust_20181002_v01.cdf. The most common cadence, 28800000000000 [ns] = PT8H, occurred for all 2 timesteps. 

V2 dust impact rate (corrected for wave dead time and under-counting)

Counts based on variable 'psp_fld_l3_dust_V2_event_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/dust/2018/psp_fld_l3_dust_20181002_v01.cdf. The most common cadence, 237677540000 [ns] = PT3M57.67754S, occurred for 6.6667% of the 2 timesteps. 

Counts based on variable 'psp_fld_l3_dust_ej2000_pointing_epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/dust/2018/psp_fld_l3_dust_20181002_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 1439 timesteps. 

PSP FIELDS Level 3 Merged Search Coil and Fluxgate Magnetic Field Waveform

PSP FIELDS Merged Search Coil Magnetometer and Fluxgate Magnetometer (SCaM), SCaM data. Merged SCaM data is composed of SCM and MAG data from the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. The SCM is sampled by the Digital Fields Board (DFB), discussed in ref. [3]. For an overview of FIELDS/MAG calibration see ref. [4].SCaM data consists of continuous time-series data from the SCM and MAG sensors. Merged SCaM data is a Level 3 (l3) product derived from the direct sum of weighted and time corrected l1 MAG and SCM data [4]. The weighting coefficients are designed to optimize the SCaM signal to the integrated instrumental noise floor.The Level 3 SCaM product uses SCM data which has been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter gain/phase response, and (iv) the SCM preamplifier gain/phase response. The SCM data is empirically gain-matched to the MAG, with correction factors included in the metadata [4]. Information on SCM sample rate is provided at a 1 min cadence.The Level 3 SCaM product uses orthogonalized MAG data with spacecraft zero offsets removed. Spacecraft zero offset data, along with the native MAG range and sample-rate meta-data is provided at a 1 minute cadence. The Level 3 SCaM data product in this file may be in spacecraft coordinates (e.g. X,Y,Z), RTN coordinates (R,T,N), or SCM sensor coordinates (U,V,W). For large parts of the PSP mission, anomalous performance of the SCM sensor-X axis (in the U direction) precludes merging in SC or RTN coordinates. In these cases data is only provided for the SCM sensor coordinate system (V,W).References: 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s1121401502116 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s1121401602445 3. Malaspina, D.M., Ergun, R.E., Bolton, M. et al. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA0223444. Bowen, T.A., Bale, S.D., Bonnell, J.W., Dudok DeWit, T. et al. (2020) JGR Space Physics, https://doi.org/10.1029/2020JA027813

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/merged_scam_wf/2018/psp_fld_l3_merged_scam_wf_2018100200_v02.cdf. The most common cadence, 13653248 [ns] = PT0.013653S, occurred for 58.6442% of the 336059 timesteps. 

Merged Search Coil and MAG Waveform (from all.xml/instrument/description/@short)

L3 Magnetic Field from Merged MAG and SCM in SCM sensor (uvw) coordinates

PSP FIELDS Radio Frequency Spectrometer (RFS), HFR data.The RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the RFS, see [3].The RFS produces auto and cross spectral data products in two frequency ranges, the LFR (Low Frequency Receiver) range and the HFR (High Frequency Receiver) range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR HiRes spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 3 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the polyphase filter bank (PFB), and the FFT spectral processing as described in [3]. Instrumental background noise from the preamp and RFS analog section has been removed from the L3 data. Level 3 flux variables are converted from power spectral density using base capacitance and antenna effective length values from [4]. This conversion assumes that the PSP/FIELDS antenna response can be characterized as an ideal short dipole, and the antenna impedance is capacitive. At higher frequencies (above ~7 MHz), the antenna no longer responds as an ideal dipole, and at very high densities, the resistive component of the antenna impedance can result in an impedance that is not purely capacitive. The effects of non-ideal dipole antenna response and non-capacitive impedance are not included in the current version of Level 3 processing.Units for spectral quantities are V^2/Hz and W/m^2/Hz (flux). Flux is computed for cross dipole measurements (V1V2 and V3V4) and for psp_fld_l3_rfs_hfr_PSD_FLUX.The psp_fld_l3_rfs_hfr_PSD_FLUX, psp_fld_l3_rfs_hfr_PSD_SFU, and psp_fld_l3_rfs_hfr_STOKES_V variables incorporate both RFS channels to generate an estimate of power spectral density and circular polarization for radio emission with a source near the Sun. Corrections for spacecraft attitude and antenna non-orthogonality have been applied [5]. The PSD_SFU variable contains the flux from PSD_FLUX, converted to sfu and normalized to a distance of 1 au. These quantities are directly comparable to the equivalently named quantities in the STEREO and Solar Orbiter Level 3 CDF files.Time resolution of the RFS varies with instrument mode. During encounter (when PSP is within 0.25 AU of the Sun), cadence for RFS HFR and LFR spectra is typically about 7 seconds.  During cruise mode, which is the default mode for operations outside of 0.25 AU, cadence for HFR and LFR spectra is about 56 seconds.References:1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-62. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-53. Pulupa, M., Bale, S. D., Bonnell, J.W. et al. (2017) JGR Space Physics, 122, 2836-2854. https://doi.org/10.1002/2016JA0233454. Page, B., Bassett, N., Lecacheux, A. et al. (2022) Astronomy & Astrophysics, 668, A127. https://doi.org/10.1051/0004-6361/2022446215. Lecacheux, A. (2011) in Planetary, Solar and Heliospheric Radio Emissions (PRE VII), 13-36. https://doi.org/10.1553/PRE7s13

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 11 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_hfr_auto_averages_ch0_V1V2, @1 => epoch_hfr_auto_averages_ch1_V3V4, @2 => epoch_hfr_coher_V1V2_V3V4, @3 => epoch_hfr_phase_V1V2_V3V4, @4 => epoch_hfr_position, @5 => epoch_hfr_stokes, @6 => epoch_hfr_auto_peaks_ch0_V1V2, @7 => epoch_hfr_auto_peaks_ch1_V3V4, @8 => epoch_hfr_cross_im_V1V2_V3V4, @9 => epoch_hfr_cross_re_V1V2_V3V4, @10 => epoch_hfr_temperature.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 11 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_hfr_auto_averages_ch0_V1V2, @1 => epoch_hfr_auto_averages_ch1_V3V4, @2 => epoch_hfr_coher_V1V2_V3V4, @3 => epoch_hfr_phase_V1V2_V3V4, @4 => epoch_hfr_position, @5 => epoch_hfr_stokes, @6 => epoch_hfr_auto_peaks_ch0_V1V2, @7 => epoch_hfr_auto_peaks_ch1_V3V4, @8 => epoch_hfr_cross_im_V1V2_V3V4, @9 => epoch_hfr_cross_re_V1V2_V3V4, @10 => epoch_hfr_temperature.)

Counts based on variable 'epoch_hfr_auto_averages_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Unit vector for V1V2 antenna(s) in RTN frame for times when V1V2 spectra were recorded in HFR ch0.

Unit vector for V1V2 antenna(s) in J2000 frame for times when V1V2 spectra were recorded in HFR ch0.

Unit vector for V1V2 antenna(s) in IAU_JUPITER frame for times when V1V2 spectra were recorded in HFR ch0.

Counts based on variable 'epoch_hfr_auto_averages_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Unit vector for V3V4 antenna(s) in RTN frame for times when V3V4 spectra were recorded in HFR ch1.

Unit vector for V3V4 antenna(s) in J2000 frame for times when V3V4 spectra were recorded in HFR ch1.

Unit vector for V3V4 antenna(s) in IAU_JUPITER frame for times when V3V4 spectra were recorded in HFR ch1.

Counts based on variable 'epoch_hfr_coher_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_hfr_phase_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Time for PSP spacecraft position data in several coordinate systems.

Distance from the solar center for PSP spacecraft in units of solar radii (Rs).

Counts based on variable 'epoch_hfr_position' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 100.0000% of the 1439 timesteps. Cadence = 60000000000 [ns] = PT1M.

HFR Flux Density (Stokes I) data, from cross dipole measurements.

Counts based on variable 'epoch_hfr_stokes' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 29.6192% of the 2007 timesteps. Cadence = 6990478280 [ns] = PT6.990478S.

HFR Flux Density (Stokes I) data, from cross dipole measurements, normalized to 1 AU.

HFR Circular Polarization (Stokes V) data, normalized to Stokes I.

Counts based on variable 'epoch_hfr_auto_peaks_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_hfr_auto_peaks_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_hfr_cross_im_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

HFR Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_hfr_cross_re_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 46.9894% of the 3184 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

HFR Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_hfr_temperature' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_hfr/2018/psp_fld_l3_rfs_hfr_20181002_v03.cdf. The most common cadence occurred for 100.0000% of the 1439 timesteps. Cadence = 60000000000 [ns] = PT1M.

PSP FIELDS Radio Frequency Spectrometer (RFS), LFR data.The RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. For a description of the RFS, see [3].The RFS produces auto and cross spectral data products in two frequency ranges, the LFR (Low Frequency Receiver) range and the HFR (High Frequency Receiver) range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR HiRes spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 3 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the polyphase filter bank (PFB), and the FFT spectral processing as described in [3]. Instrumental background noise from the preamp and RFS analog section has been removed from the L3 data. Level 3 flux variables are converted from power spectral density using base capacitance and antenna effective length values from [4]. This conversion assumes that the PSP/FIELDS antenna response can be characterized as an ideal short dipole, and the antenna impedance is capacitive. At higher frequencies (above ~7 MHz), the antenna no longer responds as an ideal dipole, and at very high densities, the resistive component of the antenna impedance can result in an impedance that is not purely capacitive. The effects of non-ideal dipole antenna response and non-capacitive impedance are not included in the current version of Level 3 processing.Units for spectral quantities are V^2/Hz and W/m^2/Hz (flux). Flux is computed for cross dipole measurements (V1V2 and V3V4) and for psp_fld_l3_rfs_lfr_PSD_FLUX.The psp_fld_l3_rfs_lfr_PSD_FLUX, psp_fld_l3_rfs_lfr_PSD_SFU, and psp_fld_l3_rfs_lfr_STOKES_V variables incorporate both RFS channels to generate an estimate of power spectral density and circular polarization for radio emission with a source near the Sun. Corrections for spacecraft attitude and antenna non-orthogonality have been applied [5]. The PSD_SFU variable contains the flux from PSD_FLUX, converted to sfu and normalized to a distance of 1 au. These quantities are directly comparable to the equivalently named quantities in the STEREO and Solar Orbiter Level 3 CDF files.Time resolution of the RFS varies with instrument mode. During encounter (when PSP is within 0.25 AU of the Sun), cadence for RFS HFR and LFR spectra is typically about 7 seconds.  During cruise mode, which is the default mode for operations outside of 0.25 AU, cadence for HFR and LFR spectra is about 56 seconds.References:1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-62. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-53. Pulupa, M., Bale, S. D., Bonnell, J.W. et al. (2017) JGR Space Physics, 122, 2836-2854. https://doi.org/10.1002/2016JA0233454. Page, B., Bassett, N., Lecacheux, A. et al. (2022) Astronomy & Astrophysics, 668, A127. https://doi.org/10.1051/0004-6361/2022446215. Lecacheux, A. (2011) in Planetary, Solar and Heliospheric Radio Emissions (PRE VII), 13-36. https://doi.org/10.1553/PRE7s13

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 15 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_lfr_auto_averages_ch0_V1V2, @1 => epoch_lfr_auto_averages_ch1_V3V4, @2 => epoch_lfr_coher_V1V2_V3V4, @3 => epoch_lfr_phase_V1V2_V3V4, @4 => epoch_lfr_position, @5 => epoch_lfr_stokes, @6 => epoch_lfr_auto_peaks_ch0_V1V2, @7 => epoch_lfr_auto_peaks_ch1_V3V4, @8 => epoch_lfr_hires_averages_ch0_V1V2, @9 => epoch_lfr_hires_averages_ch1_V3V4, @10 => epoch_lfr_hires_peaks_ch0_V1V2, @11 => epoch_lfr_hires_peaks_ch1_V3V4, @12 => epoch_lfr_cross_im_V1V2_V3V4, @13 => epoch_lfr_cross_re_V1V2_V3V4, @14 => epoch_lfr_temperature.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 15 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_lfr_auto_averages_ch0_V1V2, @1 => epoch_lfr_auto_averages_ch1_V3V4, @2 => epoch_lfr_coher_V1V2_V3V4, @3 => epoch_lfr_phase_V1V2_V3V4, @4 => epoch_lfr_position, @5 => epoch_lfr_stokes, @6 => epoch_lfr_auto_peaks_ch0_V1V2, @7 => epoch_lfr_auto_peaks_ch1_V3V4, @8 => epoch_lfr_hires_averages_ch0_V1V2, @9 => epoch_lfr_hires_averages_ch1_V3V4, @10 => epoch_lfr_hires_peaks_ch0_V1V2, @11 => epoch_lfr_hires_peaks_ch1_V3V4, @12 => epoch_lfr_cross_im_V1V2_V3V4, @13 => epoch_lfr_cross_re_V1V2_V3V4, @14 => epoch_lfr_temperature.)

Counts based on variable 'epoch_lfr_auto_averages_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Unit vector for V1V2 antenna(s) in RTN frame for times when V1V2 spectra were recorded in LFR ch0.

Unit vector for V1V2 antenna(s) in J2000 frame for times when V1V2 spectra were recorded in LFR ch0.

Unit vector for V1V2 antenna(s) in IAU_JUPITER frame for times when V1V2 spectra were recorded in LFR ch0.

Counts based on variable 'epoch_lfr_auto_averages_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Unit vector for V3V4 antenna(s) in RTN frame for times when V3V4 spectra were recorded in LFR ch1.

Unit vector for V3V4 antenna(s) in J2000 frame for times when V3V4 spectra were recorded in LFR ch1.

Unit vector for V3V4 antenna(s) in IAU_JUPITER frame for times when V3V4 spectra were recorded in LFR ch1.

Counts based on variable 'epoch_lfr_coher_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_lfr_phase_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_lfr_position' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 100.0000% of the 1439 timesteps. Cadence = 60000000000 [ns] = PT1M.

LFR Flux Density (Stokes I) data, from cross dipole measurements.

Counts based on variable 'epoch_lfr_stokes' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 28.9551% of the 1962 timesteps. Cadence = 6990478280 [ns] = PT6.990478S.

LFR Flux Density (Stokes I) data, from cross dipole measurements, normalized to 1 AU.

LFR Circular Polarization (Stokes V) data, normalized to Stokes I.

Counts based on variable 'epoch_lfr_auto_peaks_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_lfr_auto_peaks_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

Counts based on variable 'epoch_lfr_hires_averages_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

LFR HiRes Auto Spectra, Ch0: V1V2 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_lfr_hires_averages_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

LFR HiRes Auto Spectra, Ch1: V3V4 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_lfr_hires_peaks_ch0_V1V2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

LFR HiRes Peak Spectra, Ch0: V1V2 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_lfr_hires_peaks_ch1_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

LFR HiRes Peak Spectra, Ch1: V3V4 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_lfr_cross_im_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

LFR Cross Spectra Imag Part, Ch0: V1V2 Ch1: V3V4 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_lfr_cross_re_V1V2_V3V4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 44.9380% of the 3045 timesteps. Cadence = 6990478336 [ns] = PT6.990478S.

LFR Cross Spectra Real Part, Ch0: V1V2 Ch1: V3V4 in units of flux density (W/m^2/Hz)

Counts based on variable 'epoch_lfr_temperature' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr/2018/psp_fld_l3_rfs_lfr_20181002_v03.cdf. The most common cadence occurred for 100.0000% of the 1439 timesteps. Cadence = 60000000000 [ns] = PT1M.

PSP FIELDS Level 3 Electron Density Data from Radio Frequency Spectrometer (RFS) Low Frequency Receiver (LFR) Quasi-Thermal Noise (QTN) Spectroscopy

Quasi-thermal noise (QTN) spectroscopy is an efficient tool for measuring in situ macroscopic plasma properties in space, using a passive wave receiver at the ports of an electric antenna [1]. The Radio Frequency Spectrometer (RFS) is a dual channel digital spectrometer, designed for both remote sensing of radio waves and in situ measurement of electrostatic fluctuations using signals from the V1-V4 electric field antennas [2]. Usually, the two RFS channels record differences between V1-V2 and V3-V4 antennas (dipole mode). It allows us to retrieve plasma properties independently by two sets of antennas. The plasma line is automatically identified in a frequency range determined by the density model based on spacecraft distance from the Sun. The frequency range is manually adjusted for intervals when the plasma line occurs at lower or higher frequencies than predicted. We assume that the plasma line is well identified if detected at the same frequency by the V1-V2 and V3-V4 dipoles simultaneously. We assume that the plasma frequency is equal to the geometric mean of the plasma line and the preceding  frequency channel. In other words, the plasma frequency corresponds to the steepest positive slope below the plasma line. The provided error bars are calculated from the frequency resolution of the RFS instrument.[1] Meyer-Vernet, N., Issautier, K., & Moncuquet, M. (2017). Quasi-thermal noise spectroscopy: The art and the practice. Journal of Geophysical Research: Space Physics, 122, 7925-7945. https://doi.org/10.1002/2017ja024449[2] Bale, S. D., Goetz, K., Harvey, P. R., Turin, P., Bonnell, J. W., Dudok de Wit, T., et al. (2016). The FIELDS instrument suite for Solar probe plus. Measuring the coronal plasma and magnetic field, plasma waves and turbulence, and radio signatures of Solar transients. Space Science Reviews, 204(1-4), 49-82. https://doi.org/10.1007/s11214-016-0244-5

This project acknowledges the Parker Solar Probe FIELDS instrument team and the FIELDS science data center for providing these solar wind plasma measurements.

NASA open data policy applies. Consultation with the instrument team is strongly recommended.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/rfs_lfr_qtn/psp_fld_l3_rfs_lfr_qtn_20181019_20181031_v01.cdf. The most common cadence, 6990478720 [ns] = PT6.990479S, occurred for 22.9998% of the 3671 timesteps. 

Solar Wind Electron Density (from Master/CDFglobalAttributes/Data_type)

Lower uncertainty associated with QTN electron density at channel 0

Upper uncertainty associated with QTN electron density at channel 0

Lower uncertainty associated with QTN electron density at channel 1

Upper uncertainty associated with QTN electron density at channel 1

Position vector in HEEQ coordinates (Define Rs = 695700km) (X-component)

Position vector in HEEQ coordinates (Define Rs = 695700km) (Y-component)

Position vector in HEEQ coordinates (Define Rs = 695700km) (Z-component)

Parker Solar Probe FIELDS Level 3 Simplified Quasi-Thermal Noise (SQTN) data, using the Radio Frequency Spectrometer (RFS) spectra when connected to V1V2 dipole antenna

Parker Solar Probe/FIELDS Simplified Quasi-Thermal Noise data (SQTN).The SQTN spectroscopy is a method which allows to deduce the electron density and the core temperature of the plasma surrounding a s/c, by using the power spectra acquired from an electric dipole antenna (see [1] for the PSP case, and references therein).There are two dipoles on the PSP/FIELDS experiment [2] exploitable for the SQTN, named V1V2 and V3V4, which are both connected to the FIELDS Radio Frequency Spectrometer (RFS), see [3].The density is deduced from the plasma frequency (fp) detection algorithm, applied to RFS available spectra, with elimination of questionable detection (or false positive) using QTN theory (see [1]). No fp detection results in filling the data by -1e31 (for all variables provided here). In particular, since we are using 2x2m dipoles on PSP, the fp detection is impossible when the local Debye length is larger than about 5m. On a daily basis, the typical rate of validated detection of fp is more than 90% of the available spectra when PSP is within 0.25 AU of the Sun, but this rate may drop to only 20% at larger distances (0.5 AU being the upper limit used to product this CDF file, which corresponds at most to +/- 15 days around the exact date of the PSP perihelion).When the fp detection is validated, fp errors bars are defined taking into account the RFS_LFR spectral resolution (64 pseudo-logarithmically spaced frequencies in the range of 10 kHz-1.7 MHz), then refined by using QTN theory, and this finally provides the error bars for the density (electron_density_delta). The electron density is then deduced as the most probable value within the error bars, using again QTN theory.Note the electron density provided here is fully independant of antennas calibrations and floating potential, but not the electron core temperature which is deduced from the QTN level below fp (see [1]), so the core temperature will be certainly more subject to future improvments of this CDF file (see version and mods, v00 corresponding to the method exactly as published for the two first encounters/perihelions by PSP in [1]).All variables provided here were not subject to post-processing noise filtering nor any interpolation/smoothing of data.The time resolution of the RFS varies with instrument mode, so does these electron data derived from RFS data.  During encounter (when PSP is within 0.25 AU of the Sun), cadence for RFS HFR and LFR spectra is typically about 7 seconds (and about 3.5 seconds during +/- 3 days around the perihelion date from encounter 06). During cruise mode, which is the default mode for operations outside of 0.25 AU, cadence for HFR and LFR spectra is about 56 seconds.References:1. Moncuquet, M., Meyer-Vernet, N., Issautier, K. et al. (2020), Astrophysical Journal Supplement Series, 246:44. https://doi.org/10.3847/1538-4365/ab5a842. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-53. Pulupa, M., Bale, S. D., Bonnell, J.W. et al. (2017) JGR Space Physics, 122, 2836-2854. https://doi.org/10.1002/2016JA023345

In publications, we recommend to add the following sentence in the acknowledgments:  "The authors acknowledge LESIA (Laboratoire d Etudes Spatiales et Instrumentation en Astrophysique), Observatoire de PARIS, CNRS (Centre National de la Recherche Scientifique) and CNES (Centre National d Etudes Spatiales) for support for production of these data and CDPP (Centre de Donnees de la Physique des Plasmas) for their archiving and provision."

In_situ electron density and core temperature (SQTN from V1V2 dipole of Parker Solar Probe during Encounter 01)

The PSP/FIELDS data provided here are publicly available. We suggest contacting Michel.Moncuquet@obspm.fr (LESIA) when using these data and for any further question. For parents data, see PSP/FIELDS Rules of the Road available at http://fields.ssl.berkeley.edu/rules/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/fields/l3/sqtn_rfs_v1v2/2018/psp_fld_l3_sqtn_rfs_v1v2_20181015_v1.0.cdf. The most common cadence, 55924070784 [ns] = PT55.924071S, occurred for 24.1580% of the 373 timesteps. 

Simplified Quasi-Thermal Noise from V1V2 dipole (from all.xml/instrument/description/@short)

Heliospheric Physics Space Physics (from Master/CDFglobalAttributes/Discipline)

Level 3 data, time series (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/ephemeris/helio1day/psp_helio1day_position_20180813_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 3824 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/ephemeris/helio1hr/psp_helio1hr_position_20180813_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 91799 timesteps. 

EPI-Hi 10 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

PSP IS☉IS Instrument Suite, Rules of the Road, SOC web site, UNH

Parker Solar Probe, PSP, IS☉IS Instrument Suite, Rules of the Road, Spacecraft Operations Center, SOC, web site, Univ. of New Hampshire

PSP IS☉IS Instrument Suite, Energetic Particle Data - User Guide, SOC web site, UNH

Parker Solar Probe, PSP, IS☉IS Instrument Suite, Energetic Particle Data - User Guide, Spacecraft Operations Center, SOC, web site, Univ. of New Hampshire

Parker Solar Probe, PSP, IS☉IS Instrument Suite Description: McComas, D. J. et al., Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation, Space Sci. Rev., 204, 187-256 (2016)

Parker Solar Probe, PSP, IS☉IS Instrument Suite, Spacecraft Operations Center, SOC, web site, Univ. of New Hampshire. This is the official science data host site for the IS☉IS instrument suite and visualization toolkit.

Parker Solar Probe, PSP, FIELDS Instrument Suite, Spacecraft Operations Center, SOC, web site, UC Berkeley. The magnetic field data used for pitch angle calculation of IS☉IS energetic particle data is provided courtesy of the PSP FIELDS team.

Cite as, "McComas et al. (2016)" and contact the ISOIS instrument team before publication. Please do not distribute this file.

Integrated Science Investigation of the Sun, Energetic Particle Instrument Hi (from all.xml/instrument/description/@short)

Level 2 HET 10-second rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi HET 300 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 HET 5-minute rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi HET 3600 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 HET hourly rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi HET 60 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 HET 1-minute rates (from Master/CDFglobalAttributes/Data_type)

Level 2 LET1 10-second rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi LET1 300 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 LET1 5-minute rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi 3600 seconds rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 LET1 hourly rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi LET1 60 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 LET1 1-minute rates (from Master/CDFglobalAttributes/Data_type)

Level 2 LET2 10-second rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi LET2 300 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 LET2 5-minute rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi LET2 3600 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 LET2 hourly rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi LET2 60 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 LET2 1-minute rates (from Master/CDFglobalAttributes/Data_type)

EPI-Hi second rates cdf. Time tags indicate time of collection.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Level 2 one-second rates (from Master/CDFglobalAttributes/Data_type)

EPI-Lo, Ion Composition mode.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_ChanC, @1 => Epoch_ChanD, @2 => Epoch_ChanP, @3 => Epoch_ChanR, @4 => Epoch_ChanT.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_ChanC, @1 => Epoch_ChanD, @2 => Epoch_ChanP, @3 => Epoch_ChanR, @4 => Epoch_ChanT.)

Integrated Science Investigation of the Sun, Energetic Particle Instrument Lo (from all.xml/instrument/description/@short)

EPI-Lo, Particle Energy mode.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_ChanE, @1 => Epoch_ChanF, @2 => Epoch_ChanG.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_ChanE, @1 => Epoch_ChanF, @2 => Epoch_ChanG.)

Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1

Integrated Science Investigation of the Sun (from all.xml/instrument/description/@short)

EPI-Hi HET 3600 second rates cdf. Time tags indicate midpoint of integration.Instrument paper: Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation. McComas, D. J. et al (2016). Space Sci. Rev., doi:10.1007/s11214-014-0059-1EPI-Hi 3600 seconds rates cdf. Time tags indicate midpoint of integration.EPI-Lo, Ion Composition mode.EPI-Lo, Particle Energy mode.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => HET_Epoch, @1 => Epoch, @2 => Epoch_ChanP, @3 => Epoch_ChanE.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => HET_Epoch, @1 => Epoch, @2 => Epoch_ChanP, @3 => Epoch_ChanE.)

Differential Electron Energy Flux for the SPAN-A Electron Instrument

Parker Solar Probe, PSP, SWEAP Data Access web site, Smithsonian Astrophysical Observatory

Parker Solar Probe, PSP, SWEAP Instrument Suite Description: Kasper, J.C., Abiad, R., Austin, G. et al., Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus, Space Scii. Rev., 204, 131–186 (2016)

Parker Solar Probe, PSP, SWEAP home page, Smithsonian Astrophysical Observatory

SPDF/CDAWeb. Please also acknowledge the data producer: Michael L. Stevens at Center for Astrophysics, Harvard and Smithsonian

SPDF/SSCWeb. Please also acknowledge the data producer: Michael L. Stevens at Center for Astrophysics, Harvard and Smithsonian

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Michael L. Stevens at Center for Astrophysics, Harvard and Smithsonian

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l2/spa_sf0_16ax8dx32e/2018/psp_swp_spa_sf0_l2_16ax8dx32e_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.8082% of the 357 timesteps. 

SWEAP generic Sensor Experiment (from all.xml/instrument/description/@short)

Electron Pitch Angle Distribution for the SPAN-Electron instrument

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l3/spa_sf0_pad/2018/psp_swp_spa_sf0_l3_pad_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.8082% of the 357 timesteps. 

Parker Solar Probe/Solar Wind Electrons Alphas and Protons/Solar Probe ANalyzers (from all.xml/instrument/description/@short)

Solar Wind Particle Distributions (from Master/CDFglobalAttributes/Data_type)

Differential Energy Flux vs Energy at Each Pitch Angle (spectrograms)

Differential Energy Flux vs Pitch Angle at Each Energy Level (spectrograms)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l2/spa_sf1_32e/2018/psp_swp_spa_sf1_l2_32e_20181002_v04.cdf. The most common cadence, 1747619840 [ns] = PT1.74762S, occurred for 26.1203% of the 6837 timesteps. 

Electron Differential Energy Flux at each measured energy/deflector step and anode of the SPAN-Electron instrument

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l2/spb_sf0_16ax8dx32e/2018/psp_swp_spb_sf0_l2_16ax8dx32e_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.8215% of the 357 timesteps. 

Electron Pitch Angle Distribution for the SPAN-B Electron Instrument

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l3/spb_sf0_pad/2018/psp_swp_spb_sf0_l3_pad_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.8215% of the 357 timesteps. 

Electron Differential Energy Flux at each measured energy step, and averaged over all deflection steps and anodes of the SPAN-Electron instrument

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l2/spb_sf1_32e/2018/psp_swp_spb_sf1_l2_32e_20181002_v04.cdf. The most common cadence, 1747620096 [ns] = PT1.74762S, occurred for 25.8873% of the 6776 timesteps. 

Solar Probe Cup (SPC) charge flux distributions comprise electrical current as a function of time and energy-per-charge, with appropriate instrument response elements considered and calibrations applied. This is a two SWEAP SPC experiment level 2 (L2) standard data product.

This project acknowledges the Parker Solar Probe SWEAP instrument team and the SWEAP science data center for providing these solar wind plasma measurements.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spc/l2/l2i/2018/psp_swp_spc_l2i_20181031_v01.cdf. The most common cadence, 873820032 [ns] = PT0.87382S, occurred for 34.1889% of the 31835 timesteps. 

Solar Wind Electrons Alphas and Protons / Solar Probe Cup (from all.xml/instrument/description/@short)

Solar Wind Ion Distribution Function (from Master/CDFglobalAttributes/Data_type)

rough estimate angle of the mean flow into the cup, in radians, in SPC coordinates

This file includes the densities, vector velocities, and scalar (radial component) temperatures of the solar wind protons measured by the Solar Probe Cup (SPC). These are determined both by a direct computation of the velocity moments of the reduced distribution function and by attempting to fit the primary peak in the ion I(V) curve with a Maxwellian model.When such fitting is successful, the data set also includes Maxwellian model fits to the alpha-particle (He++) and tertiary (usually proton beam or shoulder) populations.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spc/l3/l3i/2018/psp_swp_spc_l3i_20181031_v01.cdf. The most common cadence, 873820032 [ns] = PT0.87382S, occurred for 34.1889% of the 31835 timesteps. 

Solar Wind Ion velocity moments and fits (from Master/CDFglobalAttributes/Data_type)

Global quality flag, signifying whether the data for this epoch are suitable for use without caveate.

Proton bulk velocity from the 1st moment of the reduced distribution function, in the spacecraft frame (Only Good Quality)

proton bulk velocity moment upper uncertainty in the spacecraft frame

proton bulk velocity moment lower uncertainty in the spacecraft frame

Proton bulk velocity from the 1st moment of the reduced distribution function in [inertial] RTN coordinate system (Only Good Quality)

Proton density estimate from the 0th moment of the reduced distribution function (Only Good Quality)

Proton radial [most probable] thermal speed estimate from the 2nd velocity moment of the reduced distribution function (Only Good Quality)

Primary proton population velocity, from 1-dimensional Maxwellian fitting, in the spacecraft frame (Only Good Quality)

Primary proton population velocity, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (Only Good Quality)

Primary proton population density, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Primary proton population radial [most probable] thermal speed, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Proton bulk velocity, from 1-dimensional Maxwellian fitting, in the spacecraft frame (Only Good Quality)

Proton bulk velocity, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (Only Good Quality)

[Total] proton density, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Proton radial [most probable] thermal speed component, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Alpha particle velocity vector, from 1-dimensional Maxwellian fitting, in the spacecraft frame (Only Good Quality)

Alpha particle velocity vector, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (Only Good Quality)

Alpha particle density, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Alpha particle radial [most probable] thermal speed, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Population 3 velocity vector, from 1-dimensional Maxwellian fitting, in the spacecraft frame (Only Good Quality)

Population 3 velocity vector, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (Only Good Quality)

Population 3 particle density, from 1-dimensional Maxwellian fitting. (Only Good Quality)

Population 3 particle radial [most probable] thermal speed, from 1-dimensional Maxwellian fitting. (Only Good Quality)

PSP Spacecraft position in the Heliocentric Inertial system, in km

PSP Spacecraft velocity in the Heliocentric Inertial system, in km/s

Proton bulk velocity from the 1st moment of the reduced distribution function, in the spacecraft frame (All Qualities)

Proton bulk velocity from the 1st moment of the reduced distribution function in [inertial] RTN coordinate system (All Qualities)

Proton density estimate from the 0th moment of the reduced distribution function (All Qualities)

Proton radial [most probable] thermal speed estimate from the 2nd velocity moment of the reduced distribution function (All Qualities)

Primary proton population velocity, from 1-dimensional Maxwellian fitting, in the spacecraft frame (All Qualities)

Primary proton population velocity, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (All Qualities)

Primary proton population density, from 1-dimensional Maxwellian fitting. (All Qualities)

Primary proton population radial [most probable] thermal speed, from 1-dimensional Maxwellian fitting. (All Qualities)

Proton bulk velocity, from 1-dimensional Maxwellian fitting, in the spacecraft frame (All Qualities)

Proton bulk velocity, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (All Qualities)

[Total] proton density, from 1-dimensional Maxwellian fitting. (All Qualities)

Proton radial [most probable] thermal speed component, from 1-dimensional Maxwellian fitting. (All Qualities)

Alpha particle velocity vector, from 1-dimensional Maxwellian fitting, in the spacecraft frame (All Qualities)

Alpha particle velocity vector, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (All Qualities)

Alpha particle density, from 1-dimensional Maxwellian fitting. (All Qualities)

Alpha particle radial [most probable] thermal speed, from 1-dimensional Maxwellian fitting. (All Qualities)

Population 3 velocity vector, from 1-dimensional Maxwellian fitting, in the spacecraft frame (All Qualities)

Population 3 velocity vector, from 1-dimensional Maxwellian fitting, in the [inertial] RTN frame (All Qualities)

Population 3 particle density, from 1-dimensional Maxwellian fitting. (All Qualities)

Population 3 particle radial [most probable] thermal speed, from 1-dimensional Maxwellian fitting. (All Qualities)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spe/l3/spe_sf0_pad/2018/psp_swp_spe_sf0_l3_pad_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.8082% of the 357 timesteps. 

Proton Differential Energy Flux at each measured energy/deflector step and anode of the SPAN-Ion instrument

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spi/l2/spi_sf00_8dx32ex8a/2018/psp_swp_spi_sf00_l2_8dx32ex8a_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.1362% of the 346 timesteps. 

Partial moments of the Proton distribution function in the SPAN-Ion instrument, PSP spacecraft, and RTN coordinate systems. User should be aware that the full ion distribution is typically NOT in the FOV of the instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spi/l3/spi_sf00_l3_mom/2018/psp_swp_spi_sf00_l3_mom_20181002_v04.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.1362% of the 346 timesteps. 

Partial Moment Velocity in RTN Coordinates and Sun reference frame

Partial moments of the Proton distribution function in the instrument frame of reference. User should be aware that the full ion distribution is typically NOT in the FOV of the instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spi/l3/spi_sf00_mom_inst/2018/psp_swp_spi_sf00_l3_mom_inst_20181002_v03.cdf. The most common cadence, 27962099328 [ns] = PT27.962099S, occurred for 21.1362% of the 346 timesteps. 

Proton-Contaminated Alpha Differential Energy Flux at Each Measured Energy/Deflector Step and Anode of the SPAN-Ion Instrument

Michael D. McManus et al 2022 ApJ 933 43 DOI 10.3847/1538-4357/ac6ba3

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spi/l2/spi_sf01_8dx32ex8a/2018/psp_swp_spi_sf01_l2_8dx32ex8a_20181002_v04.cdf. The most common cadence, 55924138496 [ns] = PT55.924138S, occurred for 21.2714% of the 174 timesteps. 

Partial moments of the Alpha distribution function in the SPAN-Ion instrument, PSP spacecraft, and RTN coordinate systems. User should be aware that the full ion distribution is typically NOT in the FOV of the instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spi/l3/spi_sf0a_l3_mom/2018/psp_swp_spi_sf0a_l3_mom_20181002_v04.cdf. The most common cadence, 55924138496 [ns] = PT55.924138S, occurred for 21.2714% of the 174 timesteps. 

Partial moments of the Alpha distribution function in the instrument frame of reference. User should be aware that the full ion distribution is typically NOT in the FOV of the instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/psp/sweap/spi/l3/spi_sf0a_mom_inst/2018/psp_swp_spi_sf0a_l3_mom_inst_20181002_v03.cdf. The most common cadence, 55924138496 [ns] = PT55.924138S, occurred for 21.7604% of the 178 timesteps. 

High-energy low-time resolution electron fluxes ~0.02-1.0 MeV (with multi-spin accumulations plotted at end of accumulation in sector order)

Current QuickLook and Summary Plots, Instrument Information and All Data

Science Gateway (including Mission Rules of the Road for Data Usage)

SPDF/CDAWeb. Please also acknowledge the data producer: Lou Lanzerotti at New Jersey Institute of Technology

SPDF/SSCWeb. Please also acknowledge the data producer: Lou Lanzerotti at New Jersey Institute of Technology

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Lou Lanzerotti at New Jersey Institute of Technology

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/esrhelt/2012/rbsp-a-rbspice_lev-2_esrhelt_20121113_v1.2.4-00.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 25.7951% of the 146 timesteps. 

Radiation Belt Storm Probe A - RBSP Ion Composition Experiment (from all.xml/observatory/description/@short)

Radiation Belt Storm Probe A - RBSP Ion Composition Experiment (from Master/CDFglobalAttributes/Source_name)

Electron Species Rate High Energy Low Time resolution (from Master/CDFglobalAttributes/Data_type)

Ephemeris Time of the start  of the accumulation for this measurement.

FEDU: Electron flux spectrograms in energy, by telescope in sector order (multi-spin accums plotted at end of accum; T0= ~110 PA, T3= ~all PAs, T5= FEDU background)

---> Quality flag for the measurement for each telescope/channel/timestep. .see PREBM standards for definition

---> The current sector number where each spin is divided into 36 sectors. Note: CDF_UINT4 data was converted to HAPI double.

---> The current spin number of the spacecraft. Note: CDF_UINT4 data was converted to HAPI double.

---> Dipole L value calculated using the SM Reference Frame and taken from the definitive SPICE SPK kernels that are available at the time. 

Low-energy high-time resolution electron fluxes ~0.02-1.0 MeV (with spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/esrleht/2012/rbsp-a-rbspice_lev-2_esrleht_20121113_v1.2.4-00.cdf. The most common cadence, 607000000 [ns] = PT0.607S, occurred for 37.4565% of the 4197 timesteps. 

Electron Species Rate Low Energy High Time resolution (from Master/CDFglobalAttributes/Data_type)

FEDU: Electron flux spectrograms in energy, by telescope in sector order (T0= ~110 PA, T3= ~all PAs, T5= FEDU background)

Diagnostic Data Use only - DO NOT USE FOR SCIENTIFIC PURPOSES. High-energy low-time resolution RBSPICE Ion Energy mode measurement of all particle fluxes (electron/ion)  ~0.05-1.0 MeV (with multi-spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/isrhelt/2012/rbsp-a-rbspice_lev-2_isrhelt_20121028_v1.1.3-01.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 52.5288% of the 3739 timesteps. 

Ion Species Rate High Energy Low Time resolution (from Master/CDFglobalAttributes/Data_type)

FIDU: Ion flux spectrograms in energy, by telescope in sector order (multi-spin accums plotted at end of accum; T0= ~110 PA, T3= ~all PAs, T5= ~70 PA)

TOF x Energy Hydrogen Rates (with spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/tofxeh/2013/rbsp-a-rbspice_lev-2_tofxeh_20130126_v1.2.9-01.cdf. The most common cadence, 906000000 [ns] = PT0.906S, occurred for 76.5584% of the 36317 timesteps. 

Radiation Belt Storm Probe A (from all.xml/observatory/description/@short)

Radiation Belt Storm Probe A (from Master/CDFglobalAttributes/Source_name)

Time of Flight vs Energy Hydrogen (from Master/CDFglobalAttributes/Data_type)

FPDU: Proton flux spectrograms in energy, by telescope in sector order 

TOF x Energy Ion Fluxes 0.02-1 MeV measured at high energy resolution and low time resolution  (with multi-spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/tofxeion/2012/rbsp-a-rbspice_lev-2_tofxeion_20121028_v1.1.6-00.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 52.1776% of the 3714 timesteps. 

TOF x Energy Ion Fluxes (from Master/CDFglobalAttributes/Data_type)

FIDU: Ion flux spectrograms in energy, by telescope in sector order (multi-spin accums plotted at end of accum)

TOF x E non Hydrogen (Helium and Oxygen) Rates ~0.02-1.0 MeV measured at high energy and low time resolution (with spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/tofxenonh/2013/rbsp-a-rbspice_lev-2_tofxenonh_20130126_v1.2.9-01.cdf. The most common cadence, 1812000000 [ns] = PT1.812S, occurred for 55.3504% of the 13128 timesteps. 

TOF x Energy nonH ions (from Master/CDFglobalAttributes/Data_type)

FHeDU: Helium flux spectrograms in energy, by telescope in sector order (multi-spin accums plotted at end of accum)

FODU: Oxygen flux spectrograms in energy, by telescope in sector order (multi-spin accums plotted at end of accum)

High-energy low-time resolution proton and oxygen fluxes from TOF x PH Hydrogen Rates (with multi-spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/tofxphhhelt/2012/rbsp-a-rbspice_lev-2_tofxphhhelt_20121028_v1.1.6-00.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 52.1776% of the 3714 timesteps. 

TOF x PH Proton and Oxygen Fluxes (from Master/CDFglobalAttributes/Data_type)

FPDU: Proton flux spectrograms in energy, by telescope in sector order (multi-spin accums plotted at end of accum)

TOF x Pulse Height Hydrogen and Oxygen Fluxes ~0.01-0.2 MeV measured at low energy resolution and high time resolution (with spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rbspice/tofxphhleht/2013/rbsp-a-rbspice_lev-2_tofxphhleht_20130126_v1.2.9-00.cdf. The most common cadence, 906000000 [ns] = PT0.906S, occurred for 76.5584% of the 36317 timesteps. 

TOF x PH H and O Fluxes (from Master/CDFglobalAttributes/Data_type)

FPDU: Proton flux spectrograms in energy, by telescope in sector order (spin accums plotted at end of accum)

High Energy Low Time resolution electron intensities and pressures sorted by pitch angles

rbspa rbspice high energy res low time res electron energy intensities/pressures sorted by pitch angles.

The RBSPICE instrument was supported under a NASA Contract with the New Jersey Institute of Technology, with subcontracts to The Johns Hopkins University Applied Physics Laboratory and to Fundamental Technologies LLC.

Van Allen Probes Science Gateway for access to Data, Models, Software and Tools for Researchers, Students and the General Public, JHU/APL

Van Allen Probes Science Gateway for access to Data, Models, Software and Tools for Researchers, Students and the General Public at the Applied Physics Laboratory, Johns Hopkins University

Van Allen Probes Science Gateway, Mission Rules of the Road for Data Usage, JHU/APL

Van Allen Probes Science Gateway, Mission Rules of the Road for Data Usage, Applied Physics Laboratory at the Applied Physics Laboratory, Johns Hopkins University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_esrhelt/2012/rbsp-a-rbspice_lev-3-pap_esrhelt_20121113_v1.2.1-03.cdf. The most common cadence, 109204000000 [ns] = PT1M49.204S, occurred for 6.6667% of the 4 timesteps. 

Level 3 by Pitch Angle and Pressure (from all.xml/instrument/description/@short)

High Energy Low Time Electrons (from Master/CDFglobalAttributes/Data_type)

FEDU:  UniDirectional Differential Electron Flux, 20-940 keV, binned by pitch angle in 17 bins (as energy-angle displays)

The Poisson statistical counting percentage error of the measurement for each energy channel and bin calculated as 1/sqrt(Counts)*100.

Quality flag for the measurement for each pitch angle bin/timestep. .see PREBM standards for definition

Calculated Electron perpendicular partial pressure for energies 20Kev-940KeV.  Does not include noisy energy channels.

---> Calculated Electron parallel partial pressure for energies 20Kev-940KeV.  Does not include noisy energy channels.

---> Number Density calculated by integrating the distribution function over energy (20Kev-940KeV) and pitch angle for Electrons. Does not include noisy energy channels.

Pitch Angle and Energy Integrated total intensity of Electrons observed during the spin for energies 20Kev-940KeV. Does not include noisy energy channels.

Omni Directional Total Electron Flux per spin for energies 20Kev-940KeV

---> Observed minimum intensity in the spin for each energy channel

---> Observed maximum intensity in the spin for each energy channel

---> McElqain L value calculated at the Equator (derived from ECT MagEphem data).

---> Roeder's L* value (derived from ECT MagEphem data) for the average pitch angle.

---> Integral invariant for the average pitch angle derived from ECT MagEphem data.

---> Magnetic Local Time of S/C in Centerted Dipole Coordinates derived from ECT MagEphem data.

Low Energy High Time resolution electron intensities and pressures sorted by pitch angles

rbspa rbspice low energy res high time res electron energy intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_esrleht/2012/rbsp-a-rbspice_lev-3-pap_esrleht_20121113_v1.2.1-03.cdf. The most common cadence, 10920000000 [ns] = PT10.92S, occurred for 13.6876% of the 85 timesteps. 

Low Energy High Time Electrons (from Master/CDFglobalAttributes/Data_type)

FEDU:  UniDirectional Differential Electron Flux, 23-430 keV, binned by pitch angle in 17 bins (as energy-angle displays)

Calculated Electron perpendicular partial pressure for energies 23Kev-430KeV.  Does not include noisy energy channels.

---> Calculated Electron parallel partial pressure for energies 23Kev-430KeV.  Does not include noisy energy channels.

---> Number Density calculated by integrating the distribution function over energy (23Kev-430KeV) and pitch angle for Electrons. Does not include noisy energy channels.

Pitch Angle and Energy Integrated total intensity of Electrons observed during the spin for energies 23Kev-430KeV. Does not include noisy energy channels.

Omni Directional Total Electron Flux per spin for energies 23Kev-430KeV

TOF x Energy High Energy Low Time resolution proton intensities and pressures sorted by pitch angles

rbspice high energy res low time res tofxe proton intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxeh/2013/rbsp-a-rbspice_lev-3-pap_tofxeh_20130126_v1.2.4-03.cdf. The most common cadence, 10870000000 [ns] = PT10.87S, occurred for 42.4595% of the 1678 timesteps. 

Time of Flight vs Energy of Hydrogen (from Master/CDFglobalAttributes/Data_type)

FPDU:  UniDirectional Differential Proton Flux, 0.05-0.6 Mev, binned by pitch angle in 17 bins (as energy-angle displays)

Calculated proton perpendicular partial pressure for energies 50Kev-660KeV.  Does not include noisy energy channels.

---> Calculated proton parallel partial pressure for energies 50Kev-660KeV.  Does not include noisy energy channels.

---> Number Density calculated by integrating the distribution function over energy (50Kev-660KeV) and pitch angle for protons. Does not include noisy energy channels.

Pitch Angle and Energy Integrated total intensity of protons observed during the spin for energies 50Kev-660KeV. Does not include noisy energy channels.

Omni Directional Total Proton Flux per spin for energies 40Kev-660KeV

TOF x Energy High Energy Low Time resolution Helium intensities and pressures sorted by pitch angles

rbspice high energy res low time res tofxe helium intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxehe/2015/rbsp-a-rbspice_lev-3-pap_tofxehe_20150115_v2.2.4-01.cdf. The most common cadence, 10946000000 [ns] = PT10.946S, occurred for 54.5030% of the 3032 timesteps. 

Time of Flight vs Energy of Helium (from Master/CDFglobalAttributes/Data_type)

FHeDU:UniDirectional Differential He Flux,  0.06-0.9 MeV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

Calculated Helium perpendicular partial pressure for energies: 60Kev-590KeV.  Does not include noisy energy channels.

Calculated Helium parallel partial pressure for energies: 60Kev-590KeV.  Does not include noisy energy channels.

The Number Density (#/cm^3) calculated by integrating the distribution function over energy (60Kev-590KeV) and pitch angle for Helium. Does not include noisy energy channels.

Pitch Angle Integrated and Energy Integrated total intensity of Helium observed during the spin for energies: 60kev-590keV. Does not include noisy energy channels.

Omni Directional Total Helium Flux per spin for energies: 60keV-590keV (Counts/(MeV-s-cm^2))

---> Observed minimum intensity in the spin for each energy channel measured (60keV-590keV): Counts/(MeV-cm^2-s)

---> Observed maximum intensity in the spin for each energy channel measured (60keV-590keV): Counts/(MeV-cm^2-s)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxehe/2013/rbsp-a-rbspice_lev-3-pap_tofxehe-0_20130126_v2.1.1-01.cdf. The most common cadence, 10870000000 [ns] = PT10.87S, occurred for 42.1053% of the 1664 timesteps. 

FHeDU:UniDirectional Differential He Flux,  0.06-0.6 MeV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

TOF x Energy High Energy Low Time resolution ion intensities and pressures sorted by pitch angles

rbspice high energy res low time res tofxe ion intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxeion/2012/rbsp-a-rbspice_lev-3-pap_tofxeion_20121029_v1.1.1-00.cdf. The most common cadence, 109192000000 [ns] = PT1M49.192S, occurred for 7.2427% of the 57 timesteps. 

Time of Flight vs Energy of Ions (from Master/CDFglobalAttributes/Data_type)

Ephemeris Time of the start of the accumulation for this measurement.

FIDU:  UniDirectional Differential Ion Flux, 0.04-18.5 Mev, binned by pitch angle in 17 bins (as energy-angle displays)

Quality flag for the measurement for each pitch angle bin/timestep. See PREBM standards for definition

Calculated Ion perpendicular partial pressure for energies 48kev-5MeV.  Does not include noisy energy channels.

---> Calculated Ion parallel partial pressure for energies 48kev-5MeV.  Does not include noisy energy channels.

---> Number Density calculated by integrating the distribution function over energy (48kev-5MeV) and pitch angle for Ions. Does not include noisy energy channels.

Pitch Angle and Energy Integrated total intensity of Ions observed during the spin for energies 48kev-5MeV. Does not include noisy energy channels.

Omni Directional Total Ion Flux per spin for energies 21kev-10MeV

TOF x Energy High Energy Low Time resolution Oxygen intensities and pressures sorted by pitch angles

rbspice high energy res low time res tofxe oxygen intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxeo/2015/rbsp-a-rbspice_lev-3-pap_tofxeo_20150115_v2.2.4-01.cdf. The most common cadence, 10946000000 [ns] = PT10.946S, occurred for 54.5030% of the 3032 timesteps. 

Time of Flight vs Energy of Oxygen (from Master/CDFglobalAttributes/Data_type)

FODU:UniDirectional Differential Oxygen Flux,  0.14-0.9 MeV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

Calculated Oxygen perpendicular partial pressure for energies: 125keV-980keV.  Does not include noisy energy channels.

Calculated Oxygen parallel partial pressure for energies: 125keV-980keV.  Does not include noisy energy channels.

The Number Density (#/cm^3) calculated by integrating the distribution function over energy (125kev-980keV) and pitch angle for Oxygen. Does not include noisy energy channels.

Pitch Angle Integrated and Energy Integrated total intensity of Oxygen observed during the spin for energies: 125kev-980keV. Does not include noisy energy channels.

Omni Directional Total Oxygen Flux per spin for energies: 125keV-980keV (Counts/(MeV-s-cm^2))

---> Observed minimum intensity in the spin for each energy channel measured

---> Observed maximum intensity in the spin for each energy channel measured

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxeo/2013/rbsp-a-rbspice_lev-3-pap_tofxeo-0_20130126_v2.1.1-01.cdf. The most common cadence, 10870000000 [ns] = PT10.87S, occurred for 42.1053% of the 1664 timesteps. 

FODU:UniDirectional Differential Oxygen Flux,  0.14-1.1 MeV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

Calculated Oxygen perpendicular partial pressure for energies: 125keV-1260keV.  Does not include noisy energy channels.

Calculated Oxygen parallel partial pressure for energies: 125keV-1260keV.  Does not include noisy energy channels.

The Number Density (#/cm^3) calculated by integrating the distribution function over energy (125keV-1260keV) and pitch angle for Oxygen. Does not include noisy energy channels.

Pitch Angle Integrated and Energy Integrated total intensity of Oxygen observed during the spin for energies: 60kev-590keV. Does not include noisy energy channels.

Omni Directional Total Oxygen Flux per spin for energies: 125keV-1260keV (Counts/(MeV-s-cm^2))

TOF x Pulse Height Energies High Energy Low Time resolution proton intensities and pressures sorted by pitch angles

rbspice high energy res low time res tofxph proton intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxphhhelt/2012/rbsp-a-rbspice_lev-3-pap_tofxphhhelt_20121029_v1.1.1-01.cdf. The most common cadence, 109192000000 [ns] = PT1M49.192S, occurred for 7.2427% of the 57 timesteps. 

Time of Flight vs Proton Energies from Pulse Heights with partial pressures (from Master/CDFglobalAttributes/Data_type)

FPDU:  UniDirectional Differential Proton Flux, 7-51 keV, binned by pitch angle in 17 bins (as energy-angle displays)

Calculated proton perpendicular partial pressure for energies 7keV-51keV.  Does not include noisy energy channels.

---> Calculated proton parallel partial pressure for energies 7keV-51keV.  Does not include noisy energy channels.

---> Number Density calculated by integrating the distribution function over energy (7keV-51keV) and pitch angle for protons. Does not include noisy energy channels.

Pitch Angle and Energy Integrated total intensity of protons observed during the spin for energies 7keV-51keV. Does not include noisy energy channels.

Omni Directional Total Proton Flux per spin for energies 7keV-51keV

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxphhleht/2013/rbsp-a-rbspice_lev-3-pap_tofxphhleht_20130126_v1.2.4-03.cdf. The most common cadence, 10870000000 [ns] = PT10.87S, occurred for 42.4595% of the 1678 timesteps. 

Calculated proton perpendicular partial pressure for energies 7keV-100keV.  Does not include noisy energy channels.

---> Calculated proton parallel partial pressure for energies 7keV-100keV.  Does not include noisy energy channels.

---> Number Density calculated by integrating the distribution function over energy (7keV-100keV) and pitch angle for protons. Does not include noisy energy channels.

Pitch Angle and Energy Integrated total intensity of protons observed during the spin for energies 7keV-100keV. Does not include noisy energy channels.

Omni Directional Total Proton Flux per spin for energies 7keV-100keV

TOF x Pulse Height Energies High Energy Low Time resolution Oxygen intensities and pressures sorted by pitch angles

rbspice high energy res low time res tofxph oxygen intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxphohelt/2012/rbsp-a-rbspice_lev-3-pap_tofxphohelt_20121029_v1.2.4-03.cdf. The most common cadence, 109192000000 [ns] = PT1M49.192S, occurred for 7.2427% of the 57 timesteps. 

Time of Flight vs Pulse Height Energy of Oxygen Intensities/Pressures (from Master/CDFglobalAttributes/Data_type)

FODU:UniDirectional Differential Oxygen Flux,  49-177 keV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

Calculated Oxygen perpendicular partial pressure for energies: 49-177keV.  Does not include noisy energy channels.

Calculated Oxygen parallel partial pressure for energies: 49-177keV.  Does not include noisy energy channels.

The Number Density (#/cm^3) calculated by integrating the distribution function over energy (49-177keV) and pitch angle for Oxygen. Does not include noisy energy channels.

Pitch Angle Integrated and Energy Integrated total intensity of Oxygen observed during the spin for energies: 49-177keV. Does not include noisy energy channels.

Omni Directional Total Oxygen Flux per spin for energies: 49-177keV (Counts/(MeV-s-cm^2))

TOF x Pulse Height Energies Low Energy High Time resolution Oxygen intensities and pressures sorted by pitch angles

rbspice low energy res high time res tofxph oxygen intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/pap_tofxpholeht/2013/rbsp-a-rbspice_lev-3-pap_tofxpholeht_20130126_v1.2.4-03.cdf. The most common cadence, 10870000000 [ns] = PT10.87S, occurred for 42.4595% of the 1678 timesteps. 

FODU:UniDirectional Differential Oxygen Flux,  49-161 keV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

Calculated Oxygen perpendicular partial pressure for energies: 49-161keV.  Does not include noisy energy channels.

Calculated Oxygen parallel partial pressure for energies: 49-161keVkeV.  Does not include noisy energy channels.

The Number Density (#/cm^3) calculated by integrating the distribution function over energy (49-161keVkeV) and pitch angle for Oxygen. Does not include noisy energy channels.

Pitch Angle Integrated and Energy Integrated total intensity of Oxygen observed during the spin for energies: 49-161keV. Does not include noisy energy channels.

Omni Directional Total Oxygen Flux per spin for energies: 49-161keV (Counts/(MeV-s-cm^2))

---> Observed minimum intensity in the spin for each energy channel measured (49-161keV): Counts/(MeV-cm^2-s)

---> Observed maximum intensity in the spin for each energy channel measured (49-161keV): Counts/(MeV-cm^2-s)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/esrhelt/2012/rbsp-a-rbspice_lev-3_esrhelt_20121113_v1.1.9-03.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 25.7951% of the 146 timesteps. 

---> The Second Invariant ( I*sqrt(Bm) ) for the average pitch angle derived from ECT MagEphem data.

The pitch angle based upon the look direction of each telescope, alpha=cos-1(B*(-look))

---> A flag describing the Quality of the Pitch Angle as calculated, 0=good, 1=bad.

The particle velocity unit vector for each telescope look direction (i.e. the negative of the telescope look direction unit vector). (No CDAWeb Plotting)

Roeder's L* value (derived from ECT MagEphem data) for each of the telescopes based upon the telescope pitch angle.

---> The Integral invariant for the pitch angle of each telescope derived from ECT MagEphem data.

---> Second Invariant ( I*sqrt(Bm) ) for the pitch angle of each telescope derived from ECT MagEphem data.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/esrleht/2012/rbsp-a-rbspice_lev-3_esrleht_20121113_v1.1.9-03.cdf. The most common cadence, 607000000 [ns] = PT0.607S, occurred for 37.4565% of the 4197 timesteps. 

Diagnostic Data Use only - DO NOT USE FOR SCIENTIFIC PURPOSES. High-energy low-time resolution RBSPICE Ion Energy mode measurement with pitch angles of all particle fluxes (electron/ion)  ~0.05-1.0 MeV (with multi-spin accumulations plotted at end of accumulation in sector order)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/isrhelt/2012/rbsp-a-rbspice_lev-3_isrhelt_20121029_v1.1.9-00.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 55.0295% of the 3917 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/tofxeh/2013/rbsp-a-rbspice_lev-3_tofxeh_20130126_v1.1.12-01.cdf. The most common cadence, 906000000 [ns] = PT0.906S, occurred for 76.5584% of the 36317 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/tofxeion/2012/rbsp-a-rbspice_lev-3_tofxeion_20121029_v1.1.12-02.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 55.3386% of the 3939 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/tofxenonh/2013/rbsp-a-rbspice_lev-3_tofxenonh_20130126_v1.1.12-01.cdf. The most common cadence, 1812000000 [ns] = PT1.812S, occurred for 55.3504% of the 13128 timesteps. 

TOF by Energy nonH ions (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/tofxphhhelt/2012/rbsp-a-rbspice_lev-3_tofxphhhelt_20121029_v1.1.12-02.cdf. The most common cadence, 1213000000 [ns] = PT1.213S, occurred for 55.3386% of the 3939 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/rbspice/tofxphhleht/2013/rbsp-a-rbspice_lev-3_tofxphhleht_20130126_v1.1.12-01.cdf. The most common cadence, 906000000 [ns] = PT0.906S, occurred for 76.5584% of the 36317 timesteps. 

The particle velocity unit vector for each telescope look direction (i.e. the negative of the telescope look direction unit vector).

1-second density and other parameters inferred by digitizing the trace on the spectrograms.

Density and other parameters inferred by digitizing the trace on the spectrograms.

Electron densities inferred from plasma wave
                spectra obtained by the Waves instrument
                on Van Allen Probes, W. S. Kurth, S. De Pascuale, J. B. Faden, C. A. Kletzing, G. B. Hospodarsky, S. Thaller, and J. R. Wygant, published in JGR

This paper details how electron density was inferred primarily from the upper hybrid resonance frequency.

data access (including advanced Autoplot graphics for data files

Van Allen Probes Electric and Magnetic Field Instrument Suite and Integrated Science, EMFISIS, Home Page at the University of Iowa

Van Allen Probes EMFISIS Web Page with Mission and Instrument Team Links, UI

Van Allen Probes Electric and Magnetic Field Instrument Suite and Integrated Science, EMFISIS, Web Page with Mission and Instrument Team Links at the University of Iowa

Van Allen Probes Electric and Magnetic Field Instrument Suite and Integrated Science, EMFISIS, Data Access including advanced Autoplot Graphics with Links to the Data Use Policy and Magnetometer Release Notes at the University of Iowa

SPDF/CDAWeb. Please also acknowledge the data producer: Craig Kletzing at University of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: Craig Kletzing at University of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Craig Kletzing at University of Iowa

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l4/emfisis/density/2012/rbsp-a_density_emfisis-l4_20120915_v1.5.16.cdf. The most common cadence, 6000000000 [ns] = PT6S, occurred for 97.7452% of the 11271 timesteps. 

Electric and Magnetic Field Instrument Suite and Integrated Science (from all.xml/instrument/description/@short)

Ratio of electron plasma oscillation (wpe) to cyclotron gyration (wce)

Current EMFISIS/MAG Issues, Caveats and Production Release Notes

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/hfr/spectra-burst/2012/rbsp-a_hfr-spectra-burst_emfisis-l2_20120901_v1.2.6.cdf. The most common cadence, 499999940 [ns] = PT0.5S, occurred for 37.6394% of the 1215 timesteps. 

Electric and Magnetic Field Instrument Level 2 (from all.xml/instrument/description/@short)

HFR Spectra from burst data (from Master/CDFglobalAttributes/Data_type)

---> HFR receiver Antenna Select (0 - U axis,1 - V axis,2 - W axis {spin axis})

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/hfr/spectra-merged/2012/rbsp-a_hfr-spectra-merged_emfisis-l2_20120902_v1.2.11.cdf. The most common cadence, 5999999046 [ns] = PT5.999999S, occurred for 31.3563% of the 4515 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/hfr/spectra/2012/rbsp-a_hfr-spectra_emfisis-l2_20120830_v1.2.7.cdf. The most common cadence, 6000000000 [ns] = PT6S, occurred for 15.3595% of the 141 timesteps. 

High Frequency Receiver (HFR) Field Waveform Samples in V/m (Selectable between the U, V and W Axes)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_expanded.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_expanded.)

Radiation Belt Storm Probes A (from all.xml/observatory/description/@short)

Radiation Belt Storm Probes A (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/hfr/waveform/2012/rbsp-a_hfr-waveform_emfisis-l2_20120901_v1.2.9.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 20.8835% of the 52 timesteps. 

Attenuator select indicator for U and V axis.  0-Off, 1-On.   Switches in a 19 dB attenuator.  

---> Axis channel indicator for the HFR.  0-U axis, 1-V axis, 2-W axis.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/1sec/gei/2012/rbsp-a_magnetometer_1sec-gei_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 80.4454% of the 3143 timesteps. 

Electric and Magnetic Field Instrument (from all.xml/instrument/description/@short)

Latitude (angle delta) of the field vector (where (0,0) is the positive Bx direction)

Longitude (angle lambda) of the field vector (where (0,0) is the positive Bx direction)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/1sec/geo/2012/rbsp-a_magnetometer_1sec-geo_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 80.4454% of the 3143 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/1sec/gse/2012/rbsp-a_magnetometer_1sec-gse_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 80.4454% of the 3143 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/1sec/gsm/2012/rbsp-a_magnetometer_1sec-gsm_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 80.4454% of the 3143 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/1sec/sm/2012/rbsp-a_magnetometer_1sec-sm_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 80.4454% of the 3143 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/4sec/gei/2012/rbsp-a_magnetometer_4sec-gei_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 24.0779% of the 235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/4sec/geo/2012/rbsp-a_magnetometer_4sec-geo_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 24.0779% of the 235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/4sec/gse/2012/rbsp-a_magnetometer_4sec-gse_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 24.0779% of the 235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/4sec/gsm/2012/rbsp-a_magnetometer_4sec-gsm_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 24.0779% of the 235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/4sec/sm/2012/rbsp-a_magnetometer_4sec-sm_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 24.0779% of the 235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/hires/gei/2012/rbsp-a_magnetometer_hires-gei_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6142% of the 249146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/hires/geo/2012/rbsp-a_magnetometer_hires-geo_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6142% of the 249146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/hires/gse/2012/rbsp-a_magnetometer_hires-gse_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6142% of the 249146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/hires/gsm/2012/rbsp-a_magnetometer_hires-gsm_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6142% of the 249146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/emfisis/magnetometer/hires/sm/2012/rbsp-a_magnetometer_hires-sm_emfisis-l3_20120830_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6142% of the 249146 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/magnetometer/uvw/2012/rbsp-a_magnetometer_uvw_emfisis-l2_20120830_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6142% of the 249146 timesteps. 

WaveForm Receiver (WFR) Spectral Matrix ~5-10,000 Hz (Merged, Diagonal Elements Only)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/wfr/spectral-matrix-diagonal-merged/2012/rbsp-a_wfr-spectral-matrix-diagonal-merged_emfisis-l2_20120901_v1.2.9.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 21.1464% of the 3346 timesteps. 

wfr-spectral-matrix-diagonal (from Master/CDFglobalAttributes/Data_type)

Diagonal Elements Only (from Master/CDFglobalAttributes/Data_type)

WaveForm Receiver (WFR) Spectral Matrix ~5-10000 Hz (Diagonal Elements Only)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/wfr/spectral-matrix-diagonal/2012/rbsp-a_wfr-spectral-matrix-diagonal_emfisis-l2_20120830_v1.2.5.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 21.7797% of the 700 timesteps. 

WFR-spectral-matrix-diagonal (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/wfr/spectral-matrix/2012/rbsp-a_wfr-spectral-matrix_emfisis-l2_20120830_v1.2.5.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 21.7797% of the 700 timesteps. 

Electric and Magnetic Field Instrument Suite Level 2 (from all.xml/instrument/description/@short)

WFR Full Spectral Matrix (from Master/CDFglobalAttributes/Data_type)

WaveForm Receiver (WFR) Three Axis Electric Field (EU, EV, EW) and Three Axis Magnetic field (BU, BV, BW)  continuous burst waveforms @ 35 kS/sec

Three Axis Electric Field (EU, EV, EW) and Three Axis Magnetic field (BU, BV, BW)  continuous burst waveforms208896 samples @ 35 kS/sec.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/wfr/waveform-continuous-burst/2012/rbsp-a_wfr-waveform-continuous-burst_emfisis-l2_20120901t22_v1.2.5.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 31.3725% of the 16 timesteps. 

WFR Three Axis Electric Field (EU, EV, EW) and Three Axis Magnetic field (BU, BV, BW)  waveforms as 16384 samples @ 35 kS/sec

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/emfisis/wfr/waveform/2012/rbsp-a_wfr-waveform_emfisis-l2_20120830_v1.2.4.cdf. The most common cadence, 299997854769 [ns] = PT4M59.997855S, occurred for 18.1818% of the 2 timesteps. 

Probes-A EMFISIS wave normal angle products and sheath corrected electric field level Level-4

Wave Normal Analysis products, based on L1 spectral matrix survey E and B data, and produced via PRASSADCO (Santolik, et al., Radio Sci., 38(1), 1010, 2003). A correction for antenna sheath effects has been applied to the electric field data, before being input to PRASSADCO. The correction is density-dependent, so fill values are inserted for E-dependent data where a density estimate is not available. Be aware that the spin-plane E antennas began deployment at 2012-09-13T19:44, and were not fully deployed until 2012-09-22T19:48. The spin-axis deployment began on 2012-09-24T17:59 and did not fully complete until 2012-12-07T04:41. Noise levels in the E data are increased by incomplete antenna deployment. There was a significant upgrade to the onboard calibration tables, for both E and B in Feb 2013. Prior to this, the highest survey frequency bin (11.24 kHz) used a flawed cal value that resulted in both amplitude and phase errors. The effect is stronger for the B data. New, corrected, tables took effect at 2013-02-12T04:30:00. In Mar 2013, there was a ~2-day interval where a software issue resulted in the wrong calibration tables being used for both E and B data. These data should be used with extreme caution. The interval is 2013-03-21T06:53:00 to 2013-03-23T05:46:00.

Hartley, D. P., Christopher, I. W., Kletzing, C. A., Kurth, W. S., Santolik, O., Kolmasova, I., et al. (2023). Chorus wave properties from Van Allen Probes: Quantifying the impact of the sheath corrected electric field. Geophysical Research Letters, 50, e2023GL102922.

Demonstriating the use of sheath corrected e-field in poliarization analysis

Kletzing, C.A., Bortnik, J., Hospodarsky, G. et al. The Electric and Magnetic Fields Instrument Suite and Integrated Science (EMFISIS): Science, Data, and Usage Best Practices. Space Sci Rev 219, 28 (2023).

Kletzing, C.A., Kurth, W.S., Acuna, M. et al. The Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) on RBSP. Space Sci Rev 179, 127–181 (2013).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l4/emfisis/wna-survey-sheath-corrected-e/2012/rbsp-a_wna-survey-sheath-corrected-e_emfisis-l4_20120831_v2.0.1.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 35.3322% of the 4861 timesteps. 

Sum of Two Perpendicular Electric Power Spectral Densities Using Faraday Law

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l4/emfisis/wna-survey/2012/rbsp-a_wna-survey_emfisis-l4_20120831_v2.0.1.cdf. The most common cadence, 5999999106 [ns] = PT5.999999S, occurred for 35.3322% of the 4861 timesteps.

Wave Normal Analysis (from Master/CDFglobalAttributes/Data_type)

Current QuickLook & Summary Plots, Instrument Information and All Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/esrhelt/2012/rbsp-b-rbspice_lev-2_esrhelt_20121202_v1.2.4-00.cdf. The most common cadence, 1822000000 [ns] = PT1.822S, occurred for 47.5229% of the 2235 timesteps. 

Radiation Belt Storm Probe B - RBSP Ion Composition Experiment (from all.xml/observatory/description/@short)

Radiation Belt Storm Probe B - RBSP Ion Composition Experiment (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/esrleht/2012/rbsp-b-rbspice_lev-2_esrleht_20121202_v1.2.4-00.cdf. The most common cadence, 911000000 [ns] = PT0.911S, occurred for 46.6770% of the 11090 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/isrhelt/2012/rbsp-b-rbspice_lev-2_isrhelt_20121029_v1.2.4-01.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 67.5211% of the 4794 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/tofxeh/2012/rbsp-b-rbspice_lev-2_tofxeh_20121114_v1.2.9-01.cdf. The most common cadence, 608000000 [ns] = PT0.608S, occurred for 58.0667% of the 24100 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/tofxeion/2012/rbsp-b-rbspice_lev-2_tofxeion_20121029_v1.2.9-01.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 67.4507% of the 4789 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/tofxenonh/2012/rbsp-b-rbspice_lev-2_tofxenonh_20121114_v1.2.9-01.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 58.9582% of the 12235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/tofxphhhelt/2012/rbsp-b-rbspice_lev-2_tofxphhhelt_20121029_v1.2.9-00.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 67.4507% of the 4789 timesteps. 

Radiation Belt Storm Probe B (from all.xml/observatory/description/@short)

Radiation Belt Storm Probe B (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rbspice/tofxphhleht/2012/rbsp-b-rbspice_lev-2_tofxphhleht_20121202_v1.2.9-00.cdf. The most common cadence, 911000000 [ns] = PT0.911S, occurred for 78.9414% of the 55439 timesteps. 

rbspb rbspice high energy res low time res electron energy intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_esrhelt/2012/rbsp-b-rbspice_lev-3-pap_esrhelt_20121202_v1.1.1-02.cdf. The most common cadence, 109345000000 [ns] = PT1M49.345S, occurred for 13.2124% of the 102 timesteps. 

rbspb rbspice low energy res high time res electron energy intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_esrleht/2012/rbsp-b-rbspice_lev-3-pap_esrleht_20121202_v1.2.1-03.cdf. The most common cadence, 10935000000 [ns] = PT10.935S, occurred for 15.7735% of the 312 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxeh/2012/rbsp-b-rbspice_lev-3-pap_tofxeh_20121114_v1.2.4-05.cdf. The most common cadence, 10938000000 [ns] = PT10.938S, occurred for 37.1528% of the 856 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxehe/2012/rbsp-b-rbspice_lev-3-pap_tofxehe_20121115_v2.1.1-02.cdf. The most common cadence, 10938000000 [ns] = PT10.938S, occurred for 23.4132% of the 1848 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxehe/2012/rbsp-b-rbspice_lev-3-pap_tofxehe-0_20121114_v2.1.1-01.cdf. The most common cadence, 10938000000 [ns] = PT10.938S, occurred for 36.6753% of the 845 timesteps. 

rbspice high energy res low time res tofxeion ion intensities/pressures sorted by pitch angles.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxeion/2012/rbsp-b-rbspice_lev-3-pap_tofxeion_20121029_v1.1.1-00.cdf. The most common cadence, 109344000000 [ns] = PT1M49.344S, occurred for 10.3268% of the 79 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxeo/2015/rbsp-b-rbspice_lev-3-pap_tofxeo_20150115_v2.2.4-01.cdf. The most common cadence, 10819000000 [ns] = PT10.819S, occurred for 34.3807% of the 2276 timesteps. 

FODU:UniDirectional Differential Oxygen Flux,  0.06-0.9 MeV, one record per spin binned by pitch angle in 17 bins  (as energy-angle displays)

The Number Density (#/cm^3) calculated by integrating the distribution function over energy (125keV-980keV) and pitch angle for Oxygen. Does not include noisy energy channels.

Pitch Angle Integrated and Energy Integrated total intensity of Oxygen observed during the spin for energies: 125keV-980keV. Does not include noisy energy channels.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxeo/2012/rbsp-b-rbspice_lev-3-pap_tofxeo-0_20121114_v2.1.1-01.cdf. The most common cadence, 10938000000 [ns] = PT10.938S, occurred for 36.6753% of the 845 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxphhhelt/2012/rbsp-b-rbspice_lev-3-pap_tofxphhhelt_20121029_v1.2.4-05.cdf. The most common cadence, 109344000000 [ns] = PT1M49.344S, occurred for 10.3268% of the 79 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxphhleht/2012/rbsp-b-rbspice_lev-3-pap_tofxphhleht_20121202_v1.2.4-01.cdf. The most common cadence, 10934000000 [ns] = PT10.934S, occurred for 35.8742% of the 2099 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxphohelt/2012/rbsp-b-rbspice_lev-3-pap_tofxphohelt_20121029_v1.2.4-02.cdf. The most common cadence, 109344000000 [ns] = PT1M49.344S, occurred for 10.3268% of the 79 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/pap_tofxpholeht/2012/rbsp-b-rbspice_lev-3-pap_tofxpholeht_20121202_v1.2.4-01.cdf. The most common cadence, 10934000000 [ns] = PT10.934S, occurred for 35.8742% of the 2099 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/esrhelt/2012/rbsp-b-rbspice_lev-3_esrhelt_20121202_v1.1.9-03.cdf. The most common cadence, 1822000000 [ns] = PT1.822S, occurred for 47.5229% of the 2235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/esrleht/2012/rbsp-b-rbspice_lev-3_esrleht_20121202_v1.1.9-03.cdf. The most common cadence, 911000000 [ns] = PT0.911S, occurred for 46.6770% of the 11090 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/isrhelt/2012/rbsp-b-rbspice_lev-3_isrhelt_20121029_v1.1.7-02.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 67.5211% of the 4794 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/tofxeh/2012/rbsp-b-rbspice_lev-3_tofxeh_20121114_v1.1.12-00.cdf. The most common cadence, 608000000 [ns] = PT0.608S, occurred for 58.0667% of the 24100 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/tofxeion/2012/rbsp-b-rbspice_lev-3_tofxeion_20121029_v1.1.12-00.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 67.4507% of the 4789 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/tofxenonh/2012/rbsp-b-rbspice_lev-3_tofxenonh_20121114_v1.1.12-00.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 58.9582% of the 12235 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/tofxphhhelt/2012/rbsp-b-rbspice_lev-3_tofxphhhelt_20121029_v1.1.12-00.cdf. The most common cadence, 1215000000 [ns] = PT1.215S, occurred for 67.4507% of the 4789 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/rbspice/tofxphhleht/2012/rbsp-b-rbspice_lev-3_tofxphhleht_20121202_v1.1.12-00.cdf. The most common cadence, 911000000 [ns] = PT0.911S, occurred for 78.9414% of the 55439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l4/emfisis/density/2012/rbsp-b_density_emfisis-l4_20120915_v1.5.15.cdf. The most common cadence, 6000000000 [ns] = PT6S, occurred for 97.6880% of the 11239 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/hfr/spectra-burst/2012/rbsp-b_hfr-spectra-burst_emfisis-l2_20120903_v1.2.3.cdf. The most common cadence, 499999762 [ns] = PT0.5S, occurred for 41.2324% of the 1345 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/hfr/spectra-merged/2012/rbsp-b_hfr-spectra-merged_emfisis-l2_20120901_v1.2.3.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 26.2219% of the 3616 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/hfr/spectra/2012/rbsp-b_hfr-spectra_emfisis-l2_20120901_v1.2.3.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 26.2219% of the 3616 timesteps. 

Radiation Belt Storm Probes B (from all.xml/observatory/description/@short)

Radiation Belt Storm Probes B (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/hfr/waveform/2012/rbsp-b_hfr-waveform_emfisis-l2_20120901_v1.2.2.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 30.7453% of the 99 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/1sec/gei/2012/rbsp-b_magnetometer_1sec-gei_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 74.6652% of the 64507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/1sec/geo/2012/rbsp-b_magnetometer_1sec-geo_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 74.6652% of the 64507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/1sec/gse/2012/rbsp-b_magnetometer_1sec-gse_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 74.6652% of the 64507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/1sec/gsm/2012/rbsp-b_magnetometer_1sec-gsm_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 74.6652% of the 64507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/1sec/sm/2012/rbsp-b_magnetometer_1sec-sm_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 74.6652% of the 64507 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/4sec/gei/2012/rbsp-b_magnetometer_4sec-gei_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 3999998000 [ns] = PT3.999998S, occurred for 22.0391% of the 4760 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/4sec/geo/2012/rbsp-b_magnetometer_4sec-geo_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 3999998000 [ns] = PT3.999998S, occurred for 22.0391% of the 4760 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/4sec/gse/2012/rbsp-b_magnetometer_4sec-gse_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 3999998000 [ns] = PT3.999998S, occurred for 22.0391% of the 4760 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/4sec/gsm/2012/rbsp-b_magnetometer_4sec-gsm_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 3999998000 [ns] = PT3.999998S, occurred for 22.0391% of the 4760 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/4sec/sm/2012/rbsp-b_magnetometer_4sec-sm_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 3999998000 [ns] = PT3.999998S, occurred for 22.0391% of the 4760 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/hires/gei/2012/rbsp-b_magnetometer_hires-gei_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.5169% of the 5502628 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/hires/geo/2012/rbsp-b_magnetometer_hires-geo_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.5169% of the 5502628 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/hires/gse/2012/rbsp-b_magnetometer_hires-gse_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.5169% of the 5502628 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/hires/gsm/2012/rbsp-b_magnetometer_hires-gsm_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.5169% of the 5502628 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/emfisis/magnetometer/hires/sm/2012/rbsp-b_magnetometer_hires-sm_emfisis-l3_20120901_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.5169% of the 5502628 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/magnetometer/uvw/2012/rbsp-b_magnetometer_uvw_emfisis-l2_20120831_v1.7.1.cdf. The most common cadence, 15625000 [ns] = PT0.015625S, occurred for 99.6603% of the 5163074 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/wfr/spectral-matrix-diagonal-merged/2012/rbsp-b_wfr-spectral-matrix-diagonal-merged_emfisis-l2_20120901_v1.2.2.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 26.7189% of the 3684 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/wfr/spectral-matrix-diagonal/2012/rbsp-b_wfr-spectral-matrix-diagonal_emfisis-l2_20120901_v1.2.2.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 26.7189% of the 3684 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/wfr/spectral-matrix/2012/rbsp-b_wfr-spectral-matrix_emfisis-l2_20120901_v1.2.2.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 26.7189% of the 3684 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/wfr/waveform-continuous-burst/2012/rbsp-b_wfr-waveform-continuous-burst_emfisis-l2_20120902t20_v1.2.4.cdf. The most common cadence, 5999997258 [ns] = PT5.999997S, occurred for 38.0952% of the 16 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/emfisis/wfr/waveform/2012/rbsp-b_wfr-waveform_emfisis-l2_20120901_v1.2.2.cdf. The most common cadence, 899994217515 [ns] = PT14M59.994218S, occurred for 5.9322% of the 7 timesteps. 

Probes-B EMFISIS wave normal angle products and sheath corrected electric field Level-4

Wave Normal Analysis products, based on L1 spectral matrix survey E and B data, and produced via PRASSADCO (Santolik, et al., Radio Sci., 38(1), 1010, 2003). A correction for antenna sheath effects has been applied to the electric field data, before being input to PRASSADCO. The correction is density-dependent, so fill values are inserted for E-dependent data where a density estimate is not available. Be aware that the spin-plane E antennas began deployment at 2012-09-13T23:06, and were not fully deployed until 2012-09-22T22:32. The spin-axis deployment began on 2012-09-24T20:33 and did not fully complete until 2012-12-07T17:25. Noise levels in the E data are increased by incomplete antenna deployment. There was a significant upgrade to the onboard calibration tables, for both E and B in Feb 2013. Prior to this, the highest survey frequency bin (11.24 kHz) used a flawed cal value that resulted in both amplitude and phase errors. The effect is stronger for the B data. New, corrected, tables took effect at 2013-02-13T01:48:00. In Mar 2013, there was a ~2-day interval where a software issue resulted in the wrong calibration tables being used for both E and B data. These data should be used with extreme caution. The interval is 2013-03-21T09:35:00 to 2013-03-23T02:07:00.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l4/emfisis/wna-survey-sheath-corrected-e/2012/rbsp-b_wna-survey-sheath-corrected-e_emfisis-l4_20120901_v2.0.1.cdf. The most common cadence, 5999996781 [ns] = PT5.999997S, occurred for 26.7189% of the 3684 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l4/emfisis/wna-survey/2012/rbsp-b_wna-survey_emfisis-l4_20120831_v1.7.1.cdf. The most common cadence, 6000000000 [ns] = PT6S, occurred for 32.1294% of the 4252 timesteps.

This work was supported by Van Allen Probes (RBSP) EFW funding provided by JHU/APL Contract No. TBD under NASA's Prime Contract No. TBD; EFW PI, J. R. Wygant, UMN.

Open Data for Scientific Use; please see EFW "Rules of the Road" (http://rbsp.space.umn.edu/data_policy.html) for details of the Van Allen Probes Mission and EFW Instrument "Rules of the Road", and the EFW-FAQ (http://rbsp.space.umn.edu/efw_faq.html) for details of and caveats on instrument performance and data quality.

SPDF/CDAWeb. Please also acknowledge the data producer: J. R. Wygant at University of Minnesota

SPDF/SSCWeb. Please also acknowledge the data producer: J. R. Wygant at University of Minnesota

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. R. Wygant at University of Minnesota

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch, @1 => epoch_qual.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch, @1 => epoch_qual.)

Van Allen Probes (RBSP) A (from all.xml/observatory/description/@short)

Electric Field and Waves L2 (from all.xml/instrument/description/@short)

Van Allen Probes (RBSP) A (from Master/CDFglobalAttributes/Source_name)

High Resolution DC Electric Field in UVW Coordinates (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/e-highres-uvw/2012/rbspa_efw-l2_e-hires-uvw_20120923_v03.cdf. The most common cadence, 31250000000 [ps] = PT0.03125S, occurred for 93.8761% of the 2595526 timesteps. 

Counts based on variable 'epoch_qual' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/e-highres-uvw/2012/rbspa_efw-l2_e-hires-uvw_20120923_v03.cdf. The most common cadence, 10000000000000 [ps] = PT10S, occurred for all 8640 timesteps. 

Spinfit (10.9 sec resolution) DC Electric Field estimates in M-GSE coordinates.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch, @1 => epoch_hsk.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch, @1 => epoch_hsk.)

Spinfit DC Electric Field in M-GSE Coordinates (from Master/CDFglobalAttributes/Data_type)

Spinfit E-field in MGSE (autoscale, VxB subtracted, i.e. near GSE)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/e-spinfit-mgse/2012/rbspa_efw-l2_e-spinfit-mgse_20120905_v01.cdf. The most common cadence, 11592180000000 [ps] = PT11.59218S, occurred for 0.3779% of the 11 timesteps. 

An array that indicates a global estimate of EFW data quality, as well as a breakdown of observatory and instrument-level data quality issues that impact the global quality estimate..

Angles b/t the Ey and Ez MGSE spinplane directions and the background magnetic field.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_qual, @1 => epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_qual, @1 => epoch.)

E-Field and Waves L2 (from all.xml/instrument/description/@short)

Despun (32 samples/sec) Electric Field estimates in M-GSE coordinates (from Master/CDFglobalAttributes/Data_type)

---> EFW quality array (global estimate of EFW data quality, plus 13 underlying observatory and instrument-level data quality factors)

Counts based on variable 'epoch_qual' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/esvy_despun/2012/rbspa_efw-l2_esvy_despun_20120905_v01.cdf. The most common cadence, 11800000000000 [ps] = PT11.8S, occurred for 99.9863% of the 7320 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/esvy_despun/2012/rbspa_efw-l2_esvy_despun_20120905_v01.cdf. The most common cadence, 59999995749149 [ps] = PT59.999996S, occurred for 45.0694% of the 649 timesteps. 

Filterbank peak and average values 1-7000 Hz from RBSP-EFW (with peak and average values returned for 2 of 20 possible sources at any one time)

 This work was supported by Van Allen Probes (RBSP) EFW funding provided by JHU/APL Contract No. TBD under NASA's Prime Contract No. TBD; EFW PI, J. R. Wygant, UMN.

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/fbk/2012/rbspa_efw-l2_fbk_20120905_v02.cdf. The most common cadence, 125000000000 [ps] = PT0.125S, occurred for 73.4212% of the 190912 timesteps. 

On-Board Spin-Fit 4-8000 Hz electric and magnetic field spectral data from RBSP-EFW (with 7 of 75 possible sources returned at any one time)

Six spectral products are returned. The possible sources are:.E12dc,E34dc,E56dc.E12ac,E34ac,E56ac.Edcpar,Edcprp.Eacpar,Eacprp.V1ac,V2ac,V3ac,V4ac,V5ac,V6ac.SCMU,SCMV,SCMW.SCMpar,SCMprp,.(V1ac+V2ac+V3ac+V4ac)/4,.Edcprp2, Eacprp2, SCMprp2.

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/spec/2012/rbspa_efw-l2_spec_20120905_v02.cdf. The most common cadence, 3999938964843 [ps] = PT3.999939S, occurred for 36.8073% of the 3115 timesteps. 

DERIVED FROM: Spinfit DC Electric Field estimates in M-GSE coordinates

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_v, @1 => epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => epoch_v, @1 => epoch.)

Spinfit DC Efield in MGSE Coord (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch_v' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/vsvy-highres/2012/rbspa_efw-l2_vsvy-hires_20120905_v04.cdf. The most common cadence, 62500000000 [ps] = PT0.0625S, occurred for 87.1038% of the 471612 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/efw/vsvy-highres/2012/rbspa_efw-l2_vsvy-hires_20120905_v04.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for all 86400 timesteps. 

Spinfit DC electric field estimates in the M-GSE coordinate system - see the EFW-FAQ (http://rbsp.space.umn.edu/efw_faq.html) for a description of the spin fit algorithm and the M-GSE coordinate system.One 2D vector estimate of the E-field is computed at a cadence of once per spin period (typ. 10.7 to 11.1 s) using the survey E-field data product - the potential difference between EFW sensors V1 and V2 (E12) or V3 and V4 (E34) sampled at a nominal rate of 32 samp/s with a resolution of 16 bits.The X-component of the E-field estimate, corresponding to the axial component in the spacecraft coordinate system, is set to zero in this data product.  See the EFW-FAQ (http://rbsp.space.umn.edu/efw_faq.html) for a discussion of this convention for this data product.The VxB electric field in the spacecraft frame due to orbital motion of the spacecraft around the Earth as computed from the spacecraft orbital velocity and measured B-field in the spaceraft frame has been subtracted from the measured electric field, and so the data product is in the quasi-inertial frame equivalent to GSE (i.e. it is NOT in the corotation frame of the Earth!).Each spin fit is time-tagged with the time corresponding to the middle of the spin of data that went into the spin fit algorithm; in other words, if a given spin covers the interval [t1, t2), then the spin fit E-field estimate associated with that spin is given the time tag 0.5*(t1 + t2).The root mean square residual between the data included in the fit and the resulting best-fit model, sigma, and the final number of points included in the spin fit, npts, are also provided at spin-period cadence.The nominal dynamic range of the E-field estimate is +/- 1 V/m in any component.

This work was supported by Van Allen Probes (RBSP) EFW funding provided by JHU/APL Contract No. 922613 under NASA's Prime Contract No. NNN06AA01C; EFW PI, J. R. Wygant, UMN.

Electric Field and Waves (from all.xml/instrument/description/@short)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/efw/2012/rbspa_efw-l3_20120918_v01.cdf. The most common cadence, 6299249000000 [ps] = PT6.299249S, occurred for 0.7640% of the 131 timesteps. 

The RPS instrument is a solid state detector telescope combined with a Cherenkov radiator. It measures protons with energies from about 60 MeV to about 2 GeV. For more information, see http://rbsp.aerospace.org/. For a complete description of the instrument, see Mazur et al., 2012, The Relativistic Proton Spectrometer (RPS) for the Van Allen Probes Mission (formerly known as Radiation Belt Storm Probes, RBSP), Space Science Reviews. DOI 10.1007/s11214-012-9926-9,  http://www.springerlink.com/content/p84680786570g7qp/. The instrument PI, Dr. Joe Mazur, can be reached at Joseph.E.Mazur@aero.org.

The Aerospace Corporation designed and built the RPS instrument with funding from The National Reconnaissance Office. The RPS Principal Investigator is Dr. Joseph Mazur

Van Allen Probes RPS, Web Page for Instrument Summary and Data Access, ViRBO

Van Allen Probes Relativistic Proton Spectrometer, RPS, Web Page for Instrument Description Summary and Data Access Links, at the Virtual Radiation Belt Observatory

Those wishing to use RPS data are strongly urged to notify the PI of the topic of their work. This will enable the RPS team to assist in use of the data and to track the instrument's utility to the broader community.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Mazur at The Aerospace Corporation

SPDF/SSCWeb. Please also acknowledge the data producer: J. Mazur at The Aerospace Corporation

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Mazur at The Aerospace Corporation

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rps/psbr-rps-1min/2012/rbspa_l2-1min_psbr-rps_20120902_v3.0.0.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Proton Spectrometer Belt Research - Relativistic Proton Spectrometer (from all.xml/instrument/description/@short)

Source of Measured field - 0 indicates MAG L0 file, 1 indicates MAG L1 file, etc. If 255, then the OPQ77 model field is used for computing Alpha and Beta

Unidirectional, differential flux vs energy (Isotropic assumption)

Quality flag for FPDI fluxes: 0 - highest quality, 1 - problem with time resolution, 2 - contamination, 3 - saturation, 4 - other problem, 5 - possible electron background, 10 -not yet quality checked

Third (drift) invariant  of particle with 90 degree pitch angle in OPQ

Equatorial pitch angle of particle with 90 degree pitch angle in OPQ

OPQ model magnetic field strength at local minimum along local field line

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => EVENT_Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => EVENT_Epoch.)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rps/psbr-rps/2012/rbspa_l2_psbr-rps_20120902_v3.0.0.cdf. The most common cadence, 253 [ms] = PT0.253S, occurred for 99.9146% of the 340504 timesteps. 

Attitude quality flag: 0 - definitive, 1 - quick-look, 2 - predicted

Angle of incidence of particle coming from center of Earth (relative to normal incidence)

RPS bore sight vector in GEO (parallel to incoming normally incident particle)

RMS error in ln(FPDU) including Poisson and FPDU_Crosscalib_RMSE

Quality flag for FPDU fluxes: 0 - highest quality, 1 - problem with time resolution (less than 5% live time in sector), 2 - contamination, 3 - saturation, 4 - other problem, 5 - possible electron background, 10 -not yet quality checked

Gyrophase angle of incoming particle along RPS boresight axis (zero when heading away from Earth)

Spin phase angle of RPS boresight. Phase of 0 occurs at minimum pitch angle. Phase of 90 occurs when Alpha is 90 and increasing

Magnetic field strength at mirror point for incoming particle along RPS boresight axis

Equatorial pitch angle (OPQ) of incoming particle along RPS boresight axis

McIlwain integral invariant of normally incident particle in OPQ

Kaufmann K, modified second invariant, of normally incident particle in OPQ

Minimum geodetic altitude on drift orbit of normally incident particle in OPQ

Equatorial pitch angle (T89Q) of incoming particle along RPS boresight axis

McIlwain integral invariant of normally incident particle in T89Q

Kaufmann K, modified second invariant, of normally incident particle in T89Q

T89Q model magnetic field strength at local minimum along local field line

Minimum geodetic altitude on drift orbit of normally incident particle in T89Q

Equatorial pitch angle (T89D) of incoming particle along RPS boresight axis

McIlwain integral invariant of normally incident particle in T89D

Kaufmann K, modified second invariant, of normally incident particle in T89D

T89D model magnetic field strength at local minimum along local field line

Minimum geodetic altitude on drift orbit of normally incident particle in T89D

Equatorial pitch angle (TS04D) of incoming particle along RPS boresight axis

McIlwain integral invariant of normally incident particle in TS04D

Kaufmann K, modified second invariant, of normally incident particle in TS04D

TS04D model magnetic field strength at local minimum along local field line

Minimum geodetic altitude on drift orbit of normally incident particle in TS04D

MET of event, combination of Packet's MET_SEC and  EVENT_SUBTIME_CODE

Counts based on variable 'EVENT_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/rps/psbr-rps/2012/rbspa_l2_psbr-rps_20120902_v3.0.0.cdf. The most common cadence, 16 [ms] = PT0.016S, occurred for 1.4199% of the 2405 timesteps. 

Mission day of level 0 files for this data point. Note: CDF_UINT4 data was converted to HAPI double.

Estimated event energy using the average of minimum 2 SSD deposits algorithm

Event classification (-1:INVALID, 0:UNKNOWN, 1:PEN, 2:CHE, 3:ALPHA mode, 127:FILL)

Electron fluxes ~20-4000 keV and proton fluxes ~50-1500 keV from ECT/MAGEIS

Van Allen Probes Energetic Particle, Composition, and Thermal Plasma Suite, ECT, Home Page at the University of New Hampshire

Van Allen Probes Energetic Particle, Composition, and Thermal Plasma Suite, ECT, Science Operations Center, SOC, and Data Services Web Page at the Los Alamos National Laboratory

Van Allen Probes ECT SOC, Data Access Links to MagEIS Particle Data, LANL

Van Allen Probes Energetic Particle, Composition, and Thermal Plasma Suite, ECT, Science Operations Center, SOC, Data Access Links to Pitch Angle resolved Magnetic Electron Ion Spectrometer, MagEIS, Particle Web Site for access to Magnetic Field Data the Los Alamos National Laboratory

SPDF/CDAWeb. Please also acknowledge the data producer: J. Bernard Blake / JBernard.Blake@aero.org at The Aerospace Corporation

SPDF/SSCWeb. Please also acknowledge the data producer: J. Bernard Blake / JBernard.Blake@aero.org at The Aerospace Corporation

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Bernard Blake / JBernard.Blake@aero.org at The Aerospace Corporation

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_prot.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_prot.)

ECT Magnetic Electron Ion Spectrometer Level 2 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/mageis/sectors/rel03/2012/rbspa_rel03_ect-mageis-l2_20120907_v4.1.0.cdf. The most common cadence, 11600 [ms] = PT11.6S, occurred for 96.6200% of the 6489 timesteps. 

FESA_CORR: Background-corrected Spin-Averaged Differential Electron Flux ~20-4000 keV

Flag to indicate whether or not the electron coincidence is enabled (0=disabled; 1=enabled).

---> Flag to indicate mode of the MagEIS instruments (0=maintenance; 1=science; 2=high rate).

---> Flag to indicate whether or not the electron detectors are in the normal-bias or low-bias state (0=low bias; 1=normal bias)

---> Ratio of the background estimate divided by the main rate rate, for the spin-averaged data.

[Time-series] Position of the satellite in geographic coordinates

Counts based on variable 'Epoch_prot' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/mageis/sectors/rel03/2012/rbspa_rel03_ect-mageis-l2_20120907_v4.1.0.cdf. The most common cadence, 11598 [ms] = PT11.598S, occurred for 32.4713% of the 2147 timesteps. 

FPDU: Unidirectional Differential Proton Flux ~50-1500 keV, in up to 31 energy and 64 sector bins (energy-sector displays)

Electron fluxes 2-20 MeV and proton fluxes 20-120 MeV from ECT/REPT

SPDF/CDAWeb. Please also acknowledge the data producer: D. Baker at University of Colorado at Boulder

SPDF/SSCWeb. Please also acknowledge the data producer: D. Baker at University of Colorado at Boulder

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Baker at University of Colorado at Boulder

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/rept/sectors/rel03/2012/rbspa_rel03_ect-rept-sci-l2_20120901_v5.0.0.cdf. The most common cadence, 18527 [ms] = PT18.527S, occurred for 15.7982% of the 379 timesteps. 

Relativistic Electron Proton Telescope Level-2 (from all.xml/instrument/description/@short)

FESA: Spin-Averaged Differential Electron Flux 2-20 MeV, in 12 energy bands (spectrogram)

FEDU: Unidirectional Differential Electron Flux 2-20 MeV, in 12 energy and 36 angle bins (energy-angle displays)

FPSA: Spin-Averaged Differential Proton Flux 20-120 MeV (spectrograms)

FPDU - Unidirectional Differential Proton Flux 20-120 MeV, in 8 energy and 36 angle bins (energy-angle displays)

RBSP/ECT REPT Pitch Angle Resolved Electron and Proton Fluxes. Electron energies: 2 - 59.45 MeV. Proton energies: 21.25 - 0 MeV

This work was supported by Van Allen Probes/RBSP-ECT funding provided by JHU/APL Contract No. 967399 under NASA's Prime Contract No. NAS5-01072.

REPT (Relativistic Electron Proton Telescope), Level 3 science data

See Usage Guidelines at: http://www.rbsp-ect.lanl.gov/DataProductsUsage.php

Van Allen Probes, Radiation Belt Storm Probe A (from all.xml/observatory/description/@short)

ECT REPT - Relativistic Electron Proton Telescope, Level 3 science data (from all.xml/instrument/description/@short)

Van Allen Probes, Radiation Belt Storm Probe A (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/rept/sectors/rel03/2012/rbspa_rel03_ect-rept-sci-l3_20120901_v5.0.0.cdf. The most common cadence, 18527 [ms] = PT18.527S, occurred for 15.7982% of the 379 timesteps. 

FEDU_Unbinned_0to180 - Unidirectional Differential Electron Flux (raw sector data).

---> FEDU_Unbinned_0to360 - Unidirectional Differential Electron Flux (raw sector data).

Lstar - Roederer's generalized L-shell parameter. Computed for 90deg. particles using OP77Q external field and IGRF internal field.

---> L - McIlwain's L-shell parameter. Computed for 90deg. particles using OP77Q external field and IGRF internal field.

---> I - Integral invariant. Computed for 90deg. particles using OP77Q external field and IGRF internal field.

---> B_Calc - Magnitude of computed model field at the S/C. Computed using OP77Q external field and IGRF internal field.

---> B_Eq - Magnitude of computed model field at the Minimum-|B| point along the field line threading the S/C. Computed using OP77Q external field and IGRF internal field.

---> MLT - Eccentric Dipole Magnetic Local Time. Computed using OP77Q external field and IGRF internal field.

---> MLAT - Eccentric Dipole Magnetic Latitude. Computed using OP77Q external field and IGRF internal field.

Counts based on variable 'Epoch_prot' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/rept/sectors/rel03/2012/rbspa_rel03_ect-rept-sci-l3_20120901_v5.0.0.cdf. The most common cadence, 18527 [ms] = PT18.527S, occurred for 15.7982% of the 379 timesteps. 

FPDU_Unbinned_0to180 - Unidirectional Differential Proton Flux (raw sector data).

---> FPDU_Unbinned_0to360 - Unidirectional Differential Proton Flux (raw sector data).

[NO PLOTS] FPDU_Unbinned_LightMask_0to360 - LightMask for FPDU_Unbinned_0to360 array.

Spin resolved HOPE science data.  Plasma moments from electrons >200 eV and ions >30 eV measured at apogee in alternate spin cadence.

Distribute freely, acknowledge original PI. Please contact PI before any publication or presentation of data.

SPDF/CDAWeb. Please also acknowledge the data producer: Herbert Funsten at Los Alamos National Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Herbert Funsten at Los Alamos National Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Herbert Funsten at Los Alamos National Laboratory

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_Ion, @1 => Epoch_Ele.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_Ion, @1 => Epoch_Ele.)

ECT Helium Oxygen Proton Electron Plasma Analyszer Level 3 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/hope/moments/rel04/2012/rbspa_rel04_ect-hope-mom-l3_20121025_v7.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 47.3668% of the 1556 timesteps. 

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/hope/moments/rel04/2012/rbspa_rel04_ect-hope-mom-l3_20121025_v7.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 43.2265% of the 1605 timesteps. 

Pitch angle resolved ECT-HOPE science data.  Electron fluxes ~15-50,000 eV, ion fluxes ~1-50,000 eV. Electrons and ions measured in alternate spin cadence. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_Ele, @1 => Epoch_Ion.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_Ele, @1 => Epoch_Ion.)

ECT Helium Oxygen Proton Electron Plasma Analyszer Fluxes by Pitch Angle Level 3 (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/hope/pitchangle/rel04/2012/rbspa_rel04_ect-hope-pa-l3_20121025_v7.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 43.2265% of the 1605 timesteps. 

FEDU: Unidirectional Differential Electron Flux ~15-50,000 eV, in 72 energy and 11 pitch angle bins (energy-angle displays)

---> Spectrograms by energy at sample pitch angles (perigee mode excluded)

---> Spectrograms by pitch angle at sample energies (perigee mode excluded)

Model magnetic field strength at magnetic equator (electron timebase)

Position of the satellite in geographic coordinates (electron timebase)

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/hope/pitchangle/rel04/2012/rbspa_rel04_ect-hope-pa-l3_20121025_v7.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 47.3668% of the 1556 timesteps. 

FPDU: Unidirectional Differential Proton Flux ~1-50,000 eV, in 72 energy and 11 pitch angle bins (energy-angle displays)

---> Spectrograms by pitch angle at sample energies (perigees excluded)

FODU: Unidirectional Differential Oxygen Flux ~1-50,000 eV, in 72 energy and 11 pitch angle bins (energy-angle displays)

FHEDU: Unidirectional Differential Helium Flux ~1-50,000 keV, in 72 energy and 11 pitch angle bins (energy-angle displays)

---> Model magnetic field strength at magnetic equator (ion timebase)

---> Position of the satellite in geographic coordinates (ion timebase)

Spin resolved ECT-HOPE science data. Electron fluxes ~15-50,000 eV, ion fluxes ~1-50,000 eV. Electrons and ions measured in alternate spin cadence. 

ECT Helium Oxygen Proton Electron Plasma Analyszer Level 2 (from all.xml/instrument/description/@short)

Position of the satellite in geographic coordinates (ion timebase)

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/hope/sectors/rel04/2012/rbspa_rel04_ect-hope-sci-l2_20121025_v6.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 47.3668% of the 1556 timesteps. 

Model magnetic field strength at magnetic equator (ion timebase)

[CreateCDF ONLY] FPDU: Differential directional proton flux ~15-50,000 eV (5 Detectors, 16 Sectors, 72 Energies) 

[CreateCDF ONLY] FHeDU: Differential directional helium flux ~15-50,000 eV (5 Detectors, 16 Sectors, 72 Energies) 

[CreateCDF ONLY] FODU: Differential directional oxygen flux ~1-50,000 eV (5 Detectors, 16 Sectors, 72 Energies) 

---> Position of the satellite in geographic coordinates (electron timebase)

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/hope/sectors/rel04/2012/rbspa_rel04_ect-hope-sci-l2_20121025_v6.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 43.2265% of the 1605 timesteps. 

---> Model magnetic field strength at magnetic equator (electron timebase)

[CreateCDF ONLY] FEDU: Differential directional electron flux ~15-50,000 eV (5 Detectors, 16 Sectors, 72 Energies) 

Spin averaged ECT-HOPE science data. Electron fluxes ~15-50,000 eV, ion fluxes ~1-50,000 eV. Electrons and ions measured in alternate spin cadence. 

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/hope/spinaverage/rel04/2012/rbspa_rel04_ect-hope-sci-l2sa_20121025_v6.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 47.3668% of the 1556 timesteps. 

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l2/ect/hope/spinaverage/rel04/2012/rbspa_rel04_ect-hope-sci-l2sa_20121025_v6.1.0.cdf. The most common cadence, 24346 [ms] = PT24.346S, occurred for 43.2265% of the 1605 timesteps. 

Electron fluxes ~20-4000keV and proton fluxes ~60-1500 keV from ECT/MagEIS

Van Allen Probes, RBSPECT/MagEIS (Radiation Belt Storm Probes Energetic particle, Composition and Thermal plasma suite/Magnetic Electron Ion Spectrometer, Level 3 Pitch Angle Sorted Data.

SPDF/CDAWeb. Please also acknowledge the data producer: J. Bernard Blake (JBernard.Blake@aero.org) at The Aerospace Corporation

SPDF/SSCWeb. Please also acknowledge the data producer: J. Bernard Blake (JBernard.Blake@aero.org) at The Aerospace Corporation

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Bernard Blake (JBernard.Blake@aero.org) at The Aerospace Corporation

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => FPDU_Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => FPDU_Epoch.)

ECT Magnetic Electron Ion Spectrometer, Normal Rate Level-3 Data (from all.xml/instrument/description/@short)

FEDU: Unidirectional Differential Electron Flux, ~20-4000 keV in 23 energy and 11 pitch angle bins (energy-angle displays)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/mageis/sectors/rel04/2012/rbspa_rel04_ect-mageis-l3_20120907_v8.1.0.cdf. The most common cadence, 11598 [ms] = PT11.598S, occurred for 32.4667% of the 2148 timesteps. 

[Movie] FEDU: Unidirectional Differential Electron Flux, ~20-4000 keV in 23 energy and 11 pitch angle bins (energy-angle displays)

---> FEDU_ERROR - sqrt of Unidirectional Differential Electron Counts

FEDU_CORR - Background-Corrected Unidirectional Differential Electron Flux

[Movie] FEDU_CORR - Background-Corrected Unidirectional Differential Electron Flux

---> FEDU_CORR_ERROR - Estimate of the percent error in the corrected electron flux.

---> LstarVsAlpha - Roederer's generalized L-shell parameter. Pitch angle depenedent (pitch angles are local pitch angles). Computed using OP77Q external field and IGRF internal field.

FPDU: Unidirectional Differential Proton Flux, ~60-1300 keV in 21 energy and 32 pitch angle bins (energy-angle displays)

Counts based on variable 'FPDU_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspa/l3/ect/mageis/sectors/rel04/2012/rbspa_rel04_ect-mageis-l3_20120907_v8.1.0.cdf. The most common cadence, 11598 [ms] = PT11.598S, occurred for 32.4713% of the 2147 timesteps. 

[Movie] FPDU: Unidirectional Differential Proton Flux, ~60-1300 keV in 21 energy and 32 pitch angle bins (energy-angle displays)

Van Allen Probes (RBSP) B (from all.xml/observatory/description/@short)

Van Allen Probes (RBSP) B (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/e-highres-uvw/2012/rbspb_efw-l2_e-hires-uvw_20120923_v03.cdf. The most common cadence, 31250000000 [ps] = PT0.03125S, occurred for 99.3753% of the 2747524 timesteps. 

Counts based on variable 'epoch_qual' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/e-highres-uvw/2012/rbspb_efw-l2_e-hires-uvw_20120923_v03.cdf. The most common cadence, 10000000000000 [ps] = PT10S, occurred for all 8640 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/e-spinfit-mgse/2012/rbspb_efw-l2_e-spinfit-mgse_20120905_v01.cdf. The most common cadence, 11621674000000 [ps] = PT11.621674S, occurred for 3.1414% of the 6 timesteps. 

Counts based on variable 'epoch_qual' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/esvy_despun/2012/rbspb_efw-l2_esvy_despun_20120905_v01.cdf. The most common cadence, 11800000000000 [ps] = PT11.8S, occurred for 99.9863% of the 7320 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/esvy_despun/2012/rbspb_efw-l2_esvy_despun_20120905_v01.cdf. The most common cadence, 59999995749149 [ps] = PT59.999996S, occurred for 45.0694% of the 649 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/fbk/2012/rbspb_efw-l2_fbk_20120905_v02.cdf. The most common cadence, 125000000000 [ps] = PT0.125S, occurred for 91.5702% of the 16848 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/spec/2012/rbspb_efw-l2_spec_20120905_v02.cdf. The most common cadence, 3999984741210 [ps] = PT3.999985S, occurred for 41.2781% of the 239 timesteps. 

Counts based on variable 'epoch_v' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/vsvy-highres/2012/rbspb_efw-l2_vsvy-hires_20120905_v04.cdf. The most common cadence, 62500000000 [ps] = PT0.0625S, occurred for 96.0176% of the 35394 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/efw/vsvy-highres/2012/rbspb_efw-l2_vsvy-hires_20120905_v04.cdf. The most common cadence, 1000000000000 [ps] = PT1S, occurred for all 86400 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/efw/2012/rbspb_efw-l3_20120918_v01.cdf. The most common cadence, 6350799000000 [ps] = PT6.350799S, occurred for 0.5858% of the 86 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rps/psbr-rps-1min/2012/rbspb_l2-1min_psbr-rps_20120901_v3.0.0.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rps/psbr-rps/2012/rbspb_l2_psbr-rps_20120901_v3.0.0.cdf. The most common cadence, 252 [ms] = PT0.252S, occurred for 98.9091% of the 338191 timesteps. 

Counts based on variable 'EVENT_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/rps/psbr-rps/2012/rbspb_l2_psbr-rps_20120901_v3.0.0.cdf. The most common cadence, 16 [ms] = PT0.016S, occurred for 3.4414% of the 24451 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/mageis/sectors/rel03/2012/rbspb_rel03_ect-mageis-l2_20120907_v4.0.0.cdf. The most common cadence, 11600 [ms] = PT11.6S, occurred for 73.4316% of the 5478 timesteps. 

Counts based on variable 'Epoch_prot' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/mageis/sectors/rel03/2012/rbspb_rel03_ect-mageis-l2_20120907_v4.0.0.cdf. The most common cadence, 11627 [ms] = PT11.627S, occurred for 29.5609% of the 2181 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/rept/sectors/rel03/2012/rbspb_rel03_ect-rept-sci-l2_20120902_v5.0.0.cdf. The most common cadence, 18425 [ms] = PT18.425S, occurred for 17.8118% of the 337 timesteps. 

Van Allen Probes, Radiation Belt Storm Probe B (from all.xml/observatory/description/@short)

Van Allen Probes, Radiation Belt Storm Probe B (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/rept/sectors/rel03/2012/rbspb_rel03_ect-rept-sci-l3_20120902_v5.0.1.cdf. The most common cadence, 18425 [ms] = PT18.425S, occurred for 17.8118% of the 337 timesteps. 

Counts based on variable 'Epoch_prot' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/rept/sectors/rel03/2012/rbspb_rel03_ect-rept-sci-l3_20120902_v5.0.1.cdf. The most common cadence, 18425 [ms] = PT18.425S, occurred for 17.8118% of the 337 timesteps. 

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/hope/moments/rel04/2012/rbspb_rel04_ect-hope-mom-l3_20121026_v7.3.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 49.8167% of the 1767 timesteps. 

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/hope/moments/rel04/2012/rbspb_rel04_ect-hope-mom-l3_20121026_v7.3.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 49.0273% of the 1739 timesteps. 

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/hope/pitchangle/rel04/2012/rbspb_rel04_ect-hope-pa-l3_20121026_v7.2.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 49.0273% of the 1739 timesteps. 

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/hope/pitchangle/rel04/2012/rbspb_rel04_ect-hope-pa-l3_20121026_v7.2.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 49.8167% of the 1767 timesteps. 

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/hope/sectors/rel04/2012/rbspb_rel04_ect-hope-sci-l2_20121025_v6.1.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 46.0025% of the 1496 timesteps. 

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/hope/sectors/rel04/2012/rbspb_rel04_ect-hope-sci-l2_20121025_v6.1.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 43.7860% of the 1596 timesteps. 

Counts based on variable 'Epoch_Ion' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/hope/spinaverage/rel04/2012/rbspb_rel04_ect-hope-sci-l2sa_20121025_v6.1.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 46.0025% of the 1496 timesteps. 

Counts based on variable 'Epoch_Ele' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l2/ect/hope/spinaverage/rel04/2012/rbspb_rel04_ect-hope-sci-l2sa_20121025_v6.1.0.cdf. The most common cadence, 24347 [ms] = PT24.347S, occurred for 43.7860% of the 1596 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/mageis/sectors/rel04/2012/rbspb_rel04_ect-mageis-l3_20120906_v8.2.0.cdf. The most common cadence, 11625 [ms] = PT11.625S, occurred for 47.6948% of the 600 timesteps. 

Counts based on variable 'FPDU_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rbsp/rbspb/l3/ect/mageis/sectors/rel04/2012/rbspb_rel04_ect-mageis-l3_20120906_v8.2.0.cdf. The most common cadence, 11625 [ms] = PT11.625S, occurred for 46.5986% of the 411 timesteps. 

RBSP/ECT REPT Monthly Intensities as a function of Energy, Pitch Angle and L-shell from the Selesnick model

The files contain model radiation belt proton intensity derived from data taken by the Van Allen Probes REPT instruments using the method described by: Selesnick, R. S., Baker, D. N., Kanekal, S. G., Hoxie, V. C., & Li, X. (2018).  Modeling the proton radiation belt with Van Allen Probes Relativistic Electron-Proton Telescope data. Journal of Geophysical Research: Space Physics, 123. https://doi.org/10.1002/2017JA024661 Each file contains average intensity, as a function of kinetic energy, equatorial pitch angle, and L-shell, derived from 1 month of data. 

Selesnick, R.S., Baker, D.N., Kanekal, S.G., Hoxie, V.C., X. Li, Modeling the Proton Radiation Belt with Van Allen Probes Relativistic Electron-Proton Telescope Data, J. Geophys. Res. Space Phys., 123, 685-697, https://doi.org/10.1002/2017JA024661, 2018

Van Allen Probes Energetic Particle, Composition, and Thermal Plasma Suite Data Usage Web Page, LANL

Van Allen Probes Energetic Particle, Composition, and Thermal Plasma Suite Data Usage and Acknowledgement Web Page, Los Alamos National Laboratory

REPT (Relativistic Electron Proton Telescope), Level 3 Selesnick model

Van Allen Probes, Radiation Belt Storm (from all.xml/observatory/description/@short)

Van Allen Probes, Radiation Belt Storm (from Master/CDFglobalAttributes/Source_name)

ECT REPT - Relativistic Electron Proton Telescope, Level 3 science data (from Master/CDFglobalAttributes/Data_type)

[MOVIE DISPLAY] Natural Log of Proton Intensity at E=26.1 MeV (#25)

[MOVIE DISPLAY] Natural Log of Proton Intensity at PA=10.0 deg (#5)

[NO PLOTS] 1-sigma uncertainties for the NL natural logarithms of proton intensity

1-sigma uncertainties for the NL natural logarithms of Proton Intensity at E=40.9 MeV (#50)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at E=100.1 MeV (#100)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at E=245 MeV (#150)

1-sigma uncertainties for the NL natural logarithms of Proton Intensity at PA=22.5 deg (#10)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at PA=47.5 deg (#20)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at PA=72.5 deg (#30)

1-sigma uncertainties for the NL natural logarithms of Proton Intensity at L=1.6 (#10)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at L=2.1 (#20)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at L=2.6 (#30)

---> 1-sigma uncertainties for the NL natural logarithms of Proton Intensity at L=3.1 (#40)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 101

The Responsive Environmental Assessment Commercially Hosted (REACH) constellation is collection of 32 small sensors hosted on six orbital planes of the Iridium-Next space vehicles in low earth orbit. Each sensor contains two micro-dosimeters sensitive to the passage of charged particles from the Earth's radiation belts. There are six distinct dosimeter types spread among the 64 individual sensors, which are unique in shielding and electronic threshold. When taken together, this effectively enables a high time-cadence measurement of protons and electrons in six integral energy channels over the entire globe.

The development of the netCDF files was supported by the SPI Goddard HISFM 2022. The success of the REACH project is owed to a long line of people who have contributed to it over the many years of development. The REACH hardware team in The Aerospace Corporation's xLab organization included Paul Carranza, Sue Crain, Bill Crain, Andrew Hsu, Brian McCarthy, John McHale, Can Nguyen, Mario Perez, Deb Salvaggio, and Gerrit Sorensen, all critical to designing and fabricating the first 18 of the 32 REACH pods. Millennium Engineering and Integration (MEI) manufactured the remaining 14 pods. Doug Holker was instrumental in nearly all facets of REACH development, outreach, support, endorsement and project management for the entirety of the project lifetime. The REACH project was led in chronological order by the following USAF Program Managers: Capt Dan Kimmich, Lt Garrett Ellis, Lt Justin Shimasaki, Capt Sean Quintana, Capt Felix Abeyta, Lt Kurt Mann, Maj James Crane, Capt Omar Manning, Lt Zach Morley, Capt Scott Day, Lt Zeesha Braslawsce, and Lt Ryan Francies. This list reflects their ranks at the time of involvement. Recent management is possible through the SMC/Development Corp program office support Pete Cunningham. Data transport is provided by Iridium, L3Harris, and data processing of the Level 0 files is performed by Robin Barnes and supported by Tom Sotirelis and Mike Kelly at the Johns Hopkins Applied Physics Laboratory. Alexa Halford, now of NASA Goddard Space Flight Center, prototyped many higher-level REACH data products and performed intra-calibration of the dosimeters.

See Usage Guidelines at: https://zenodo.org/record/6423507#.YmMqcfPMLCU

SPDF/CDAWeb. Please also acknowledge the data producer: Joe Mazur (joseph.e.mazur@aero.org) at The Aerospace Corporation

SPDF/SSCWeb. Please also acknowledge the data producer: Joe Mazur (joseph.e.mazur@aero.org) at The Aerospace Corporation

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Joe Mazur (joseph.e.mazur@aero.org) at The Aerospace Corporation

The Responsive Environmental Assessment Commercially Hosted, satellite id  101 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  101 (from all.xml/instrument/description/@short)

Magnetospheric Science, Space Weather (from Master/CDFglobalAttributes/Discipline)

The Responsive Environmental Assessment Commercially Hosted, satellite id  101 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 102

The Responsive Environmental Assessment Commercially Hosted, satellite id  102 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  102 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  102 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 105

The Responsive Environmental Assessment Commercially Hosted, satellite id  105 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  105 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  105 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 108

The Responsive Environmental Assessment Commercially Hosted, satellite id  108 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  108 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  108 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 113

The Responsive Environmental Assessment Commercially Hosted, satellite id  113 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  113 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  113 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 114

The Responsive Environmental Assessment Commercially Hosted, satellite id  114 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  114 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  114 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 115

The Responsive Environmental Assessment Commercially Hosted, satellite id  115 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  115 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  115 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 116

The Responsive Environmental Assessment Commercially Hosted, satellite id  116 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  116 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  116 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 133

The Responsive Environmental Assessment Commercially Hosted, satellite id  133 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  133 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  133 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 134

The Responsive Environmental Assessment Commercially Hosted, satellite id  134 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  134 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  134 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 135

The Responsive Environmental Assessment Commercially Hosted, satellite id  135 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  135 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  135 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 136

The Responsive Environmental Assessment Commercially Hosted, satellite id  136 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  136 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  136 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 137

The Responsive Environmental Assessment Commercially Hosted, satellite id  137 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  137 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  137 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 138

The Responsive Environmental Assessment Commercially Hosted, satellite id  138 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  138 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  138 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 139

The Responsive Environmental Assessment Commercially Hosted, satellite id  139 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  139 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  139 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 140

The Responsive Environmental Assessment Commercially Hosted, satellite id  140 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  140 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  140 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 148

The Responsive Environmental Assessment Commercially Hosted, satellite id  148 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  148 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  148 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 149

The Responsive Environmental Assessment Commercially Hosted, satellite id  149 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  149 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  149 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 162

The Responsive Environmental Assessment Commercially Hosted, satellite id  162 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  162 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  162 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 163

The Responsive Environmental Assessment Commercially Hosted, satellite id  163 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  163 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  163 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 164

The Responsive Environmental Assessment Commercially Hosted, satellite id  164 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  164 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  164 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 165

The Responsive Environmental Assessment Commercially Hosted, satellite id  165 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  165 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  165 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 166

The Responsive Environmental Assessment Commercially Hosted, satellite id  166 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  166 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  166 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 169

The Responsive Environmental Assessment Commercially Hosted, satellite id  169 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  169 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  169 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 170

The Responsive Environmental Assessment Commercially Hosted, satellite id  170 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  170 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  170 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 171

The Responsive Environmental Assessment Commercially Hosted, satellite id  171 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  171 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  171 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 172

The Responsive Environmental Assessment Commercially Hosted, satellite id  172 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  172 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  172 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 173

The Responsive Environmental Assessment Commercially Hosted, satellite id  173 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  173 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  173 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 175

The Responsive Environmental Assessment Commercially Hosted, satellite id  175 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  175 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  175 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 176

The Responsive Environmental Assessment Commercially Hosted, satellite id  176 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  176 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  176 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 180

The Responsive Environmental Assessment Commercially Hosted, satellite id  180 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  180 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  180 (from Master/CDFglobalAttributes/Source_name)

Dosimeter measurements from the Responsive Environmental Assessment Commerically Hosted satellite 181

The Responsive Environmental Assessment Commercially Hosted, satellite id  181 (from all.xml/observatory/description/@short)

, The Responsive Environmental Assessment Commercially Hosted (REACH)  version-3 Data for,vehical ID  181 (from all.xml/instrument/description/@short)

The Responsive Environmental Assessment Commercially Hosted, satellite id  181 (from Master/CDFglobalAttributes/Source_name)

Rocket Experiment for Neutral Upwelling 2, RENU2, Mission Overview Web Page, University of New Hampshire

Rocket Experiment for Neutral Upwelling 2, RENU2, Instrument Overview Web Page, Lynch Rocket Lab, Dartmouth University

UNH Web Page for the Instrumentation onboard the RENU2 Sounding Rocket

Lessard, M.R., Fritz, B., Sadler, B., Cohen, I., Kenward, D., Godbole, N., Clemmons, J.H., Hecht, J.H., Lynch, K.A., Harrington, M., Roberts, T.M., Hysell, D., Crowley, G., Sigernes, F., Syrjasuo, M., Ellingson, P., Partamies, N., Moen, J., Clausen, L., Oksavik, K., and T. Yeoman, Overview of the Rocket Experiment for Neutral1, Upwelling Sounding Rocket 2 (RENU2), Geophys. Res. Lett., 46, https://doi.org/10.1029/2018GL081885

SPDF/CDAWeb. Please also acknowledge the data producer: Marc Lessard, David Hysell at University of New Hampshire, Cornell University

SPDF/SSCWeb. Please also acknowledge the data producer: Marc Lessard, David Hysell at University of New Hampshire, Cornell University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Marc Lessard, David Hysell at University of New Hampshire, Cornell University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/efield/2015/renu2_h0_efield_20151213_v01.cdf. The most common cadence, 1007080 [ns] = PT0.001007S, occurred for 47.2874% of the 183994 timesteps. 

Rocket Experiment for Neutral Upwelling 2 (from all.xml/observatory/description/@short)

COrnell Wire BOom Yo-yo (from all.xml/instrument/description/@short)

Rocket Experiment for Neutral Upwelling 2 (from Master/CDFglobalAttributes/Source_name)

electric field - perpendicular East in geomagnetic coordinates, despun with v x B component removed

electric field - perpendicular North in geomagnetic coordinates, despun with v x B component removed

SPDF/CDAWeb. Please also acknowledge the data producer: Marc Lessard at University of New Hampshire

SPDF/SSCWeb. Please also acknowledge the data producer: Marc Lessard at University of New Hampshire

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Marc Lessard at University of New Hampshire

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/eplas/2015/renu2_h0_eplas_20151213_v01.cdf. The most common cadence, 42000000 [ns] = PT0.042S, occurred for all 11403 timesteps. 

Electron Plasma Instrument (from all.xml/instrument/description/@short)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => epoch_skin, @2 => epoch_electrons.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => epoch_skin, @2 => epoch_electrons.)

Electron Retarding Potential Analyzer (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/erpamain/2015/renu2_h0_erpamain_20151213_v01.cdf. The most common cadence, 256012000 [ns] = PT0.256012S, occurred for 31.9710% of the 618 timesteps. 

Counts based on variable 'epoch_skin' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/erpamain/2015/renu2_h0_erpamain_20151213_v01.cdf. The most common cadence, 488000 [ns] = PT0.000488000S, occurred for 37.9306% of the 432409 timesteps. 

Counts based on variable 'epoch_electrons' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/erpamain/2015/renu2_h0_erpamain_20151213_v01.cdf. The most common cadence, 127991000 [ns] = PT0.127991S, occurred for 41.7565% of the 1859 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/erpasub/2015/renu2_h0_erpasub_20151213_v01.cdf. The most common cadence, 256012000 [ns] = PT0.256012S, occurred for 30.1905% of the 618 timesteps. 

Counts based on variable 'epoch_skin' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/erpasub/2015/renu2_h0_erpasub_20151213_v01.cdf. The most common cadence, 488000 [ns] = PT0.000488000S, occurred for 38.9594% of the 467045 timesteps. 

Counts based on variable 'epoch_electrons' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/erpasub/2015/renu2_h0_erpasub_20151213_v01.cdf. The most common cadence, 127991000 [ns] = PT0.127991S, occurred for 42.6373% of the 1995 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Marc Lessard at University of New Hampshire, Cornell University

SPDF/SSCWeb. Please also acknowledge the data producer: Marc Lessard at University of New Hampshire, Cornell University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Marc Lessard at University of New Hampshire, Cornell University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/fgm/2015/renu2_h0_fgm_20151213_v01.cdf. The most common cadence, 1000000 [ns] = PT0.001S, occurred for 99.9998% of the 659998 timesteps. 

Magnetic Field Instrument (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: James Clemmons at University of New Hampshire

SPDF/SSCWeb. Please also acknowledge the data producer: James Clemmons at University of New Hampshire

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: James Clemmons at University of New Hampshire

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/ig2/2015/renu2_h0_ig2_20151213_v01.cdf. The most common cadence, 1000000 [ns] = PT0.001S, occurred for 98.9291% of the 460139 timesteps. 

Thermospheric Science (from Master/CDFglobalAttributes/Discipline)

RENU2 PMT counts converted to Rayleighs and background subtracted

SPDF/CDAWeb. Please also acknowledge the data producer: Jim Hecht at University of New HampshireAerospace Corporation

SPDF/SSCWeb. Please also acknowledge the data producer: Jim Hecht at University of New HampshireAerospace Corporation

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Jim Hecht at University of New HampshireAerospace Corporation

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_green.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_green.)

Photomultiplier Tube (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/pmt/2015/renu2_h0_pmt_20151213_v02.cdf. The most common cadence, 4000000 [ns] = PT0.004S, occurred for 95.7158% of the 201769 timesteps. 

Counts based on variable 'Epoch_green' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/pmt/2015/renu2_h0_pmt_20151213_v02.cdf. The most common cadence, 4000000 [ns] = PT0.004S, occurred for 95.7158% of the 201769 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/uvpmt/2015/renu2_h0_uvpmt_20151213_v01.cdf. The most common cadence, 1007080 [ns] = PT0.001007S, occurred for 33.1392% of the 160725 timesteps. 

Ultraviolet Photomultiplier Tube (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/renu2/vlf/2015/renu2_h0_vlf_20151213_v01.cdf. The most common cadence, 102400000 [ns] = PT0.1024S, occurred for 35.8214% of the 979 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rosetta/helio1day/rosetta_helio1day_position_20040303_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 4686 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/rosetta/helio1hr/rosetta_helio1hr_position_20040303_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 110375 timesteps. 

1-second averaged data***Important Notes*** on Accuracy of VperpM_MF (meridional),VperpZ_MF (zonal), and VparaMF (parallel) components.Geophysical flow components VperpM_MF, VperpZ_MF, and VparaMF are converted from flow velocities, Vx, Vy, and Vz measured in the S/C coordinate system. Vx points along the S/C trajectory vector, Vz is in the nadir direction, and Vy points to the right of the S/C trajectory vector (in the anti-angular momentum direction).1) Vx, Vy, and Vz are measured flow velocities at S/C coordinate in the Earth-centered Inertia Coordinate System (non-rotating) (ECI coordinate).2) VperZ_MF, VperM_MF, and VparaMF are geophysical flows in the Earth-centered Fixed Coordinated System (rotate with the Earth) (ECF coordinate).3) Uncertainty of +-(37.8-75.45) m/s in Vx based on 0.5% - 1% error in fitting could be introduced to all geophysical flow components.4) VperpM_MF at low latitude is almost identical to (-Vz). No Vx is included so that it is very reliable.5) Uncertainties from Vx could exist in VperpZ_MF and VparaMF.6) VperpZ_MF and VparaMF can be used to study the relative changes in flow velocity due to  geophysical effects.But can not be used to study the long-term variations because the result could be biased by the uncertainty in Vx.

SPDF/CDAWeb. Please also acknowledge the data producer: Shin-Yi Su at Institute of Space Science, National Central University, Taiwan, R.O.C.

SPDF/SSCWeb. Please also acknowledge the data producer: Shin-Yi Su at Institute of Space Science, National Central University, Taiwan, R.O.C.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Shin-Yi Su at Institute of Space Science, National Central University, Taiwan, R.O.C.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/formosat-rocsat/formosat-1/ipei/1999/rs_k0_ipei_19990311_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 99.9364% of the 73910 timesteps. 

Ionospheric Plasma and Electrodynamics Instrument (from all.xml/observatory/description/@short)

Ionospheric Plasma and Electrodynamics Instrument (from all.xml/instrument/description/@short)

Ionospheric Studies (from Master/CDFglobalAttributes/Discipline)

ROCSAT-1(FORMOSAT-1) (from Master/CDFglobalAttributes/Source_name)

Ionospheric Plasma and Electrodynamics Instrument (from Master/CDFglobalAttributes/Source_name)

Ion drift in S/C LVLH coordinates > x component = along the S/C trajectory vector

--------------------------> y component = opposite to angular momentum

--------------------------> z component = toward the Earth Center

Ion drift in Magnetic Field Coordinates > Component parallel to MF

--------------------------> Meridional component perpendicular to MF

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sakigake/helio1day/sakigake_helio1day_position_19850121_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 99.9154% of the 4723 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sakigake/helio1hr/sakigake_helio1hr_position_19850121_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.9974% of the 113444 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/saturn_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/saturn_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

Ionospheric parameters derived from quarter-hourly ionogramsRef: Grubb,RN The NOAA SEL HF Radar system (ionospheric sounder) NOAA Tech Memo ERL SEL-55, Space Environ Lab, Boulder, CO, 1979Ref: Jarvis,MJ & Dudeney ,JR Reduction of ambiguities in HF radar resultsthrough a revised receiving array & sounding pattern. Radio Sci 21, 151-158, 1986Ref: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME), in GGS Instrument Papers, submitted to Space Science ReviewsInfo:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UKE-mail: 19989::MORRISONQUALITY_FLAG Comprised of several additive values each with a specific meaning:-0 okay,+1 <6 echoes used for fmin,+2 <6 echoes for fEmax,+4 <6 echoes for fFmax,+8 fmin approx= min tx frequency,+16 fEmax approx= max tx frequency,+32 fFmax approx= max tx  frequency (tx=transmitter)eg 37 indicates <6 echoes used for fmin & fFmax, & fFmax approx= max tx freq

SPDF/CDAWeb. Please also acknowledge the data producer: J. Dudeney at British Antarctic Survey

SPDF/SSCWeb. Please also acknowledge the data producer: J. Dudeney at British Antarctic Survey

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Dudeney at British Antarctic Survey

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sesame/ais/1992/se_k0_ais_19920901_v01.cdf. The most common cadence, 900000 [ms] = PT15M, occurred for 98.9247% of the 92 timesteps. 

Satellite Experiments Simultaneous with Antarctic Measurements (from all.xml/observatory/description/@short)

Advanced Ionospheric Sounder (from all.xml/instrument/description/@short)

Max E-region plasma frequency  (-88.88=Insuf. echoes,-99.99=no echoes)

Max F-region plasma frequency  (-88.88=Insuf. echoes,-99.99=no echoes)

Measurements made looking in South and East directions (positive) Ref1: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME),in GGS Instrument Papers, submitted to Space Science Reviews.Ref2: Nature,317,p45 1985. Ref3: R.D.Stewart, PhD Thesis, Univ of Ulster, 1986Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UKE-mail: 19989::MORRISON

SPDF/CDAWeb. Please also acknowledge the data producer: J.R. Dudeney at British Antarctic Survey

SPDF/SSCWeb. Please also acknowledge the data producer: J.R. Dudeney at British Antarctic Survey

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J.R. Dudeney at British Antarctic Survey

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sesame/fpi/1995/se_k0_fpi_19950913_v01.cdf. The most common cadence, 1800000 [ms] = PT30M, occurred for all 3 timesteps. 

Fabry-Perot  Interferometer (from all.xml/instrument/description/@short)

South horizontal velocity from line-of-sight velocity at 30 degrees elevation

East horizontal velocity from line-of-sight velocity at 30 degrees elevation

Refers to the wavelength of the OI (558 or 630nm) emission line used

H, D and Z components of the earth's magnetic fieldMeasuring variation of field relative to arbitrary baseline. Accurate to 1nT1 minute data representing 'spot' values of the 1Hz samplingRef: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME), in GGS Instrument Papers, submitted to Space Science ReviewsInfo:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UKE-mail: 19989::MORRISON

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sesame/mag/1993/se_k0_mag_19931209_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.8608% of the 1435 timesteps. 

Equivalent overhead absorption measured 45 degrees to vertical in N,S,E,W directions, but in an L-shell-aligned coordinate system (ie rotated 17 degrees anti-clockwise from geographic). Preliminary Quiet-Day Curve used.1 minute data represent 'spot' values of the 1Hz samplingAccurate to 0.05dB, but possible baseline uncertainties of +/-0.5dBRef1: The multiple riometer system at Halley, Antarctica, in British Antarctic Survey Bulletin, no 72, p13-23, 1986Ref2: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME), in GGS Instrument Papers, submitted to Space Science ReviewsInfo:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UKE-mail: 19989::MORRISON

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sesame/rio/1994/se_k0_rio_19940102_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.8486% of the 1319 timesteps. 

30MHz Riometer Array (from all.xml/instrument/description/@short)

Omni-directional intensities in 2 narrow passband filters centred on 1kHz & 3kHzRef1: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME),in GGS Instrument Papers submitted to Space Science Reviews.Ref2: VERSIM Newsletter No.4, p7 1992.Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UKE-mail: 19989::MORRISON

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sesame/vlf/1992/se_k0_vlf_19920722_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

VLF/ELF LoggerExperiment (VELOX) (from all.xml/instrument/description/@short)

Omni-directional intensity (narrow passband filter centred on 1kHz), scalar

Omni-directional intensity (narrow passband filter centred on 3kHz), scalar

Barth, C. A. and S. M. Bailey, Comparison of a thermospheric photochemical model with SNOE observations of nitric oxide, J. Geophys. Res., doi:10.1029/2003JA010227, 2004.

SPDF/CDAWeb. Please also acknowledge the data producer: Charles A. Barth at LASP/CU

SPDF/SSCWeb. Please also acknowledge the data producer: Charles A. Barth at LASP/CU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Charles A. Barth at LASP/CU

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/snoe/NO_uvs/1min_cdaweb/l3_geo/1998/snoe_l3_geo_19980311_v01.cdf. The most common cadence, 84000 [ms] = PT1M24S, occurred for 27.1047% of the 132 timesteps. 

Student Nitric Oxide Explorer (from all.xml/observatory/description/@short)

Geographic Coordinates (from all.xml/instrument/description/@short)

Student Nitric Oxide Explorer (from Master/CDFglobalAttributes/Source_name)

Level 3A merged XPS and EGS (from Master/CDFglobalAttributes/Data_type)

Time tag rounded to nearest msecond. Denotes beginning of interval.

NO (nitric oxide) density [1/cm^3] vs altitude - average over  geographic latitude bins 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/snoe/NO_uvs/1min_cdaweb/l3_mag/1998/snoe_l3_mag_19980311_v01.cdf. The most common cadence, 84000 [ms] = PT1M24S, occurred for 11.9403% of the 56 timesteps. 

Magnetic Coordinates (from all.xml/instrument/description/@short)

NO (nitric oxide) density [1/cm^3] vs altitude - average over geomagnetic latitude bins

Description of the CELIAS-PM instrument and scientific scope can be found on CELIAS homepage http://www.ieap.uni-kiel.de/et/soho/celias/ and SOHO homepage http://sohowww.nascom.nasa.gov/ The data was created from the original ASCII dataset at https://soho.nascom.nasa.gov/data/archive.htmlThe data was created from the original ASCII dataset at https://soho.nascom.nasa.gov/data/archive.html

Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO. Sol Phys 162, 441–481 (1995)

SPDF/CDAWeb. Please also acknowledge the data producer: Robert Wimmer-Schweingruber (wimmer@physik.uni-kiel.de) at Christian Albrechts Universitat

SPDF/SSCWeb. Please also acknowledge the data producer: Robert Wimmer-Schweingruber (wimmer@physik.uni-kiel.de) at Christian Albrechts Universitat

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Robert Wimmer-Schweingruber (wimmer@physik.uni-kiel.de) at Christian Albrechts Universitat

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/celias/pm_30s/1996/soho_celias-pm_30s_19960120_v02.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 84.2726% of the 643 timesteps. 

Solar Heliospheric Observatory (from all.xml/observatory/description/@short)

Solar Heliospheric Observatory (from Master/CDFglobalAttributes/Source_name)

30 second resolution (from Master/CDFglobalAttributes/Data_type)

Start Time, number of milliseconds since 01-Jan-0000 00:00:00.000

Description of the CELIAS-PM instrument and scientific scope can be found on CELIAS homepage http://www.ieap.uni-kiel.de/et/soho/celias/ and SOHO homepage http://sohowww.nascom.nasa.gov/ The data was created from the original ASCII dataset at https://soho.nascom.nasa.gov/data/archive.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/celias/pm_5min/1996/soho_celias-pm_5min_19960120_v02.cdf. The most common cadence, 301000 [ms] = PT5M1S, occurred for 27.9070% of the 12 timesteps. 

Description of the CELIAS-SEM instrument and scientific scope can befound on CELIAS homepage http://www.ieap.uni-kiel.de/et/soho/celias/ and SOHO homepage http://sohowww.nascom.nasa.gov/ Version 4 Science Product Release Notes are available athttps://lasp.colorado.edu/eve/data_access/eve_data/lasp_soho_sem_data/long/LASP_SOHO_SEM_release_notes_v4.pdfThe data was created from the original ASCII dataset at https://soho.nascom.nasa.gov/data/archive.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/celias/sem_15s/1995/soho_celias-sem_15s_19951221_v04.cdf. The most common cadence, 15034 [ms] = PT15.034S, occurred for 34.0594% of the 1939 timesteps. 

Solar Extreme-Ultra-Violet Monitor (from all.xml/instrument/description/@short)

Ultraviolet Observations (from Master/CDFglobalAttributes/Discipline)

15 second resolution (from Master/CDFglobalAttributes/Data_type)

Centered Time, number of milliseconds since 01-Jan-0000 00:00:00.000

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/celias/sem_1day/1995/soho_celias-sem_1day_19950101_v04.01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 364 timesteps. 

Description of the COSTEP-EPHIN instrument and scientific scope can be found on the COSTEP homepage http://www.ieap.uni-kiel.de/et/ag-heber/costep/ and on the SOHO homepage http://sohowww.nascom.nasa.gov/Documentation of the COSTEP-EPHIN Level3 data product, including energy ranges of Level3 channels and status flag description (see Section 5), is available at http://ulysses.physik.uni-kiel.de/costep/level3/l3i/DOCUMENTATION-COSTEP-EPHIN-L3-20220201.pdfThe data was created from the original ASCII dataset at https://soho.nascom.nasa.gov/data/archive.html

Müller-Mellin, R., Kunow, H., Fleißner, V. et al. COSTEP - Comprehensive Suprathermal and Energetic Particle Analyser. Sol Phys 162, 483–504 (1995)

SPDF/CDAWeb. Please also acknowledge the data producer: Bernd Heber (heber@physik.uni-kiel.de) at Christian Albrechts Universitat

SPDF/SSCWeb. Please also acknowledge the data producer: Bernd Heber (heber@physik.uni-kiel.de) at Christian Albrechts Universitat

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Bernd Heber (heber@physik.uni-kiel.de) at Christian Albrechts Universitat

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/costep/ephin_l3i-10min/1995/soho_costep-ephin_l3i-10min_19950101_v01.01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 99.9710% of the 3442 timesteps. 

Electron Proton Helium Instrument (from all.xml/instrument/description/@short)

L3 10 minute intensities (from Master/CDFglobalAttributes/Data_type)

Start time, number of milliseconds since 01-Jan-0000 00:00:00.000

Proton intensity in 4 energy ranges (4.3-7.8, 7.8-25, 25-40.9, 40.9-53 MeV)

Proton systematic uncertainty in 4 energy ranges (4.3-7.8, 7.8-25, 25-40.9, 40.9-53 MeV)

Proton statistical uncertainty in 4 energy ranges (4.3-7.8, 7.8-25, 25-40.9, 40.9-53 MeV)

He intensity in 4 energy ranges (4.3-7.8, 7.8-25, 25-40.9, 40.9-53 MeV/n)

He systematic uncertainty in 4 energy ranges (4.3-7.8, 7.8-25, 25-40.9, 40.9-53 MeV/n)

He statistical uncertainty in 4 energy ranges (4.3-7.8, 7.8-25, 25-40.9, 40.9-53 MeV/n)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/costep/ephin_l3i-1day/1995/soho_costep-ephin_l3i-1day_19950101_v01.01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 23 timesteps. 

L3 1 day intensities (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/costep/ephin_l3i-1hr/1995/soho_costep-ephin_l3i-1hr_19950101_v01.01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.8258% of the 573 timesteps. 

L3 1 hour intensities (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/costep/ephin_l3i-1min/1995/soho_costep-ephin_l3i-1min_19950101_v01.01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 98.0555% of the 32778 timesteps. 

L3 1 minute intensities (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/costep/ephin_l3i-30min/1995/soho_costep-ephin_l3i-30min_19950101_v01.01.cdf. The most common cadence, 1800000 [ms] = PT30M, occurred for 99.9129% of the 1147 timesteps. 

L3 30 minute intensities (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/costep/ephin_l3i-5min/1995/soho_costep-ephin_l3i-5min_19950101_v01.01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for 99.9273% of the 6875 timesteps. 

Level3 5 minute intensities (from Master/CDFglobalAttributes/Data_type)

Description of the ERNE instrument and scientific scope can be found on the ERNE homepage https://srl.utu.fi/projects/erne/ and on the SOHO homepage http://sohowww.nascom.nasa.gov/ Description of the ERNE-HED Level2 data, including caveats,actual energy ranges of proton and He-4 channels,and status word description, is available at https://export.srl.utu.fi/export_data_description.txtReference:Torsti, J., Valtonen, E., Lumme, M., et al. 1995: Energetic particle experiment ERNE. Sol Phys 162, 505-531.https://doi.org/10.1007/BF00733438The data was created from the original ASCII dataset at https://export.srl.utu.fi/

Torsti, J., Valtonen, E., Lumme, M. et al. Energetic particle experiment ERNE. Sol Phys 162, 505–531 (1995)

SPDF/CDAWeb. Please also acknowledge the data producer: Rami Vainio (rami.vainio@utu.fi) at Space Research Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Rami Vainio (rami.vainio@utu.fi) at Space Research Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Rami Vainio (rami.vainio@utu.fi) at Space Research Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/erne/hed_l2-1min/1996/soho_erne-hed_l2-1min_19960507_v01.cdf. The most common cadence, 59953 [ms] = PT59.953S, occurred for 87.3418% of the 345 timesteps. 

High Energy Detector (from all.xml/instrument/description/@short)

Level2 1 minute resolution (from Master/CDFglobalAttributes/Data_type)

Status word, see TEXT. Note: CDF_UINT4 data was converted to HAPI double.

Description of the ERNE instrument and scientific scope can be found on the ERNE homepage https://srl.utu.fi/projects/erne/ and on the SOHO homepage http://sohowww.nascom.nasa.gov/ Description of the ERNE-LED Level2 data, including caveats,actual energy ranges of proton and He-4 channels,and status word description, is available at https://export.srl.utu.fi/export_data_description.txtReference:Torsti, J., Valtonen, E., Lumme, M., et al. 1995: Energetic particle experiment ERNE. Sol Phys 162, 505-531.https://doi.org/10.1007/BF00733438The data was created from the original ASCII dataset at https://export.srl.utu.fi/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/erne/led_l2-1min/1996/soho_erne-led_l2-1min_19960507_v01.cdf. The most common cadence, 59953 [ms] = PT59.953S, occurred for 87.3418% of the 345 timesteps. 

Low Energy Detector (from all.xml/instrument/description/@short)

Description of the ERNE instrument and scientific scope can be found on the ERNE homepage https://srl.utu.fi/projects/erne/ and on the SOHO homepage https://sohowww.nascom.nasa.gov/ Reference:Torsti, J., Valtonen, E., Lumme, M., et al. 1995: Energetic particle experiment ERNE. Sol Phys 162, 505-531.https://doi.org/10.1007/BF00733438

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/erne/heavy-ion-1hr/1996/soho_erne_heavy-ion-1hr_19960101_v01.01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 8783 timesteps. 

Energetic and Relativistic Nuclei and Electron experiment (from all.xml/instrument/description/@short)

Heavy ion 1 hour resolution (from Master/CDFglobalAttributes/Data_type)

Start of accumulation period, number of milliseconds since 01-Jan-0000 00:00:00.000

Accumulation time. Note: CDF_UINT4 data was converted to HAPI double.

C counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

N counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

O counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

Ne counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

Mg counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

Si counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

C, N, O counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

Si-Ar counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

Fe, Co, Ni counts per accumulation period in 10 energy ranges (2.7-200 MeV/n)

Description of the ERNE instrument and scientific scope can be found on the ERNE homepage https://srl.utu.fi/projects/erne/ and on the SOHO homepage https://sohowww.nascom.nasa.gov/Reference:Torsti, J., Valtonen, E., Lumme, M., et al. 1995: Energetic particle experiment ERNE. Sol Phys 162, 505-531.https://doi.org/10.1007/BF00733438

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/erne/heavy-ion-5min/1996/soho_erne_heavy-ion-5min_19960101_v01.01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 105407 timesteps. 

Heavy ion 5 minute resolution (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/helio1day/soho_helio1day_position_19951203_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 10619 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/helio1hr/soho_helio1hr_position_19951203_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 259079 timesteps. 

Merged hourly magnetic field, plasma, proton fluxes, and ephermis data of Solar Orbiter

COHO hourly and daily SOLO data were made using SOLO high resolution data from CDAWeb at https://cdaweb.gsfc.nasa.gov/. The name of the original  plasma data is '\SOLO_L2_SWA-PAS-GRND-MOM\', [ parameter names: proton bulk velocity in the RTN frame, proton density, proton temperature (Only Good Quality).] The name of  the original magnetic field data is \'SOLO_L2_MAG-RTN-NORMAL-1-MINUTE\'. The heliocentric trajectory data is from HelioWeb at https://omniweb.gsfc.nasa.gov/coho/helios/heli.htmlThis file includes the SOLO MAG magnetometer data, and density, velocity and temperature of the solar wind protons measured by the Solar Wind Analyzer (SWA). About SOLO data in COHOWeb Solar Orbiter https://omniweb.gsfc.nasa.gov/coho and https://cdaweb.gsfc.nasa.gov/.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/coho1hr_magplasma/2020/solo_coho1hr_merged_mag_plasma_20200101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

1 Hour Time Resolution from COHOWeb (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/helio1day/solo_helio1day_position_20200211_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 3932 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/helio1hr/solo_helio1hr_position_20200211_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 94439 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, Burst, Electrons, Close mode

Energetic Particle Detector (EPD). Instrument suite, part of the scientific payload aboard the Solar Orbiter mission, dedicated to the study of solar energetic particles. EPD measures electrons, protons and heavy ions with high temporal resolution over a wide energy range, from suprathermal energies to several hundreds of MeV/nucleon. It is composed of four units: SupraThermal Electrons and Protons (STEP), Electron Proton Telescope (EPT), Suprathermal Ion Spectrograph (SIS) and High Energy Telescope (HET).https://doi.org/10.1051/0004-6361/201935287

SPDF/CDAWeb. Please also acknowledge the data producer: J. Rodriguez-Pacheco at Space Research Group, Universidad de Alcala

SPDF/SSCWeb. Please also acknowledge the data producer: J. Rodriguez-Pacheco at Space Research Group, Universidad de Alcala

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J. Rodriguez-Pacheco at Space Research Group, Universidad de Alcala

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/asun-burst-ele-close/2020/solo_l2_epd-ept-asun-burst-ele-close_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, Burst, Electrons, Close mode (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, Burst, Ions

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/asun-burst-ion/2020/solo_l2_epd-ept-asun-burst-ion_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, Burst, Ions (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, High Cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/asun-hcad/2020/solo_l2_epd-ept-asun-hcad_20200513_v03.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, High Cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Anti-Sun Direction, Rates

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => EPOCH, @1 => EPOCH_1.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => EPOCH, @1 => EPOCH_1.)

Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/asun-rates/2020/solo_l2_epd-ept-asun-rates_20200513_v03.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/asun-rates/2020/solo_l2_epd-ept-asun-rates_20200513_v03.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, North direction, Burst, Electrons, Close mode

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/north-burst-ele-close/2020/solo_l2_epd-ept-north-burst-ele-close_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, North direction, Burst, Electrons, Close mode (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, North direction, Burst, Ions

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/north-burst-ion/2020/solo_l2_epd-ept-north-burst-ion_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, North direction, Burst, Ions (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, North Direction, High Cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/north-hcad/2020/solo_l2_epd-ept-north-hcad_20200513_v03.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, North direction, High Cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, North Direction, Rates

Energetic Particle Detector, Electron Proton Telescope, North direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/north-rates/2020/solo_l2_epd-ept-north-rates_20200513_v03.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/north-rates/2020/solo_l2_epd-ept-north-rates_20200513_v03.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, South direction, Burst, Electrons, Close mode

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/south-burst-ele-close/2020/solo_l2_epd-ept-south-burst-ele-close_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, South direction, Burst, Electrons, Close mode (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, South direction, Burst, Ions

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/south-burst-ion/2020/solo_l2_epd-ept-south-burst-ion_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, South direction, Burst, Ions (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, South direction, High Cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/south-hcad/2020/solo_l2_epd-ept-south-hcad_20200513_v03.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, South direction, High Cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, South Direction, Rates

Energetic Particle Detector, Electron Proton Telescope, South direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/south-rates/2020/solo_l2_epd-ept-south-rates_20200513_v03.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/south-rates/2020/solo_l2_epd-ept-south-rates_20200513_v03.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Sun direction, Burst, Electrons, Close mode

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/sun-burst-ele-close/2020/solo_l2_epd-ept-sun-burst-ele-close_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, Sun direction, Burst, Electrons, Close mode (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Sun direction, Burst, Ions

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/sun-burst-ion/2020/solo_l2_epd-ept-sun-burst-ion_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, Sun direction, Burst, Ions (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Sun direction, High Cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/sun-hcad/2020/solo_l2_epd-ept-sun-hcad_20200513_v03.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Energetic Particle Detector, Electron Proton Telescope, Sun direction, High Cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron Proton Telescope, Sun Direction, Rates

Energetic Particle Detector, Electron Proton Telescope, Sun direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/sun-rates/2020/solo_l2_epd-ept-sun-rates_20200513_v03.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/ept/sun-rates/2020/solo_l2_epd-ept-sun-rates_20200513_v03.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, Anti-Sun direction, Burst

Energetic Particle Detector, High Energy Telescope, Anti-Sun direction, Burst (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-burst/2020/solo_l2_epd-het-asun-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-burst/2020/solo_l2_epd-het-asun-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 87.7095% of the 157 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, Anti-Sun direction, Rates

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => EPOCH, @1 => EPOCH_4, @2 => EPOCH_1, @3 => EPOCH_2, @4 => EPOCH_3.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => EPOCH, @1 => EPOCH_4, @2 => EPOCH_1, @3 => EPOCH_2, @4 => EPOCH_3.)

Energetic Particle Detector, High Energy Telescope, Anti-Sun direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-rates/2020/solo_l2_epd-het-asun-rates_20200513_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-rates/2020/solo_l2_epd-het-asun-rates_20200513_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-rates/2020/solo_l2_epd-het-asun-rates_20200513_v02.cdf. The most common cadence, 30000051072 [ns] = PT30.000051S, occurred for 59.6040% of the 1716 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-rates/2020/solo_l2_epd-het-asun-rates_20200513_v02.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/asun-rates/2020/solo_l2_epd-het-asun-rates_20200513_v02.cdf. The most common cadence, 300000510208 [ns] = PT5M0.00051S, occurred for 77.3519% of the 222 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, North direction, Burst

Energetic Particle Detector, High Energy Telescope, North direction, Burst (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-burst/2020/solo_l2_epd-het-north-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-burst/2020/solo_l2_epd-het-north-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 87.7095% of the 157 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, North direction, Rates

Energetic Particle Detector, High Energy Telescope, North direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-rates/2020/solo_l2_epd-het-north-rates_20200513_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-rates/2020/solo_l2_epd-het-north-rates_20200513_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-rates/2020/solo_l2_epd-het-north-rates_20200513_v02.cdf. The most common cadence, 30000051072 [ns] = PT30.000051S, occurred for 59.6040% of the 1716 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-rates/2020/solo_l2_epd-het-north-rates_20200513_v02.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/north-rates/2020/solo_l2_epd-het-north-rates_20200513_v02.cdf. The most common cadence, 300000510208 [ns] = PT5M0.00051S, occurred for 77.3519% of the 222 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, South direction, Burst

Energetic Particle Detector, High Energy Telescope, South direction, Burst (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-burst/2020/solo_l2_epd-het-south-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-burst/2020/solo_l2_epd-het-south-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 87.7095% of the 157 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, South direction, Rates

Energetic Particle Detector, High Energy Telescope, South direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-rates/2020/solo_l2_epd-het-south-rates_20200513_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-rates/2020/solo_l2_epd-het-south-rates_20200513_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-rates/2020/solo_l2_epd-het-south-rates_20200513_v02.cdf. The most common cadence, 30000051072 [ns] = PT30.000051S, occurred for 59.6040% of the 1716 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-rates/2020/solo_l2_epd-het-south-rates_20200513_v02.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/south-rates/2020/solo_l2_epd-het-south-rates_20200513_v02.cdf. The most common cadence, 300000510208 [ns] = PT5M0.00051S, occurred for 77.3519% of the 222 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, Sun direction, Burst

Energetic Particle Detector, High Energy Telescope, Sun direction, Burst (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-burst/2020/solo_l2_epd-het-sun-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-burst/2020/solo_l2_epd-het-sun-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 87.7095% of the 157 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, High Energy Telescope, Sun direction, Rates

Energetic Particle Detector, High Energy Telescope, Sun direction, Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-rates/2020/solo_l2_epd-het-sun-rates_20200513_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.6724% of the 10138 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-rates/2020/solo_l2_epd-het-sun-rates_20200513_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 71.3700% of the 61663 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-rates/2020/solo_l2_epd-het-sun-rates_20200513_v02.cdf. The most common cadence, 30000051072 [ns] = PT30.000051S, occurred for 59.6040% of the 1716 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-rates/2020/solo_l2_epd-het-sun-rates_20200513_v02.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.5115% of the 1101 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/het/sun-rates/2020/solo_l2_epd-het-sun-rates_20200513_v02.cdf. The most common cadence, 300000510208 [ns] = PT5M0.00051S, occurred for 77.3519% of the 222 timesteps. 

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Helium histogram

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/a-hehist/2020/solo_l2_epd-sis-a-hehist_20200425_v03.cdf. The most common cadence, 1800003061120 [ns] = PT30M0.003061S, occurred for 40.4255% of the 19 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Helium histogram (from all.xml/instrument/description/@short)

Helium mass histogram. Detected counts per mass bin for particles in the energy range 0.5 - 2 MeV/n.

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle rates, fast cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/a-rates-fast/2020/solo_l2_epd-sis-a-rates-fast_20200615t122224-20200615t123724_v05.cdf. The most common cadence, 3000005120 [ns] = PT3.000005S, occurred for 56.0000% of the 168 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle rates, fast cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle rates, medium cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/a-rates-medium/2020/solo_l2_epd-sis-a-rates-medium_20200402_v06.cdf. The most common cadence, 30000050304 [ns] = PT30.00005S, occurred for 54.8571% of the 864 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle rates, medium cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle rates, slow cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/a-rates-slow/2020/solo_l2_epd-sis-a-rates-slow_20200402_v06.cdf. The most common cadence, 1800003018752 [ns] = PT30M0.003019S, occurred for 57.6923% of the 15 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle rates, slow cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Helium histogram

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/b-hehist/2020/solo_l2_epd-sis-b-hehist_20200425_v03.cdf. The most common cadence, 1800003061120 [ns] = PT30M0.003061S, occurred for 40.4255% of the 19 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Helium histogram (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle rates, fast cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/b-rates-fast/2020/solo_l2_epd-sis-b-rates-fast_20200615t122224-20200615t123724_v05.cdf. The most common cadence, 3000005120 [ns] = PT3.000005S, occurred for 56.0000% of the 168 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle rates, fast cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle rates, medium cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/b-rates-medium/2020/solo_l2_epd-sis-b-rates-medium_20200402_v06.cdf. The most common cadence, 30000050304 [ns] = PT30.00005S, occurred for 54.8571% of the 864 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle rates, medium cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle rates, slow cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/sis/b-rates-slow/2020/solo_l2_epd-sis-b-rates-slow_20200402_v06.cdf. The most common cadence, 1800003018752 [ns] = PT30M0.003019S, occurred for 57.6923% of the 15 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle rates, slow cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, SupraThermal Electrons and Protons, Burst

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/step/burst/2020/solo_l2_epd-step-burst_20200615t122228-20200615t123728_v02.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 77.5556% of the 698 timesteps. 

Energetic Particle Detector, SupraThermal Electrons and Protons, Burst (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, SupraThermal Electrons and Protons, High Cadence

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/step/hcad/2020/solo_l2_epd-step-hcad_20200430_v02.cdf. The most common cadence, 5000008448 [ns] = PT5.000008S, occurred for 58.7013% of the 10143 timesteps. 

Energetic Particle Detector, SupraThermal Electrons and Protons, High Cadence (from all.xml/instrument/description/@short)

Solar Orbiter, Level 2 Data, Energetic Particle Detector, SupraThermal Electrons and Protons, Main product

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/step/main/2021/solo_l2_epd-step-main_20211022_v01.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 74.1432% of the 31866 timesteps. 

Energetic Particle Detector, SupraThermal Electrons and Protons, Main product (from all.xml/instrument/description/@short)

Particle intensities in integral channel (ions + electrons) for pixel 1

Particle intensities in integral channel (ions + electrons) for pixel 2

Particle intensities in integral channel (ions + electrons) for pixel 3

Particle intensities in integral channel (ions + electrons) for pixel 4

Particle intensities in integral channel (ions + electrons) for pixel 5

Particle intensities in integral channel (ions + electrons) for pixel 6

Particle intensities in integral channel (ions + electrons) for pixel 7

Particle intensities in integral channel (ions + electrons) for pixel 8

Particle intensities in integral channel (ions + electrons) for pixel 9

Particle intensities in integral channel (ions + electrons) for pixel 10

Particle intensities in integral channel (ions + electrons) for pixel 11

Particle intensities in integral channel (ions + electrons) for pixel 12

Particle intensities in integral channel (ions + electrons) for pixel 13

Particle intensities in integral channel (ions + electrons) for pixel 14

Particle intensities in integral channel (ions + electrons) for pixel 15

Particle intensities in integral channel (ions + electrons) averaged for all pixels

Particle intensities in magnet channel (ions) averaged for all pixels

Solar Orbiter, Level 2 Data, Energetic Particle Detector, SupraThermal Electrons and Protons, Rates

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l2/step/rates/2020/solo_l2_epd-step-rates_20200430_v02.cdf. The most common cadence, 60000102016 [ns] = PT1M0.000102S, occurred for 76.9284% of the 1107 timesteps. 

Energetic Particle Detector, SupraThermal Electrons and Protons, Rates (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Magnetometer Data in RTN Coordinates in Burst Mode

Solar Orbiter magnetometer data was provided by Imperial College Londonand supported by the UK Space Agency

Publication quality. Take note of Quality Flag and refer to SOL-MAG-DPDD for exceptions

ESA/ESDC. Please also acknowledge the data producer: T. Horbury at The Blackett Laboratory, Imperial College London

Solar Orbiter Archive (SOAR) European Space Agency web interface

Solar Orbiter Data and Metadata via the European Space Agency Table Access Protocol (TAP) server

SPDF/CDAWeb. Please also acknowledge the data producer: T. Horbury at The Blackett Laboratory, Imperial College London

SPDF/SSCWeb. Please also acknowledge the data producer: T. Horbury at The Blackett Laboratory, Imperial College London

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. Horbury at The Blackett Laboratory, Imperial College London

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/rtn-burst/2020/solo_l2_mag-rtn-burst_20200415_v02.cdf. The most common cadence, 7815287 [ns] = PT0.007815S, occurred for 37.2122% of the 4115226 timesteps. 

Level 2 Calibrated Data (from Master/CDFglobalAttributes/Data_type)

Epoch encoded as Terrestrial Time on rotating Earth geoid, ns since J2000

Solar Orbiter L2 Magnetometer Data Derived from Low Latency Data

Dual-sensor, triaxial fluxgate magnetometerdoi:10.1051/0004-6361/201937257

"Publication quality. Take note of Quality Flag and refer to SOL-MAG-DPDD for exceptions

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/rtn-ll/2021/solo_l2_mag-rtn-ll_20210905_v04.cdf. The most common cadence, 7999996841 [ns] = PT7.999997S, occurred for 62.6910% of the 6770 timesteps. 

Solar Orbiter L2 1-Minute Magnetometer Data Derived from Low Latency Data

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/rtn-ll-1min/2021/solo_l2_mag-rtn-ll-1-minute_20210905_v04.cdf. The most common cadence, 59999996424 [ns] = PT59.999996S, occurred for 46.6991% of the 672 timesteps. 

Solar Orbiter Level 2 Magnetometer Data in RTN Coordinates in Normal Mode

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/rtn-normal/2020/solo_l2_mag-rtn-normal_20200415_v02.cdf. The most common cadence, 125004351 [ns] = PT0.125004S, occurred for 48.7509% of the 336954 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/rtn-normal-1-minute/2020/solo_l2_mag-rtn-normal-1-minute_20200415_v02.cdf. The most common cadence, 59999996424 [ns] = PT59.999996S, occurred for 46.6991% of the 672 timesteps. 

Solar Orbiter Level 2 Magnetometer Data in Spacecraft Reference Frame in Burst Mode

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/srf-burst/2020/solo_l2_mag-srf-burst_20200415_v02.cdf. The most common cadence, 7815287 [ns] = PT0.007815S, occurred for 37.2122% of the 4115226 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/srf-ll/2021/solo_l2_mag-srf-ll_20210905_v05.cdf. The most common cadence, 7999996841 [ns] = PT7.999997S, occurred for 62.6910% of the 6770 timesteps. 

Solar Orbiter Level 2 Magnetometer Data in Spacecraft Reference Frame in Normal Mode

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/srf-normal/2020/solo_l2_mag-srf-normal_20200415_v02.cdf. The most common cadence, 125004351 [ns] = PT0.125004S, occurred for 48.7509% of the 336954 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/vso-burst/2020/solo_l2_mag-vso-burst_20201226_v02.cdf. The most common cadence, 15630573 [ns] = PT0.015631S, occurred for 43.0053% of the 2377972 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/vso-normal/2020/solo_l2_mag-vso-normal_20201226_v02.cdf. The most common cadence, 125004351 [ns] = PT0.125004S, occurred for 48.7530% of the 336980 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/science/l2/vso-normal-1-minute/2020/solo_l2_mag-vso-normal-1-minute_20201226_v02.cdf. The most common cadence, 59999996424 [ns] = PT59.999996S, occurred for 46.6991% of the 672 timesteps. 

This file contains RPW HFR level 2 science survey data for the current day.

The authors must acknowledge the Solar Orbiter/RPW Investigation (M. Maksimovic, PIs) for access to data.

Data provided are publicly available. If used in presentations or publications, please acknowledge Solar Orbiter/RPW Investigation (M. Maksimovic, PIs). Please read carefully the caveats attached to the data. For reporting purposes, we request bibliography information for any publication, etc., using these data. Please send information on the use of this data to: M. Maksimovic (PI).

SPDF/CDAWeb. Please also acknowledge the data producer: M.Maksimovic at LESIA, Observatoire de Paris-CNRS

SPDF/SSCWeb. Please also acknowledge the data producer: M.Maksimovic at LESIA, Observatoire de Paris-CNRS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M.Maksimovic at LESIA, Observatoire de Paris-CNRS

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/hfr-surv/2020/solo_l2_rpw-hfr-surv_20200615_v06.cdf. The most common cadence, 10999936 [ns] = PT0.011S, occurred for 25.5209% of the 78302 timesteps. 

RPW High Frequency Receiver in survey mode (from all.xml/instrument/description/@short)

HFR sweep index number. Note: CDF_UINT4 data was converted to HAPI double.

Solar Orbiter Radio and Plasma Wave, Level 2 Low Frequency Receiver (LFR) Averaged Spectral Matrix (ASM) Data in Survey Mode

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_F0, @1 => Epoch_F1, @2 => Epoch_F2, @3 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_F0, @1 => Epoch_F1, @2 => Epoch_F2, @3 => Epoch.)

RPW Low Frequency Receiver Average Spectral Matrices data in survey mode (from all.xml/instrument/description/@short)

[NO PLOT/LIST] All the real part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in the SCM B1-B2-B3 axis system frame (ASF).

Counts based on variable 'Epoch_F0' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-asm/2020/solo_l2_rpw-lfr-surv-asm_20200615_v05.cdf. The most common cadence, 3999960960 [ns] = PT3.999961S, occurred for 22.5000% of the 18 timesteps. 

[NO PLOT/LIST] All the imaginary part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in the SCM B1-B2-B3 axis system frame (ASF).

[NO PLOT/LIST] All the real part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in spacecraft reference frame (SRF).

[NO PLOT/LIST] All the imaginary part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in spacecraft reference frame (SRF).

[NO PLOT/LIST] All the real part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in the SCM B1-B2-B3 axis system frame (ASF).

Counts based on variable 'Epoch_F1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-asm/2020/solo_l2_rpw-lfr-surv-asm_20200615_v05.cdf. The most common cadence, 3999960960 [ns] = PT3.999961S, occurred for 22.5000% of the 18 timesteps. 

[NO PLOT/LIST] All the imaginary part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in the SCM B1-B2-B3 axis system frame (ASF).

[NO PLOT/LIST] All the real part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in spacecraft reference frame (SRF).

[NO PLOT/LIST] All the imaginary part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in spacecraft reference frame (SRF).

[NO PLOT/LIST] All the real part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in the SCM B1-B2-B3 axis system frame (ASF).

Counts based on variable 'Epoch_F2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-asm/2020/solo_l2_rpw-lfr-surv-asm_20200615_v05.cdf. The most common cadence, 3999960960 [ns] = PT3.999961S, occurred for 15.0000% of the 12 timesteps. 

[NO PLOT/LIST] All the imaginary part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in the SCM B1-B2-B3 axis system frame (ASF).

[NO PLOT/LIST] All the real part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in spacecraft reference frame (SRF).

[NO PLOT/LIST] All the imaginary part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in spacecraft reference frame (SRF).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-asm/2020/solo_l2_rpw-lfr-surv-asm_20200615_v05.cdf. The most common cadence, 3996237824 [ns] = PT3.996238S, occurred for 8.2645% of the 20 timesteps. 

Solar Orbiter Radio and Plasma Wave (RPW), Level 2 Low Frequency Receiver (LFR) Basic Parameter Set 1 (BP1) Data in Survey Mode

This file contains RPW LFR level 2R Survey BP1 data of the current test.

The authors are pleased to acknowledge the Solar Orbiter/RPW Investigation (M. Maksimovic, PIs) for access to data.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_N_F0, @1 => Epoch_N_F1, @2 => Epoch_N_F2, @3 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_N_F0, @1 => Epoch_N_F1, @2 => Epoch_N_F2, @3 => Epoch.)

RPW Low Frequency Receiver Basic parameters set 1 data in Survey mode (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch_N_F0' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp1/2020/solo_l2_rpw-lfr-surv-bp1_20200615_v07.cdf. The most common cadence, 3999961000 [ns] = PT3.999961S, occurred for 37.8177% of the 8155 timesteps. 

Wave normal vector from magnetic field in normal mode at F0 in the SCM B1-B2-B3 axis system frame.

Wave normal vector from magnetic field in normal mode at F0 in spacecraft reference frame (SRF).

Real part of the X component of the Poynting vector in normal mode at F0

Argument bit = 0 if |ARG(SX)| < pi/4 or 3pi/4 < |ARG(SX)| < pi, bit arg = 1 elsewhere in normal mode at F0

Phase velocity estimated from the X projection of Maxwell-Faraday equation in normal mode at F0

Argument bit = 0 if |ARG(VPHI)| < pi/4 or 3pi/4 < |ARG(VPHI)| < pi, bit arg = 1 elsewhere in normal mode at F0

Counts based on variable 'Epoch_N_F1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp1/2020/solo_l2_rpw-lfr-surv-bp1_20200615_v07.cdf. The most common cadence, 3999961000 [ns] = PT3.999961S, occurred for 37.5162% of the 8090 timesteps. 

Wave normal vector from magnetic field in normal mode at F1 in the SCM B1-B2-B3 axis system frame.

Wave normal vector from magnetic field in normal mode at F1 in spacecraft reference frame (SRF).

Real part of the X component of the Poynting vector in normal mode at F1

Argument bit = 0 if |ARG(SX)| < pi/4 or 3pi/4 < |ARG(SX)| < pi, bit arg = 1 elsewhere in normal mode at F1

Counts based on variable 'Epoch_N_F2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp1/2020/solo_l2_rpw-lfr-surv-bp1_20200615_v07.cdf. The most common cadence, 3999961000 [ns] = PT3.999961S, occurred for 37.4281% of the 8071 timesteps. 

Wave normal vector from magnetic field in normal mode at F2 in the SCM B1-B2-B3 axis system frame.

Wave normal vector from magnetic field in normal mode at F2 in spacecraft reference frame (SRF).

Real part of the X component of the Poynting vector in normal mode at F2

Argument bit = 0 if |ARG(SX)| < pi/4 or 3pi/4 < |ARG(SX)| < pi, bit arg = 1 elsewhere in normal mode at F2

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp1/2020/solo_l2_rpw-lfr-surv-bp1_20200615_v07.cdf. The most common cadence, 2029440 [ns] = PT0.002029S, occurred for 8.6870% of the 5620 timesteps. 

Solar Orbiter Radio and Plasma Wave, Level 2 Low Frequency Receiver (LFR) Basic Parameter Set 2 (BP2) Data in Survey Mode

This file contains RPW LFR level 2R Survey BP2 data of the current test.

RPW Low Frequency Receiver Basic parameters set 2 data in Survey mode (from all.xml/instrument/description/@short)

All the real part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in normal mode in the SCM B1-B2-B3 axis system frame [no plot]

Counts based on variable 'Epoch_N_F0' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp2/2020/solo_l2_rpw-lfr-surv-bp2_20200615_v06.cdf. The most common cadence, 19999820000 [ns] = PT19.99982S, occurred for 23.0394% of the 993 timesteps. 

All the imaginary part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in normal mode in the SCM B1-B2-B3 axis system frame [no plot]

All the real part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in normal mode in spacecraft reference frame (SRF) [no plot]

All the imaginary part of the 5x5 calibrated matrices for all bins of F0 sampling frequency in normal mode in SRF [no plot]

All the real part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in normal mode in the SCM B1-B2-B3 axis system frame [no plot]

Counts based on variable 'Epoch_N_F1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp2/2020/solo_l2_rpw-lfr-surv-bp2_20200615_v06.cdf. The most common cadence, 19999820000 [ns] = PT19.99982S, occurred for 23.1555% of the 998 timesteps. 

All the imaginary part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in normal mode in the SCM B1-B2-B3 axis system frame [no plot]

All the real part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in normal mode in SRF [no plot]

All the imaginary part of the 5x5 calibrated matrices for all bins of F1 sampling frequency in normal mode in SRF [no plot]

All the real part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in the normal mode in SCM B1-B2-B3 axis system frame [no plot]

Counts based on variable 'Epoch_N_F2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp2/2020/solo_l2_rpw-lfr-surv-bp2_20200615_v06.cdf. The most common cadence, 19999820000 [ns] = PT19.99982S, occurred for 23.3411% of the 1006 timesteps. 

All the imaginary part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in normal mode in the SCM B1-B2-B3 axis system frame [no plot]

All the real part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in normal mode in SRF [no plot]

All the imaginary part of the 5x5 calibrated matrices for all bins of F2 sampling frequency in normal mode in SRF [no plot]

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-bp2/2020/solo_l2_rpw-lfr-surv-bp2_20200615_v06.cdf. The most common cadence, 2029440 [ns] = PT0.002029S, occurred for 8.9004% of the 1151 timesteps. 

Solar Orbiter Radio and Plasma Waves, Level 2 Low Frequency Receiver (LFR) Continuous Magnetic Waveform (CWF-B) in Survey Mode

This file contains RPW LFR level 2 continous waveform of magnetic data in survey mode

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-cwf-b/2020/solo_l2_rpw-lfr-surv-cwf-b_20200615_v07.cdf. The most common cadence, 62499968 [ns] = PT0.0625S, occurred for 74.7027% of the 1026092 timesteps. 

Low Frequency Receiver (from all.xml/instrument/description/@short)

Solar Orbiter Radio and Plasma Waves, Level 2 Low Frequency Reciver (LFR) Continuous Electric Waveform (CWF-E) in Survey Mode

This file contains RPW LFR level 2 continuous waveform of electric data in survey mode.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/lfr-surv-cwf-e/2020/solo_l2_rpw-lfr-surv-cwf-e_20200615_v07.cdf. The most common cadence, 62499968 [ns] = PT0.0625S, occurred for 74.7027% of the 1026092 timesteps. 

RPW Low Frequency Receiver Continuous Waveform in survey mode. Electric component. (from all.xml/instrument/description/@short)

This file contains RPW TDS level 2 regular snapshot Histogram 1D data.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/tds-surv-hist1d/2020/solo_l2_rpw-tds-surv-hist1d_20200615_v05.cdf. The most common cadence, 978776704 [ns] = PT0.978777S, occurred for 0.1789% of the 1 timesteps. 

RPW Time Domain Sampler 1D Histogram data in survey mode (from all.xml/instrument/description/@short)

This file contains RPW TDS level 2 regular snapshot Histogram 2D data.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/tds-surv-hist2d/2020/solo_l2_rpw-tds-surv-hist2d_20200615_v05.cdf. The most common cadence, 1800003046912 [ns] = PT30M0.003047S, occurred for 57.7778% of the 26 timesteps. 

RPW Time Domain Sampler 2D Histogram data in survey mode (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l2/tds-surv-stat/2020/solo_l2_rpw-tds-surv-stat_20200615_v05.cdf. The most common cadence, 16000027008 [ns] = PT16.000027S, occurred for 47.2434% of the 2545 timesteps. 

RPW Time Domain Sampler the basic statistical parameters in survey mode (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Differential Energy Flux (DEF) of Pitch Angle Data (PAD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS)

Current best quality data - see caveats file or contact SWA/EAS team for information on use

SPDF/CDAWeb. Please also acknowledge the data producer: C. J. Owen at MSSL-UCL, University College London, UK

SPDF/SSCWeb. Please also acknowledge the data producer: C. J. Owen at MSSL-UCL, University College London, UK

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C. J. Owen at MSSL-UCL, University College London, UK

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas-pad-def/2020/solo_l2_swa-eas-pad-def_20200616t090001-20200616t100000_v01.cdf. The most common cadence, 125000000 [ns] = PT0.125S, occurred for 82.7360% of the 7941 timesteps. 

Level 2 2D Burst Mode Data (from Master/CDFglobalAttributes/Data_type)

Epoch in nano-seconds since J2000, encoded as terrestrial time on rotating Earth Geoid

Electron pitch angle data - Differential Energy Flux [available 06/2020 - 10/2020, varying with energy, azimuth and elevation angles, CDAWeb plots not supported]

Electron pitch angle distribution - Differential Energy Flux [available 04/2021 - ongoing, varying with energy, azimuth and elevation angles, CDAWeb plots not supported]

Solar Orbiter Level 2 Differential Number Flux (DNF) of Pitch Angle Data (PAD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas-pad-dnf/2020/solo_l2_swa-eas-pad-dnf_20200616t090001-20200616t090500_v03.cdf. The most common cadence, 125000000 [ns] = PT0.125S, occurred for all 2399 timesteps. 

Electron pitch angle data - Differential Number Flux [available 06/2020 - 10/2020, varying with energy, azimuth and elevation angles, CDAWeb  plots not supported]

Electron pitch angle data - Differential Number Flux [available 04/2021 - ongoing, varying with energy, azimuth and elevation angles, CDAWeb plots not supported]

Solar Orbiter Level 2 Phase Space Density (PSD) of Pitch Angle Data (PAD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas-pad-psd/2020/solo_l2_swa-eas-pad-psd_20200616t090001-20200616t090500_v03.cdf. The most common cadence, 125000000 [ns] = PT0.125S, occurred for all 2399 timesteps. 

Electron pitch angle data - Phase Space Density [available 06/2020 - 10/2020, varying energy, azimuth and elevation angles, CDAWeb plots not supported]

Electron pitch angle data - Phase Space Density [available 04/2021 - ongoing, varying energy, azimuth and elevation angles, CDAWeb plots not supported]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, Energy Flux

Solar Orbiter is a space mission of international collaboration between ESA and NASA, operated by ESA Solar Orbiter Solar Wind Analyser (SWA) data are derived from scientific sensors which have been designed and created, and are operated under funding provided in numerous contracts from the UK Space Agency (UKSA), the UK Science and Technology Facilities Council (STFC), the Agenzia Spaziale Italiana (ASI), the Centre National d'etudes Spatiales (CNES, France), the Centre National de la Recherche Scientifique (CNRS, France), the Czech contribution to the ESA PRODEX programme and NASA.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-eflux/2020/solo_l2_swa-eas1-eflux_20200616_v01.cdf. The most common cadence, 100000000000 [ns] = PT1M40S, occurred for 56.2222% of the 253 timesteps. 

Solar Wind Analyzer, Elecron Analyzer System 1, Energy Flux (from all.xml/instrument/description/@short)

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, High Resolution  Nominal Mode 3D, Differential Energy Flux

Solar Orbiter is a space mission of international collaboration between ESA and NASA, operated by ESA. Solar Orbiter Solar Wind Analyser (SWA) data are derived from scientific sensors which have been designed and created, and are operated under funding provided in numerous contracts from the UK Space Agency (UKSA), the UK Science and Technology Facilities Council (STFC), the Agenzia Spaziale Italiana (ASI), the Centre National d'etudes Spatiales (CNES, France), the Centre National de la Recherche Scientifique (CNRS, France), the Czech contribution to the ESA PRODEX programme and NASA.

Solar Wind Analyzer, Electron Analyser System 1, High Resolution Nominal Mode 3D, Differential Energy Flux (from all.xml/instrument/description/@short)

EAS1 3D electron distribution - Differential Energy Flux (No Plot)

EAS1 3D electron distribution - Differential Energy Flux [varying with reordered elevation and energy] (No Plot)

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, High Resolution Nominal Mode 3D, Differential Number Flux

Solar Wind Analyzer, Electron Analyser System 1, High Resolution Nominal Mode 3D, Differential Number Flux (from all.xml/instrument/description/@short)

EAS1 3D electron distribution - Differential Number Flux (No Plot)

EAS1 3D electron distribution - Differential Number Flux [varying with reordered elevation and energy] (No Plot)

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, High Resolution Nominal Mode 3D, Phase Space Density

Solar Wind Analyzer, Electron Analyser System 1, High Resolution Nominal Mode 3D, Phase Space Density (from all.xml/instrument/description/@short)

EAS1 3D electron distribution - Phase Space Density [varying with reordered elevation and energy [No Plot]

Solar Orbiter Level 2 Nominal Mode 3D Differential Energy Flux (NM3D-DEF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 1

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-nm3d-def/2021/solo_l2_swa-eas1-nm3d-def_20210808t000008-20210808t060348_v01.cdf. The most common cadence, 9999498112 [ns] = PT9.999498S, occurred for 18.9352% of the 409 timesteps. 

Level 2 Nominal Mode 3D Data (from Master/CDFglobalAttributes/Data_type)

EAS1 3D electron distribution - Differential Energy Flux [varying with energy, azimuth and elevation angles, CDAWeb plots not supported.]

EAS1 3D electron distribution - Differential Energy Flux [varying with energy, azimuth and elevation angles, energy and elevation angle reordered; CDAWeb plots not supported.]

Solar Orbiter Level 2 Nominal Mode 3D Differential Number Flux (NM3D-DNF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 1

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-nm3d-dnf/2022/solo_l2_swa-eas1-nm3d-dnf_20220317t000001-20220317t060501_v01.cdf. The most common cadence, 9999498624 [ns] = PT9.999499S, occurred for 18.8426% of the 407 timesteps. 

EAS1 3D electron distribution - Differential Number Flux [varying with energy, azimuth and elevation angles, CDAWeb plots not supported.]

EAS1 3D electron distribution - Differential Number Flux [varying with energy, azimuth and elevation angles, energy and elevation angle reordered; CDAWeb plots not supported.]

Solar Orbiter Level 2 Nominal Mode 3D Phase Space Density (NM3D-PSD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 1

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-nm3d-psd/2021/solo_l2_swa-eas1-nm3d-psd_20210808t000008-20210808t060348_v01.cdf. The most common cadence, 9999498112 [ns] = PT9.999498S, occurred for 18.9352% of the 409 timesteps. 

EAS1 3D electron distribution - Phase Space Density [varying with energy, azimuth and elevation angles, CDAWeb plots not supported]

EAS1 3D electron distribution - Phase Space Density [varying with energy, azimuth and elevation angles, energy and elevation angle reordered; CDAWeb plots not supported.]

Solar Orbiter Level 2 Single Strahl (SS) Differential Energy Flux (DEF) of Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 1

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-ss-def/2020/solo_l2_swa-eas1-ss-def_20200615t144926-20200615t175246_v03.cdf. The most common cadence, 99999787776 [ns] = PT1M39.999788S, occurred for 6.3636% of the 7 timesteps. 

Level 2 Single Strahl 3D Data (from Master/CDFglobalAttributes/Data_type)

EAS1 single energy strahl data - Differential Energy Flux [varying with azimuth and elevation angles]

Solar Orbiter Level 2 Single Strahl (SS) Differential Number Flux (DNF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 1

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-ss-dnf/2020/solo_l2_swa-eas1-ss-dnf_20200615t144926-20200615t175246_v03.cdf. The most common cadence, 99999787776 [ns] = PT1M39.999788S, occurred for 6.3636% of the 7 timesteps. 

EAS1 single energy strahl data - Differential Number Flux [varying with azimuth and elevation angles]

Solar Orbiter Level 2 Single Strahl (SS) Phase Space Density (PSD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 1

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-ss-psd/2020/solo_l2_swa-eas1-ss-psd_20200615t144926-20200615t175246_v03.cdf. The most common cadence, 99999787776 [ns] = PT1M39.999788S, occurred for 6.3636% of the 7 timesteps. 

EAS1 single energy strahl data - Phase Space Density [varying with azimuth and elevation angles]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, Trigger Mode 3D, Differential Energy Flux

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-tm3d-def/2023/solo_l2_swa-eas1-tm3d-def_20230104t072941-20230104t073439_v01.cdf. The most common cadence, 999955968 [ns] = PT0.999956S, occurred for 29.6296% of the 88 timesteps.

Solar Wind Analyzer, Electron Analyser System 1, Trigger Mode 3D, Differential Energy Flux (from all.xml/instrument/description/@short)

EAS1 3D electron distribution - Differential Energy Flux [varying with reordered elevation and energy (No Plot)]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, Trigger Mode 3D, Differential Number Flux

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-tm3d-dnf/2023/solo_l2_swa-eas1-tm3d-dnf_20230104t072941-20230104t073439_v01.cdf. The most common cadence, 999955968 [ns] = PT0.999956S, occurred for 29.6296% of the 88 timesteps.

Solar Wind Analyzer, Electron Analyser System 1, Trigger Mode 3D, Differential Number Flux (from all.xml/instrument/description/@short)

EAS1 3D electron distribution - Differential Number Flux [varying with reordered elevation and energy (No Plot)]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 1, Trigger Mode 3D, Phase Space Density

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas1-tm3d-psd/2023/solo_l2_swa-eas1-tm3d-psd_20230104t072941-20230104t073439_v01.cdf. The most common cadence, 999955968 [ns] = PT0.999956S, occurred for 29.6296% of the 88 timesteps.

Solar Wind Analyzer, Electron Analyser System 1, Trigger Mode 3D, Phase Space Density (from all.xml/instrument/description/@short)

EAS1 3D electron distribution - Phase Space Density [varying with reordered elevation and energy (No Plot)]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, Energy Flux

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-eflux/2020/solo_l2_swa-eas2-eflux_20200616_v01.cdf. The most common cadence, 100000031872 [ns] = PT1M40.000032S, occurred for 12.0000% of the 54 timesteps. 

Solar Wind Analyzer, Elecron Analyzer System 2, Energy Flux (from all.xml/instrument/description/@short)

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, High Resolution Nominal Mode 3D, Differential Energy Flux

Solar Wind Analyzer, Electron Analyser System 2, High Resolution Nominal Mode 3D, Differential Energy Flux (from all.xml/instrument/description/@short)

EAS2 3D electron distribution - Differential Energy Flux (No Plot)

EAS2 3D electron distribution - Differential Energy Flux [varying with reordered elevation and energy ] (No Plot)

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, High Resolution Nominal mode 3D, Differential Number Flux

Solar Wind Analyzer, Electron Analyser System 2, High Resolution Nominal Mode 3D, Differential Number Flux (from all.xml/instrument/description/@short)

EAS2 3D electron distribution - Differential Number Flux (No Plot)

EAS2 3D electron distribution - Differential Number Flux [varying with reordered elevation and energy] (No Plot)

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, High Resolution Nominal Mode 3D, Phase Space Density

Solar Wind Analyzer, Electron Analyser System 2, High Resolution Nominal Mode 3D, Phase Space Density (from all.xml/instrument/description/@short)

EAS2 3D electron distribution - Phase Space Density [varying with reordered elevation and energy [No Plot]

Solar Orbiter Level 2 Nominal Mode 3D Differential Energy Flux (NM3D-DEF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 2

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-nm3d-def/2020/solo_l2_swa-eas2-nm3d-def_20200615t144838-20200615t175338_v02.cdf. The most common cadence, 99999986176 [ns] = PT1M39.999986S, occurred for 7.2072% of the 8 timesteps. 

EAS2 3D electron distribution - Differential Energy Flux [varying with energy, azimuth and elevation angles, CDAWeb plots not supported.]

EAS2 3D electron distribution - Differential Energy Flux [varying with energy, azimuth and elevation angles, energy and elevation angle reordered; CDAWeb plots not supported.]

Solar Orbiter Level 2 Nominal Mode 3D Differential Number Flux (NM3D-DNF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 2

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-nm3d-dnf/2020/solo_l2_swa-eas2-nm3d-dnf_20200615t144838-20200615t175338_v02.cdf. The most common cadence, 99999986176 [ns] = PT1M39.999986S, occurred for 7.2072% of the 8 timesteps. 

EAS2 3D electron distribution - Differential Number Flux [varying with energy, azimuth and elevation angles, CDAWeb plots not supported.]

EAS2 3D electron distribution - Differential Number Flux [varying with energy, azimuth and elevation angles, energy and elevation angle reordered; CDAWeb plots not supported.]

Solar Orbiter Level 2 Nominal Mode 3D Phase Space Density (NM3D-PSD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 2

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-nm3d-psd/2020/solo_l2_swa-eas2-nm3d-psd_20200615t144838-20200615t175338_v02.cdf. The most common cadence, 99999986176 [ns] = PT1M39.999986S, occurred for 7.2072% of the 8 timesteps. 

EAS2 3D electron distribution - Phase Space Density [varying with energy, azimuth and elevation angles, CDAWeb plots not supported.]

EAS2 3D electron distribution - Phase Space Density [varying with energy, azimuth and elevation angles, energy and elevation angle reordered; CDAWeb plots not supported.]

Solar Orbiter Level 2 Single Strahl (SS) Differential Energy Flux (DEF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 2

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-ss-def/2020/solo_l2_swa-eas2-ss-def_20200615t144926-20200615t175246_v03.cdf. The most common cadence, 99999970944 [ns] = PT1M39.999971S, occurred for 6.3636% of the 7 timesteps. 

EAS2 single energy strahl data - Differential Energy Flux [varying with azimuth and elevation angles]

Solar Orbiter Level 2 Single Strahl (SS) Differential Number Flux (DNF) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 2

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-ss-dnf/2020/solo_l2_swa-eas2-ss-dnf_20200615t144926-20200615t175246_v03.cdf. The most common cadence, 99999970944 [ns] = PT1M39.999971S, occurred for 6.3636% of the 7 timesteps. 

EAS2 single energy strahl data - Differential Number Flux [varying with azimuth and elevation angles]

Solar Orbiter Level 2 Single Strahl (SS) Phase Space Density (PSD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS) Sensor 2

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-ss-psd/2020/solo_l2_swa-eas2-ss-psd_20200615t144926-20200615t175246_v03.cdf. The most common cadence, 99999970944 [ns] = PT1M39.999971S, occurred for 6.3636% of the 7 timesteps. 

EAS2 single energy strahl data - Phase Space Density [varying with azimuth and elevation angles]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, Trigger Mode 3D, Differential Energy Flux

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-tm3d-def/2023/solo_l2_swa-eas2-tm3d-def_20230108t135646-20230108t140145_v01.cdf. The most common cadence, 999955968 [ns] = PT0.999956S, occurred for 39.5973% of the 118 timesteps.

Solar Wind Analyzer, Electron Analyser System 2, Trigger Mode 3D, Differential Energy Flux (from all.xml/instrument/description/@short)

EAS2 3D electron distribution - Differential Energy Flux [varying with reordered elevation and energy (No Plot)]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, Trigger Mode 3D, Differential Number Flux

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-tm3d-dnf/2023/solo_l2_swa-eas2-tm3d-dnf_20230108t135646-20230108t140145_v01.cdf. The most common cadence, 999955968 [ns] = PT0.999956S, occurred for 39.5973% of the 118 timesteps.

Solar Wind Analyzer, Electron Analyser System 2, Trigger Mode 3D, Differential Number Flux (from all.xml/instrument/description/@short)

EAS2 3D electron distribution - Differential Number Flux [varying with reordered elevation and energy (No Plot)]

Solar Orbiter, Level L2, Solar Wind Analyzer, Electron Analyser System 2, Trigger Mode 3D, Phase Space Density

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/eas2-tm3d-psd/2023/solo_l2_swa-eas2-tm3d-psd_20230108t135646-20230108t140145_v01.cdf. The most common cadence, 999955968 [ns] = PT0.999956S, occurred for 39.5973% of the 118 timesteps.

Solar Wind Analyzer, Electron Analyser System 2, Trigger Mode 3D, Phase Space Density (from all.xml/instrument/description/@short)

EAS2 3D electron distribution - Phase Space Density [varying with reordered elevation and energy (No Plot)]

Solar Orbiter Level 2 Solar Wind Analyser Heavy Ion Sensor Housekeeping Parameters

HK data for HIS instrument.For details see Telemetry Definitions Document, 15164-TELDEF-01.Usage notes can be found via the SWA DOI at https://doi.org/10.5270/esa-ahypgn6.

Please acknowledge Chris J. Owen (SWA PI -- UCL MSSL) & Stefano Livi (HIS PI -- SwRI). NASA Contract NNG10EK25C.

These Level 2 data require substantial processing for most applications.  Users are encouraged to use Level 3 data, which provide the most relevant data products for scientific research.  See Data Product Description Document for more information.  Contact SWA/HIS team for more information as needed.

SPDF/CDAWeb. Please also acknowledge the data producer: S. Livi at SWRI

SPDF/SSCWeb. Please also acknowledge the data producer: S. Livi at SWRI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: S. Livi at SWRI

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/his-hk/2022/solo_l2_swa-his-hk_20220101_v02.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for 71.6470% of the 1031 timesteps.

Solar Wind Analyzer, Heavy Ion Sensor, Houskeeping (from all.xml/instrument/description/@short)

Status on whether the CDH watchdog timed out (and caused a reset)

Subservice of last accepted instrument command (not from macros)

Source sequence count of last accepted instrument command (not from macros)

Subservice of last rejected instrument command (not from macros)

Source sequence count of last rejected instrument command (not from macros)

Status on whether the CPU watchdog timed out (and caused a reset)

Current step table pointer from the sweep table - E/Q index (scan or data selectable)

Currently selected row of scan control table (scan or data selectable)

Number of seconds over which the data in this product was collected

Whether analyzer supply is sweeping or static while in sweeping mode

Whether bottom deflector supply is sweeping or static while in sweeping mode

Whether top deflector supply is sweeping or static while in sweeping mode

Whether top plate supply is sweeping or static while in sweeping mode

Specifies whether reported sweep table pointers are for scan or data

Solar Orbiter Level 2 Solar Wind Analyser Heavy Ion Sensor Pulse Height Analyzed

Pulse Height Analysis data for HIS instrument in physical units. Some corrections for instrument characteristics and measurement techniques have been applied. Per Data Product Description Document, efficiency corrections have not been applied.Ion Event (PHA) words. Individual ion event data, containing full information on incident angles (elevation and azimuth), E/q, TOF and SSD energy in digital and physical units. The resolution of this data product can be 30s or 300s. In Burst mode the resolution can be 4s but this can only be run on average 1% of the time due to telemetry constraints.Usage notes can be found via the SWA DOI at https://doi.org/10.5270/esa-ahypgn6.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/his-pha/2022/solo_l2_swa-his-pha_20220101_v02.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for 0.0123% of the 2126 timesteps.

Solar Wind Analyzer, Heavy Ion Sensor, Pulse Height Analyzed (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Solar Wind Analyser Heavy Ion Sensor Rates

Rate data for HIS instrument in physical units. Some corrections for instrument characteristics and measurement techniques have been applied. Per Data Product Description Document, efficiency corrections have not been applied.Counts of unclassified ion event words on the HIS detectors (start MCP, stop MCP, SSD) as a function of E/q, integrated over incident angles, TOF and Energy. Includes full counts of events subject to decimation. Rates also include two coincidence rates, the number of events with a valid TOF and energy (triple coincidence), and a count of those with only a valid TOF (double coincidence). These rates are primarily used to evaluate the performance of the instrument, rather than for science.  In particular, they can be used for calculation of ion detection efficiency in-flight [von Steiger et al., 2000].  The resolution of this data product can be 30s or 300s. In Burst mode the resolution can be 4s but this can only be run on average 1% of the time due to telemetry constraints.Usage notes can be found via the SWA DOI at https://doi.org/10.5270/esa-ahypgn6.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/his-rates/2022/solo_l2_swa-his-rates_20220101_v02.cdf. The most common cadence, 30000000000 [ns] = PT30S, occurred for 70.6822% of the 2124 timesteps. 

Solar Wind Analyzer, Heavy Ion Sensor, Rates (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Energy Flux from Solar Wind Analyser (SWA) Proton-Alpha Sensor (PAS)

SPDF/CDAWeb. Please also acknowledge the data producer: C.J. Owen at MSSL-UCL, University College London, UK

SPDF/SSCWeb. Please also acknowledge the data producer: C.J. Owen at MSSL-UCL, University College London, UK

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C.J. Owen at MSSL-UCL, University College London, UK

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/pas-eflux/2020/solo_l2_swa-pas-eflux_20200707_v02.cdf. The most common cadence, 4000007000 [ns] = PT4.000007S, occurred for 48.9452% of the 4849 timesteps. 

Solar Wind Analyser / Proton-Alpha Sensor (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Ground Calculated Moments Data from Solar Wind Analyser (SWA) Proton-Alpha Sensor (PAS) 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/pas-grnd-mom/2020/solo_l2_swa-pas-grnd-mom_20200707_v03.cdf. The most common cadence, 4000007000 [ns] = PT4.000007S, occurred for 48.9452% of the 4849 timesteps. 

Solar Orbiter Level 2 Phase Spase Distribution Function from Solar Wind Analyser (SWA) Proton-Alpha Sensor (PAS)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l2/pas-vdf/2020/solo_l2_swa-pas-vdf_20200707_v02.cdf. The most common cadence, 4000007000 [ns] = PT4.000007S, occurred for 48.9452% of the 4849 timesteps. 

Solar Orbiter, Level 3 Data, Energetic Particle Detector, Electron Proton Telescope, 1 day resolution data

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l3/ept-1day/solo_l3_epd-ept-1day_20200101_v02.cdf. The most common cadence, 86400000000000 [ns] = P1D, occurred for all 365 timesteps.

Energetic Particle Detector, Electron Proton Telescope, 1 day resolution data (from all.xml/instrument/description/@short)

Particle flux in foil channel for the sun telescope corrected from ion contamination

Particle flux in foil channel for the anti-sun telescope corrected from ion contamination

Particle flux in foil channel for the north telescope corrected from ion contamination

Particle flux in foil channel for the south telescope corrected from ion contamination

Solar Orbiter, Level 3 Data, Energetic Particle Detector, Electron Proton Telescope, 1 hour

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l3/ept-1hour/2020/solo_l3_epd-ept-1hour_20200601_v02.cdf. The most common cadence, 3600000000000 [ns] = PT1H, occurred for all 719 timesteps.

Energetic Particle Detector, Electron Proton Telescope, 1 hour (from all.xml/instrument/description/@short)

Solar Orbiter, Level 3 Data, Energetic Particle Detector, Electron Proton Telescope, 1 minute

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/science/l3/ept-1min/2020/solo_l3_epd-ept-1min_20200513_v01.cdf. The most common cadence, 60000000000 [ns] = PT1M, occurred for all 1439 timesteps.

Energetic Particle Detector, Electron Proton Telescope, 1 minute (from all.xml/instrument/description/@short)

Particle pitch angle with respect to the average magnetic field for the Sun telescope

Particle pitch angle with respect to the average magnetic field for the Anti-Sun telescope

Particle pitch angle with respect to the average magnetic field for the North telescope

Particle pitch angle with respect to the average magnetic field for the South telescope

Solar Orbiter, Level 3, MAG and RPW, Merged magnetic data sampled at 256 Hz

This file contains waveform of merged magnetic data from MAG magnetometer and RPW-SCM search-coil sensor sampled at 256 Hz

This merged magnetic field data product has been produced by combining data from 1) the Solar Orbiter magnetometer that was provided by Imperial College London and supported by the UK Space Agency, and 2) the RPW-Search Coil Magnetometer that was provided by the LIRA and LPC2E laboratories with the support of CNES and CNRS.

Combined MAG and RPW-SCM Datasets, Solar Orbiter ESA DOI landing page

This data is publicly available. Please cite the relevant papers (MAG paper, RPW paper, SCM paper, and Solar Orbiter merged magnetic field paper) when using these data in publications and presentations, and acknowledge the PI’s of this data product. Read carefully the caveats attached to the data and send information on the use of this data as well as questions and comments to M. Kretzschmar

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/merged/science/l3/mag-rpw-scm-rtn-256/2020/solo_l3_multi-mag-rpw-scm-merged-rtn-256_20200615_v01.cdf. The most common cadence, 3906250 [ns] = PT0.003906S, occurred for 99.9547% of the 28658 timesteps.

Merged magnetic data from MAG magnetometer and RPW-SCM search-coil sensor sampled at 256 Hz (from all.xml/instrument/description/@short)

Magnetic field values (Br, Bt, Bn) in the Radial-Tangential-Normal frame

Solar Orbiter, Level 3, MAG and RPW, Merged magnetic data sampled at 4096 Hz

This file contains waveform of merged magnetic data from MAG magnetometer and RPW-SCM search-coil sensor  sampled at 4096 Hz

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/merged/science/l3/mag-rpw-scm-rtn-4096/2020/solo_l3_multi-mag-rpw-scm-merged-rtn-4096_20200615_v01.cdf. The most common cadence, 244141 [ns] = PT0.000244141S, occurred for 62.4534% of the 17906 timesteps.

Merged magnetic data from MAG magnetometer and RPW-SCM search-coil sensor sampled at 4096 Hz (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/merged/science/l3/mag-rpw-scm-srf-256/2020/solo_l3_multi-mag-rpw-scm-merged-srf-256_20200615_v01.cdf. The most common cadence, 3906250 [ns] = PT0.003906S, occurred for 99.9547% of the 28658 timesteps.

Magnetic field values (Bxsrf, Bysrf, Bzsrf) in the Spacecraft Reference Frame

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/merged/science/l3/mag-rpw-scm-srf-4096/2020/solo_l3_multi-mag-rpw-scm-merged-srf-4096_20200615_v01.cdf. The most common cadence, 244141 [ns] = PT0.000244141S, occurred for 62.4534% of the 17906 timesteps.

Solar Orbiter Radio/Plasma Wave, LFR L3 plasma density derived from the spacecraft potential

This file contains RPW LFR level 3 plasma density derived from the spacecraft potential.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-density/2020/solo_l3_rpw-bia-density_20200615_v02.cdf. The most common cadence, 62499968 [ns] = PT0.0625S, occurred for 74.7027% of the 1026092 timesteps. 

RPW Low Frequency Receiver Plasma density (from all.xml/instrument/description/@short)

Plasma density derived from probe-to-spacecraft potential and electron plasma frequency.

Solar Orbiter Radio/Plasma Wave, LFR L3 plasma density derived from the spacecraft potential, downsampled

This file contains RPW LFR level 3 plasma density derived from the spacecraft potential, downsampled.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-density-10-seconds/2020/solo_l3_rpw-bia-density-10-seconds_20200615_v02.cdf. The most common cadence, 10000000000 [ns] = PT10S, occurred for all 8626 timesteps. 

RPW Low Frequency Receiver Plasma density, downsampled (from all.xml/instrument/description/@short)

Plasma density derived from probe-to-spacecraft potential and electron plasma frequency. Median value over 10 s interval.

This file contains RPW LFR level 3 electric vector field data in SRF.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-efield/2020/solo_l3_rpw-bia-efield_20200615_v04.cdf. The most common cadence, 62499968 [ns] = PT0.0625S, occurred for 74.7027% of the 1026092 timesteps. 

RPW Low Frequency Receiver Electric field vector (from all.xml/instrument/description/@short)

Solar Orbiter Radio/Plasma Wave, LFR L3 electric field vector, downsampled

This file contains RPW LFR level 3 electric vector field data in SRF, downsampled.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-efield-10-seconds/2020/solo_l3_rpw-bia-efield-10-seconds_20200615_v04.cdf. The most common cadence, 10000000000 [ns] = PT10S, occurred for all 8626 timesteps. 

RPW Low Frequency Receiver Electric field vector, downsampled (from all.xml/instrument/description/@short)

Std. deviation of electric field vector in SRF over 10 s interval.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-scpot/2020/solo_l3_rpw-bia-scpot_20200615_v02.cdf. The most common cadence, 62499968 [ns] = PT0.0625S, occurred for 74.7027% of the 1026092 timesteps. 

RPW Low Frequency Receiver Spacecraft potential (from all.xml/instrument/description/@short)

Solar Orbiter Radio/Plasma Wave, LFR L3 spacecraft potential, downsampled

This file contains RPW LFR level 3 spacecraft potential, downsampled.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-scpot-10-seconds/2020/solo_l3_rpw-bia-scpot-10-seconds_20200615_v02.cdf. The most common cadence, 10000000000 [ns] = PT10S, occurred for all 8626 timesteps. 

RPW Low Frequency Receiver Spacecraft potential, downsampled (from all.xml/instrument/description/@short)

Spacecraft potential with respect to plasma. Median value over 10 s interval.

Std. deviation of the s/c potential with respect to plasma over 10 s interval.

Average probe-to-spacecraft potential. Median over 10 s interval.

Std. deviation of the average probe-to-spacecraft potential over 10 s interval.

Solar Orbiter Radio/Plasma Wave, LFR L3 de Hoffmann-Teller solar wind velocity

This file contains RPW LFR level 3 de Hoffmann-Teller solar wind velocity.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/bia-vht/2020/solo_l3_rpw-bia-vht_20200701-20200731_v02.cdf. The most common cadence, 600000000000 [ns] = PT10M, occurred for 75.0000% of the 387 timesteps.

RPW Low Frequency Receiver de Hoffmann-Teller solar wind velocity (from all.xml/instrument/description/@short)

de Hoffmann-Teller (HT) solar wind velocity in the SRF X direction.

Solar Orbiter Radio/Plasma Wave, data from plasma peak tracking L3

This file contains RPW plasma frequency data for the current day.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/science/l3/tnr-fp/2020/solo_l3_rpw-tnr-fp_20200615_v01.cdf. The most common cadence, 11998800000 [ns] = PT11.9988S, occurred for 13.3409% of the 117 timesteps.

Plasma plasma frequency value from the plasma peak position (from all.xml/instrument/description/@short)

Level 3 data processing (from Master/CDFglobalAttributes/Data_type)

Plasma plasma frequency value from the plasma peak position (from all.xml/instrument/@ID)

Solar Orbiter Level 2 Phase Space Density (PSD) of Nominal Mode Pitch Angle Data (NMPAD) from Solar Wind Analyser (SWA) Electron Analyser System (EAS)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l3/eas-nmpad-psd/2020/solo_l3_swa-eas-nmpad-psd_20200801_v01.cdf. The most common cadence, 100000000000 [ns] = PT1M40S, occurred for 54.3124% of the 233 timesteps. 

Level 3 electron pitch angles from 3d data (from Master/CDFglobalAttributes/Data_type)

Electron pitch angle data, both EAS1 and EAS2 combined - Phase Space Density

Solar Orbiter, Level 3 Data, Solar Wind Analyser, Heavy Ion Sensor Composition 10 Minute Resolution

Level 3 data for HIS instrumentTime series measurements of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind.Usage notes can be found via the SWA DOI at https://doi.org/10.5270/esa-ahypgn6.

This data is appropriate for general scientific use.  Users are encouraged to read the Data Product Description Document and pay attention to the quality flag.  Contact the SWA/HIS team for more information and questions about the data.

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/science/l3/his-comp-10min/2022/solo_l3_swa-his-comp-10min_20220119_v01.cdf. The most common cadence, 599995000000 [ns] = PT9M59.995S, occurred for 81.1189% of the 116 timesteps. 

Solar Wind Analyzer, Heavy Ion Sensor, Composition 10 Minute Resolution (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Low Latency Data from Energetic Particle Detector (EPD), Electron Proton Telescope (EPT), Anti-Sunward Direction Particle Rates

Energetic Particle Detector, Electron Proton Telescope, Anti-Sun direction, Particle Rates (from all.xml/instrument/description/@short)

Level 2 Low Latency Data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/asun-rates/2020/solo_ll02_epd-ept-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 51.8738% of the 263 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/asun-rates/2020/solo_ll02_epd-ept-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6667% of the 2030 timesteps. 

Solar Orbiter Level 2 Low Latency Data from Energetic Particle Detector (EPD) Electron Proton Telescope (EPT), North Direction Particle Rates

Energetic Particle Detector, Electron Proton Telescope, North direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/north-rates/2020/solo_ll02_epd-ept-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 52.1825% of the 263 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/north-rates/2020/solo_ll02_epd-ept-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6446% of the 2016 timesteps. 

Solar Orbiter Level 2 Low Latency Data from Energetic Particle Detector (EPD) Electron Proton Telescope (EPT), South Direction Particle Rates

Energetic Particle Detector, Electron Proton Telescope, South direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/south-rates/2020/solo_ll02_epd-ept-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 52.1825% of the 263 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/south-rates/2020/solo_ll02_epd-ept-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6446% of the 2016 timesteps. 

Solar Orbiter Level 2 Low Latency Data from Energetic Particle Detector (EPD) Electron Proton Telescope (EPT) Sunward Direction Particle Rates

Energetic Particle Detector, Electron Proton Telescope, Sun direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/sun-rates/2020/solo_ll02_epd-ept-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 51.8738% of the 263 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/ept/sun-rates/2020/solo_ll02_epd-ept-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6667% of the 2030 timesteps. 

Solar Orbiter Level 2 Low Latency Data of Energetic Particle Detector (EPD) High Energy Telescope (HET) Anti-Sunward Direction Particle Rates

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => EPOCH, @1 => EPOCH_2, @2 => EPOCH_3, @3 => EPOCH_4, @4 => EPOCH_1.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => EPOCH, @1 => EPOCH_2, @2 => EPOCH_3, @3 => EPOCH_4, @4 => EPOCH_1.)

Energetic Particle Detector, High Energy Telescope, Anti-Sun direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/asun-rates/2020/solo_ll02_epd-het-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 51.8738% of the 263 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/asun-rates/2020/solo_ll02_epd-het-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 300000498944 [ns] = PT5M0.000499S, occurred for 44.0000% of the 22 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/asun-rates/2020/solo_ll02_epd-het-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 600000997632 [ns] = PT10M0.000998S, occurred for 62.5000% of the 15 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/asun-rates/2020/solo_ll02_epd-het-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 3600005986048 [ns] = PT1H0.005986S, occurred for 66.6667% of the 2 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/asun-rates/2020/solo_ll02_epd-het-asun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6667% of the 2030 timesteps. 

Hydrogen high-resolution (HR) number flux in 13.5 - 105 MeV range with 5 s cadence

Solar Orbiter Level 2 Low Latency Data of Energetic Particle Detector (EPD) High Energy Telescope (HET) North Direction Particle Rates

Energetic Particle Detector, High Energy Telescope, North direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/north-rates/2020/solo_ll02_epd-het-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 52.1825% of the 263 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/north-rates/2020/solo_ll02_epd-het-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 300000498944 [ns] = PT5M0.000499S, occurred for 44.0000% of the 22 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/north-rates/2020/solo_ll02_epd-het-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 600000997632 [ns] = PT10M0.000998S, occurred for 62.5000% of the 15 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/north-rates/2020/solo_ll02_epd-het-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 3600005986048 [ns] = PT1H0.005986S, occurred for 66.6667% of the 2 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/north-rates/2020/solo_ll02_epd-het-north-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6446% of the 2016 timesteps. 

Solar Orbiter Level 2 Low Latency Data of Energetic Particle Detector (EPD) High Energy Telescope (HET) South Direction Particle Rates

Energetic Particle Detector, High Energy Telescope, South direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/south-rates/2020/solo_ll02_epd-het-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 52.1825% of the 263 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/south-rates/2020/solo_ll02_epd-het-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 300000498944 [ns] = PT5M0.000499S, occurred for 44.0000% of the 22 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/south-rates/2020/solo_ll02_epd-het-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 600000997632 [ns] = PT10M0.000998S, occurred for 62.5000% of the 15 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/south-rates/2020/solo_ll02_epd-het-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 3600005986048 [ns] = PT1H0.005986S, occurred for 66.6667% of the 2 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/south-rates/2020/solo_ll02_epd-het-south-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6446% of the 2016 timesteps. 

Solar Orbiter Level 2 Low Latency Data of Energetic Particle Detector (EPD) High Energy Telescope (HET) Sunward Direction Particle Rates

Energetic Particle Detector, High Energy Telescope, Sun direction, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/sun-rates/2020/solo_ll02_epd-het-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 30000049920 [ns] = PT30.00005S, occurred for 51.8738% of the 263 timesteps. 

Counts based on variable 'EPOCH_2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/sun-rates/2020/solo_ll02_epd-het-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 300000498944 [ns] = PT5M0.000499S, occurred for 44.0000% of the 22 timesteps. 

Counts based on variable 'EPOCH_3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/sun-rates/2020/solo_ll02_epd-het-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 600000997632 [ns] = PT10M0.000998S, occurred for 62.5000% of the 15 timesteps. 

Counts based on variable 'EPOCH_4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/sun-rates/2020/solo_ll02_epd-het-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 3600005986048 [ns] = PT1H0.005986S, occurred for 66.6667% of the 2 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/het/sun-rates/2020/solo_ll02_epd-het-sun-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 5000008320 [ns] = PT5.000008S, occurred for 66.6667% of the 2030 timesteps. 

Solar Orbiter Level 2 Low Latency data of Energetic Particle Detector (EPD) Suprathermal Ion Spectrograph (SIS) A Telescope, Particle Rates

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/sis/a-rates/2020/solo_ll02_epd-sis-a-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 1800002993024 [ns] = PT30M0.002993S, occurred for 57.1429% of the 4 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, A Telescope, Particle Rates (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Low Latency Data of Energetic Particle Detector (EPD) Suprathermal Ion Spectrograph (SIS) B Telescope Particle Rates

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/sis/b-rates/2020/solo_ll02_epd-sis-b-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 1800002993024 [ns] = PT30M0.002993S, occurred for 57.1429% of the 4 timesteps. 

Energetic Particle Detector, Suprathermal Ion Spectrograph, B Telescope, Particle Rates (from all.xml/instrument/description/@short)

Solar Orbiter Level 2 Low Latency Data from Energetic Particle Detector (EPD) SupraThermal Electrons and Protons (STEP) Particle Rates

Energetic Particle Detector, SupraThermal Electrons and Protons, Particle Rates (from all.xml/instrument/description/@short)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/step/rates/2020/solo_ll02_epd-step-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 60000099712 [ns] = PT1M0.0001S, occurred for 48.9796% of the 120 timesteps. 

Integral high resolution (HR) number flux in 2 - 60 keV range with 1 s cadence

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/epd/low_latency/ll02/step/rates/2020/solo_ll02_epd-step-rates_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 1000001664 [ns] = PT1.000002S, occurred for 91.7834% of the 13494 timesteps. 

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/mag/low_latency/ll02/2020/solo_ll02_mag_20200603t000016-20200604t000015_v01i.cdf. The most common cadence, 8000013312 [ns] = PT8.000013S, occurred for 55.6824% of the 1024 timesteps. 

Magnetic field vector in spacecraft reference frame, 8 second resolution

Solar Orbiter Level 2 Low Latency Data from Radio and Plasma Wave (RPW) Selected Burst Mode 1 (SBM1) (for Shock Crossing)

This file contains RPW Low latency SBM1 data produced by the RPW Low Latency data Pipeline.

SPDF/CDAWeb. Please also acknowledge the data producer: M. Maksimovic at LESIA, Observatoire de Paris-CNRS

SPDF/SSCWeb. Please also acknowledge the data producer: M. Maksimovic at LESIA, Observatoire de Paris-CNRS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M. Maksimovic at LESIA, Observatoire de Paris-CNRS

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/low_latency/ll02/sbm1/2020/solo_ll02_rpw-sbm1_20201005t090001-20201005t205317_v01u.cdf. The most common cadence, 42796162742144 [ns] = PT11H53M16.162742S, occurred for all 1 timesteps. 

Radio and Plasma Waves instrument - SBM1 event data (from all.xml/instrument/description/@short)

SBM1 event absolute time. Note: CDF_UINT4 data was converted to HAPI double.

Solar Orbiter Level 2 Low Latency Data from Radio and Plasma Wave (RPW) Selected Burst Mode 2 (SBM2) (for In Situ Type III)

This file contains RPW Low latency SBM2 data produced by the RPW Low Latency data Pipeline.

Data provided are private. The data users shall contact the Solar Orbiter/RPW team before any use in presentations or publications.

Radio and Plasma Waves instrument - SBM2 event data (from all.xml/instrument/description/@short)

SBM2 event absolute time. Note: CDF_UINT4 data was converted to HAPI double.

Solar Orbiter Level 2 Low Latency Data from Radio and Plasma Wave (RPW) Thermal Noise Receiver (TNR)

This file contains RPW Low latency TNR spectral power data, produced by the RPW Low Latency Data Pipeline (LLDP).

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/rpw/low_latency/ll02/tnr/2020/solo_ll02_rpw-tnr_20200603t144539-20200603t181807_v01u.cdf. The most common cadence, 4000006656 [ns] = PT4.000007S, occurred for 49.8428% of the 1744 timesteps. 

Radio and Plasma Waves instrument - Thermal Noise Receiver (from all.xml/instrument/description/@short)

Median value of the 5 top frequency channels of the TNR D band auto-correlations

Solar Orbiter Level 2 Low Latency Single Strahl (SS) Data from Solar Wind Analyzer (SWA) Electron Analyzer System (EAS)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/low_latency/ll02/eas-ss/2021/solo_ll02_swa-eas-ss_20210412t101149-20210412t162329_v01i.cdf. The most common cadence, 100000870272 [ns] = PT1M40.00087S, occurred for 12.5000% of the 3 timesteps. 

Counts based on variable 'EPOCH_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/low_latency/ll02/eas-ss/2021/solo_ll02_swa-eas-ss_20210412t101149-20210412t162329_v01i.cdf. The most common cadence, 99999817344 [ns] = PT1M39.999817S, occurred for 12.5000% of the 3 timesteps. 

Solar Orbiter Level 2 Low Latency Ratios and Spectra Data from Solar Wind Analyser (SWA) Heavy Ion Sensor (HIS)

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/low_latency/ll02/his-rat/2021/solo_ll02_swa-his-rat_20210401t015701-20210401t215700_v01i.cdf. The most common cadence, 300000502912 [ns] = PT5M0.000503S, occurred for 43.5146% of the 104 timesteps. 

Solar Orbiter Level 2 Low Latency Data from Solar Wind Analyser (SWA) Proton and Alpha Sensor (PAS) Quick Look Moments

Counts based on variable 'EPOCH' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/solar-orbiter/swa/low_latency/ll02/pas-mom/2020/solo_ll02_swa-pas-mom_20200819t160347-20200820t064915_v01c.cdf. The most common cadence, 4000006272 [ns] = PT4.000006S, occurred for 48.6133% of the 6100 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/orbit/def_at/1995/so_at_def_19950522_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 99.1150% of the 112 timesteps. 

SOHO Charge, Element and Isotope Analysis System, Key Parameters

A description of the CELIAS instrument and scientific scope can be found on WWW at http://ubeclu.unibe.ch/phim/ms/soho/ or on the SOHO homepage http://sohowww.nascom.nasa.gov/

SPDF/CDAWeb. Please also acknowledge the data producer: Peter Bochsler at Physikalisches Institut,

SPDF/SSCWeb. Please also acknowledge the data producer: Peter Bochsler at Physikalisches Institut,

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Peter Bochsler at Physikalisches Institut,

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/celias/k0/1995/so_k0_cel_19951222_v01.cdf. The most common cadence, 301000 [ms] = PT5M1S, occurred for 31.5789% of the 90 timesteps. 

Charge, Element and Isotope Analysis System (from all.xml/instrument/description/@short)

Data: 5 minute averages Time tag = center of interval References                    1.Kunow, H., et al., COSTEP -   Comprehensive Suprathermal and  Energetic Particle Analyser for SOHO, in V. Domingo, editor, The SOHO Mission - Scientific and  Technical Aspects of the        Instruments, ESA SP-1104, pages 75 - 80, 1988 2.Kunow, H., et al., COSTEP -  Comprehensive Suprathermal and  Energetic Particle Analyser for SOHO - Scientific Goals and Data Description, Proc. First SOHO  Workshop, ESA SP-348,           pages 43 - 46, 1992 2.Mueller-Mellin, R., et al.,  COSTEP -                        Comprehensive Suprathermal and  Energetic Particle Analyser,    to be published in              Solar Physics, 1995 19 Dec 1996 Caveat: 1. The EPHIN E-detector developed gradually a noise problem during 1996 and was switched off logically on 1996-305-14.40. Check EPHIN status word >Ephin_Stat< bit 2 (2^2): if set to one: E detector  is on, if set to zero, E detector is off. When off, the channels E3000, P41 and H41 show zero intensity, the energy of the next lower channel E1300 is the average of E1300 and E3000, the width of channel E1300 is the sum of the  width E1300 and E3000; P25, and H25 are changed accordingly.  Note: the KPGS calulates correctly the new fluxes in channels E1300, P25, H25. Only their interpretation needs to be changed by the user. 2. The geometric factor for the counting rate channels can be changed either by ground command or autonomously by detecting high fluxes in the center segment of detector A. Check EPHIN status word >Ephin_Stat<bits 9,10,11,12,13,17,18,19,20,21: if set to one: large geometric factor, if set to zero: small geometric factor. Note: the KPGS software calculates correctly the fluxes. No action needed by the user.

SPDF/CDAWeb. Please also acknowledge the data producer: Horst Kunow at University of Kiel, Germany

SPDF/SSCWeb. Please also acknowledge the data producer: Horst Kunow at University of Kiel, Germany

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Horst Kunow at University of Kiel, Germany

Comprehensive Suprathermal and Energetic Particle Analyzer (from all.xml/instrument/description/@short)

SOHO Energetic and Relativistic Nuclei and Electron experiment, Key Parameters

Data: 1 minute averages Time tag = center of intervalTorsti et al.: ERNE - Energetic and Relativistic Nuclei and Electron experiment, The SOHO Mission ESA SP-1104, 1988Torsti et al.: Energetic Particle Experiment ERNE published in SolarPhysics, 162, 505-531, 1995M. Lumme and Eino Valtonen: CEPAC Experiment Operations Manual, November 1994 ERNE WWW Home page  https://srl.utu.fi/projects/erne/

SPDF/CDAWeb. Please also acknowledge the data producer: J Torsti at University of Turku

SPDF/SSCWeb. Please also acknowledge the data producer: J Torsti at University of Turku

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J Torsti at University of Turku

Solar Heliospher Observatory (from all.xml/observatory/description/@short)

Solar Heliospher Observatory (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/orbit/def_or/1997/so_or_def_19970909_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

SOLAR HELIOSPHERIC OBSERVATORY (from all.xml/observatory/description/@short)

SOLAR HELIOSPHERIC OBSERVATORY (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/soho/orbit/pre_or/cdf/1995/so_or_pre_19950522_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

3 component magnetic field from miniature tri-axial magnetometer on ST5/spacecraft 094 (middle position in string-of-pearls constellation)

J. Slavin (UMich) and NASA GSFC for original data, J. Gjerloev (JHUAPL) for baseline corrections, G. Le (NASA GSFC), R. Strangeway (UCLA), R. Redmon (NOAA), Code from A. Richmond,S. de Larquier,N.A. Tsyganeko,R. Barnes used for coordinate transformations, B. Mero (CU Boulder)

SPDF/CDAWeb. Please also acknowledge the data producer: Delores Knipp at University of Colorado, Boulder

SPDF/SSCWeb. Please also acknowledge the data producer: Delores Knipp at University of Colorado, Boulder

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Delores Knipp at University of Colorado, Boulder

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/st5/094/mag/2006/st5-094_1sec_mag_20060326_v0.0.5.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 14495 timesteps. 

Space Technology 5 SC 094 (from all.xml/observatory/description/@short)

Space Technology 5 SC 094 (from Master/CDFglobalAttributes/Source_name)

1 second resolution 3 component fields (from Master/CDFglobalAttributes/Data_type)

---> Geomagnetic Field Perturbation (Solar-Magnetic Coordinates)

---> Spacecraft position in Spherical Geocentric Coordinates (R,Lat,Lon)

Baseline Corrected Geomagnetic Field Perturbation (Solar-Magnetic Coordinates)

---> Baseline Corrected Modified-Apex Geomagnetic Field Perturbation

---> Baseline Corrected Geomagnetic Field Perturbation (Geocentric Coordinates)

Spacecraft position in Altitude Adjusted Corrected Geomagnetic Coordinates (Lat,Lon,Magnetic Local Time)

International Geomagnetic Reference Field Model Output (Solar-Magnetic Coordinates)

3 component magnetic field from miniature tri-axial magnetometer on ST5/spacecraft 155 (leading position in string-of-pearls constellation)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/st5/155/mag/2006/st5-155_1sec_mag_20060325_v0.0.5.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.3225% of the 81361 timesteps. 

Space Technology 5 SC 155 (from all.xml/observatory/description/@short)

Space Technology 5 SC 155 (from Master/CDFglobalAttributes/Source_name)

3 component magnetic field from miniature tri-axial magnetometer on ST5/spacecraft 224 (trailing position in string-of-pearls constellation)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/st5/224/mag/2006/st5-224_1sec_mag_20060326_v0.0.5.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9731% of the 11150 timesteps. 

Space Technology 5 SC 224 (from all.xml/observatory/description/@short)

Space Technology 5 SC 224 (from Master/CDFglobalAttributes/Source_name)

Merged hourly magnetic field, plasma, proton fluxes, and ephermis data

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs).  These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations. About STEREO data in COHOWEB STEREO-A and -B data are from the magnetometer of the IMPACT package and from the PLASTIC plasma detector.  Principal Investigators for these packages are Janet Luhmann (UCB) and Antoinette Galvin (UNH), respectively.  Magnetic field  data were obtained as 10-min averages from the UCLA web site at http://aten.igpp.ucla.edu/forms/stereo/ascii_PLASTIC_10m_new.html, courtesy of C.T. Russell.  Proton Fluxes from http://www.srl.caltech.edu/STEREO/.  COHOWeb's magnetic field hourly averages were created at GSFC/SPDF by averaging over the six 10-min averages falling within each hour.  Hourly plasma parameter data, including plasma flow direction angles for STEREO-A but not yet for STEREO B (as of 7/11/2010), were obtained from UNH via http://fiji.sr.unh.edu/1dmax_ascii/.

Paths to magnetic field, plasma, energetic particle, and ephemeris data relevant to heliospheric studies resident at the Goddard Space Flight Center, GSFC, Space Physics Data Facility, SPDF

General information concerning the STEREO A, In-Situ Measurements of Particles and CME Transients, IMPACT, instrument

General information concerning the STEREO A, Plasma and Supra-Thermal Ion Composition, PLASTIC, instrument

STEREO Plasma and Supra-Thermal Ion Composition, PLASTIC, instrument data web site, hosted by the University of New Hampshire, UNH

SPDF/CDAWeb. Please also acknowledge the data producer: Natasha Papitashvili at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Natasha Papitashvili at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Natasha Papitashvili at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/coho1hr_magplasma/2007/sta_coho1hr_merged_mag_plasma_20070101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Solar Terrestrial Relations Observatory Ahead of the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory Ahead of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

HelioGraphic Inertial (HGI) latitude of the spacecraft position at the start of data interval

HelioGraphic Inertial (HGI) longitude of the spacecraft position at the start of data interval 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/helio1day/sta_helio1day_position_20061027_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 6690 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/helio1hr/sta_helio1hr_position_20061027_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 164423 timesteps. 

The file contains Level 1 IMPACT/HET data from the STEREO Ahead spacecraft.

SPDF/CDAWeb. Please also acknowledge the data producer: Christina Lee at UCB/SSL

SPDF/SSCWeb. Please also acknowledge the data producer: Christina Lee at UCB/SSL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Christina Lee at UCB/SSL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/het/2006/sta_l1_het_20061201_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.9305% of the 1438 timesteps. 

High Energy Telescope (from all.xml/instrument/description/@short)

Electron flux measured by HET in 3 energy bins (time series: good with plot overlay option, above)

Proton flux measured by the HET instrument in 11 energy bins (time series: good with plot overlay option, above)

The file contains burst criteria values from the IMPACT instrument on the STEREO Ahead spacecraft.

STEREO, In-situ Measurements of Particles and CME Transients, IMPACT, Experiment and Data Descriptions

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/burst/2006/sta_l1_impact_burst_20061028_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.7203% of the 16401 timesteps. 

Scaled SWAVES plasma power value used in burst criteria calculation

Scaled SWAVES HFR1 power value used in burst criteria calculation

Scaled SWAVES HFR2 power value used in burst criteria calculation

The file contains state of health data from the IMPACT instrument on the STEREO Ahead spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/hkp/2006/sta_l1_impact_hkp_20061028_v02.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.1749% of the 16347 timesteps. 

In-situ Measurements of Particles and CME Transients (from all.xml/instrument/description/@short)

Command sequence mask. Note: CDF_UINT4 data was converted to HAPI double.

PLASTIC Solid State Detector Voltage Monitor - primary side estimate

The file contains Level 1 IMPACT/LET data from the STEREO Ahead spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/let/2006/sta_l1_let_20061114_v07.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.7275% of the 366 timesteps. 

IMPACT Low Energy Telescope (from all.xml/instrument/description/@short)

Unsectored H flux at 12 energy bins in particles/(cm^2*sec*sr*MeV/nucleon)

Sectored low energy H flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 6 MeV/nuc

-->[DO NOT USE] Sectored low energy He3 flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 6 MeV/nuc (Valid before 2010-11-22)

-->Sectored low energy He4 flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 6 MeV/nuc

-->Sectored high energy He4 flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 6 and 12 MeV/nuc

-->Sectored low energy CNO flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 6 MeV/nuc

-->Sectored high energy CNO flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 6 and 12 MeV/nuc

-->Sectored low energy NiMgSi flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 6 MeV/nuc

-->Sectored high energy NeMgSi flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 6 and 12 MeV/nuc

-->Sectored low energy Fe flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 6 MeV/nuc (Valid before 2010-11-22)

-->Sectored high energy Fe flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 6 and 12 MeV/nuc (Valid before 2010-11-22)

Sectored low energy H counts in 16 look directions from 4 to 6 MeV/nuc

-->[DO NOT USE] Sectored low energy He3 counts in 16 look directions  from 4 to 6 MeV/nuc (Valid before 2010-11-22)

-->Sectored low energy He4 counts in 16 look directions  from 4 to 6 MeV/nuc

-->Sectored high energy He4 counts in 16 look directions  from 6 to 12 MeV/nuc

-->Sectored low energy CNO counts in 16 look directions  from 4 to 6 MeV/nuc

-->Sectored high energy CNO counts in 16 look directions  from 6 to 12 MeV/nuc

-->Sectored low energy NeMgSi counts in 16 look directions  from 4 to 6 MeV/nuc

-->Sectored high energy NeMgSi counts in 16 look directions  from 6 to 12 MeV/nuc

-->Sectored low energy Fe counts in 16 look directions  from 4 to 6 MeV/nuc (Valid before 2010-11-22)

-->Sectored high energy Fe counts in 16 look directions  from 6 to 12 MeV/nuc (Valid before 2010-11-22)

-->Sectored very low energy H flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 1.8 and 3.6 MeV/nuc (Valid after 2010-11-22)

-->Sectored very low energy H counts in 16 look directions from 1,8 to 3.6 MeV/nuc (Valid after 2010-11-22)

-->Sectored high energy H flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 6 and 10 MeV/nuc (Valid after 2010-11-22)

-->Sectored high energy H counts in 16 look directions from 6 to 10 MeV/nuc (Valid after 2010-11-22)

-->Sectored wide energy Fe flux in particles/(cm^2*s*sr*MeV/nuc) in 16 look directions between 4 and 12 MeV/nuc (Valid after 2010-11-22)

-->Sectored wide energy Fe counts in 16 look directions between 4 and 12 MeV/nuc (Valid after 2010-11-22)

Elemental Helium low energy sectored flux  in 16 look directions  from 4 to 6 MeV/nuc (Valid before 2010-11-22)

-->Elemental Helium low energy sectored counts  in 16 look directions  from 4 to 6 MeV/nuc (Valid before 2010-11-22)

H (proton) unsectored flux in 4 energy bins (as a time series overlay)

STEREO Ahead IMPACT/MAG Burst Mode (~0.03 sec) Magnetic Field Vectors (RTN)

The file contains Level 1 magnetic field vectors from the IMPACT/MAG instrument on the STEREO Ahead spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/rtn/magb/2006/sta_l1_magb_rtn_20061107_v06.cdf. The most common cadence, 31 [ms] = PT0.031S, occurred for 73.8086% of the 149168 timesteps. 

Solar Terrestrial Relations Observatory ` of the Sun-Earth Line (from all.xml/observatory/description/@short)

In-situ Measurements of Particles and CME Transients_Magnetometer (from all.xml/instrument/description/@short)

Solar Terrestrial Relations Observatory ` of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Magnetic field vector in RTN coordinates from the IMPACT/MAG instrument.

STEREO Ahead IMPACT/MAG Burst Mode (~0.03 sec) Magnetic Field Vectors (SC)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/sc/magb/2006/sta_l1_magb_sc_20061107_v06.cdf. The most common cadence, 31 [ms] = PT0.031S, occurred for 73.8091% of the 149169 timesteps. 

Solar Terrestrial Relations Observatory . of the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory . of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Magnetic field vector in Spacecraft coordinates from the IMPACT/MAG instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/rtn/mag/2006/sta_l1_mag_rtn_20061107_v06.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 99.9909% of the 691170 timesteps. 

Solar Terrestrial Relations Observatory , of the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory , of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

[HIGHLY ENCODED VALUES] IMPACT/MAG status flag. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/sc/mag/2006/sta_l1_mag_sc_20061107_v06.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 99.9909% of the 691170 timesteps. 

[HIGHLY ENCODED VALUES] IMPACT/MAG Status Flag. Note: CDF_UINT4 data was converted to HAPI double.

The file contains Level 1 IMPACT(In-situ Measurements of Particles and CME Transients)/SEPT data from the STEREO Ahead spacecraft.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_NS, @1 => Epoch_E.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_NS, @1 => Epoch_E.)

Solar Electron Proton Telescope (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch_NS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/sept/2006/sta_l1_sept_20061114_v08.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.7305% of the 370 timesteps. 

[DO NOT USE] Lowest Energy of each Spectral Energy Bin for Electrons

[DO NOT USE] Highest Energy of each Spectral Energy Bin for Electrons

[DO NOT USE] Highest Energy of each Spectral Energy Bin for Ions

[DO NOT USE] Geometric Mean Energy of each Spectral Energy Bin for Electrons

[DO NOT USE] Geometric Mean Energy of each Spectral Energy Bin for Ions

Counts based on variable 'Epoch_E' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/sept/2006/sta_l1_sept_20061114_v08.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.7305% of the 370 timesteps. 

The file contains Level 1 IMPACT(In-situ Measurements of Particles and CME Transients)/SIT data from the STEREO Ahead spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/sit/2007/sta_l1_sit_20070315_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Suprathermal Ion Telescope (from all.xml/instrument/description/@short)

--> H (proton) uncertainty in intensity expressed as sigma due to counting statistics

--> 3He uncertainty in intensity expressed as sigma due to counting statistics

--> 4He uncertainty in intensity expressed as sigma due to counting statistics

--> C (carbon) uncertainty in intensity expressed as sigma due to counting statistics

--> O (oxygen) uncertainty in intensity expressed as sigma due to counting statistics

--> NeS (neon through sulfur) uncertainty in intensity expressed as sigma due to counting statistics

--> Fe (iron) uncertainty in intensity expressed as sigma due to counting statistics

--> UH (ultra-heavy) uncertainty in intensity expressed as sigma due to counting statistics

The file contains Level 1 electron spectra from the IMPACT/STE instrument on the STEREO Ahead spacecraft.***NOTICE: Values for Detectors #1-4 (=STE-U #0-3) are saturated and should not be used ***

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/ste/2006/sta_l1_ste_20061101_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 99.3653% of the 2505 timesteps. 

IMPACT Suprathermal Electron Telescope (from all.xml/instrument/description/@short)

STE Electron Spectra [Values for detectors #1-4 are saturated and should not be used]

The file contains Level 1 3D burst mode electron distributions from the IMPACT(In-situ Measurements of Particles and CME Transients)/SWEA instrument on the STEREO Ahead spacecraft.  For important usage caveats see, https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html

STEREO In-Situ Measurements of Particles and CME Transients, IMPACT, Solar Wind Electron Analyzer, SWEA, Data Caveats web page, hosted by NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/swea_disb/2006/sta_l1_swea_disb_20061028_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.5736% of the 934 timesteps. 

Solar Wind Electron AnalyzerEnergy-Angle Burst Mode Distribution (from all.xml/instrument/description/@short)

SWEA 3D counts by 16 energies and 80 angles x=angles, y=energies [DO NOT USE energies below 45 eV]

The file contains Level 1 3D electron distributions from the IMPACT(In-situ Measurements of Particles and CME Transients)/SWEA instrument on the STEREO Ahead spacecraft. For important usage caveats see, https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/swea_dist/2006/sta_l1_swea_dist_20061028_v02.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 98.2966% of the 981 timesteps. 

STEREO-A  Solar Terrestrial Relations Observatory Ahead of the Sun-Earth Line (from all.xml/observatory/description/@short)

STEREO-A  Solar Terrestrial Relations Observatory Ahead of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

The file contains Level 1 spectra from the IMPACT/SWEA instrument on the STEREO Ahead spacecraft.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_Spectra, @1 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_Spectra, @1 => Epoch.)

In-situ Measurements of Particles and CME Transients/Solar Wind Electron Analyzer (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch_Spectra' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/swea_spec/2012/sta_l1_swea_spec_20121201_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 99.2939% of the 8578 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l1/impact/swea_spec/2012/sta_l1_swea_spec_20121201_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for 93.7464% of the 1619 timesteps. 

STEREO Ahead IMPACT/MAG Magnetic Field and PLASTIC Solar Wind Plasma Data

The file contains Level 2 magnetic field vectors from the IMPACT/MAG, solar wind parameters and space craft position data from the PLASTIC STEREO Ahead spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/impact/magplasma/1min/2006/sta_l2_magplasma_1m_20060101_v02.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.9910% of the 77417 timesteps. 

Solar Terrestrial Relations Observatory of the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Level-2 combined Mag and Plasma 1-minute average (from Master/CDFglobalAttributes/Data_type)

Spacecraft position in Heliocentric Aries Ecliptic (HAE) coordinates. 

Spacecraft position in Heliocentric Earth Ecliptic (HEE) coordinates.

Spacecraft position in Heliocentric Earth Equatorial (HEEQ) coordinates.

Direction cosine of radial velocity from the PLASTIC instrument.

Direction cosine of tangential velocity from the PLASTIC instrument.

Direction cosine of normal velocity from the PLASTIC instrument.

Cone Angle of magnetic field with respect to R direction (0 for anti-sunward, 180 for sunward)

Clock Angle of B-field in the T-N plane (atan2(BT,BN)). 0 along T. 90 along N.

PLASTIC - Plasma and Suprathermal Ion Composition.References: http://stereo.sr.unh.edu/stereo.html.

Please acknowledge the Principal Investigator, Dr. Antoinette Galvin of the University of New Hampshire, and NASA contract NAS5-00132.

See the rules of use available at http://stereo.sr.unh.edu/data/PLASTIC_Resources/index.htm

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Antoinette Galvin at University of New Hampshire

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Antoinette Galvin at University of New Hampshire

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Antoinette Galvin at University of New Hampshire

Counts based on variable 'epoch_10min' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/plastic/1dmax/10min/2007/sta_l2_pla_1dmax_10min_20070214_v09.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 60.1399% of the 86 timesteps. 

Solar Terrestrial Relations Observatory (from all.xml/observatory/description/@short)

Plasma and Suprathermal Ion Composition (from all.xml/instrument/description/@short)

Solar Terrestrial Relations Observatory (from Master/CDFglobalAttributes/Source_name)

1D Maxwellian Fits. 10 min averages. (from Master/CDFglobalAttributes/Data_type)

Indicates how sensitive the density value is to method for determining background correction.

Indicates when instrument flow angles are not in nominal s/c orientation.

Proton N/S Flow Angle. 1D Maxwellian Fit. Instrument Coordinates.

Counts based on variable 'epoch_1hr' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/plastic/1dmax/1hr/2007/sta_l2_pla_1dmax_1hr_20070214_v09.cdf. The most common cadence, 3599992 [ms] = PT59M59.992S, occurred for 43.4783% of the 10 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/plastic/1dmax/1min/2007/sta_l2_pla_1dmax_1min_20070214_v09.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 96.0389% of the 1382 timesteps. 

Proton 1D Maxwellian Fits (from Master/CDFglobalAttributes/Data_type)

PLASTIC> Level 2 Data. Alpha Data from RA 1DMax. 10 min averages.

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/plastic/alpha-1dmax/10min/2007/sta_l2_pla_alpha_ra_1dmax_10min_20070201_v02.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 99.7519% of the 2010 timesteps.

Alpha Data. 10 min averages (from Master/CDFglobalAttributes/Data_type)

PLASTIC> Level 2 Data. Alpha Data from RA 1DMax. 1 hour averages.

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/plastic/alpha-1dmax/1hr/2007/sta_l2_pla_alpha_ra_1dmax_1hr_20070101_v02.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 98.9061% of the 7595 timesteps.

Alpha Data. 1 hr averages (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/plastic/iron/2hr/2007/sta_l2_pla_iron_q_2hr_20070101_v02.cdf. The most common cadence, 7200000 [ms] = PT2H, occurred for all 4379 timesteps. 

Iron Charge State Data (from Master/CDFglobalAttributes/Data_type)

The file contains Level 2 PAD electron from the IMPACT SWEA instrument on the STEREO Ahead spacecraft

SPDF/CDAWeb. Please also acknowledge the data producer: Christina Lee at UC Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Christina Lee at UC Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Christina Lee at UC Berkeley Space Sciences Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l2/impact/swea/pad/2006/sta_l2_swea_pad_20061031_v04.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 98.3328% of the 2831 timesteps. 

Solar Terrestrial Relations Observatory Ahead (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory Ahead (from Master/CDFglobalAttributes/Source_name)

Pitch angle distribution in Phase Space Density (@ energies 1-10) 

The STEREO Plasma and Suprathermal Ion Composition, PLASTIC, web site with release notes and other information available, hosted by the University of New Hampshire, UNH

ReadMe for Alpha Particle, He⁺², Phase Space Densities from the STEREO PLASTIC Instrument, hosted by UNH

Description of STEREO PLASTIC Pick Up, He⁺², Phase Space Densities, PSD, in the spacecraft frame of reference as a function of V/Vsw, hosted by the University of New Hampshire, UNH

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/plastic/he2plus-f/01hr/2007/sta_l3_pla_he2pl_f_vsw_01hr_20070101_v05.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 6599 timesteps. 

PLASTIC He++ Hourly Phase Space Densities (from all.xml/instrument/description/@short)

(Stacked time-series) He++ Phase Space Density for mean V/Vsw, 6 V/Vsw means: 2.09 - 1.64 (km/s)/(km/s)

(Stacked time-series) He++ Counts for V/Vsw range, 6 V/Vsw means: 2.09 - 1.64 (km/s)/(km/s)

Readme for STEREO PLASTIC daily suprathermal He⁺ relative fluxes, last update: November 06, 2017

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/plastic/heplus/24hr/2007/sta_l3_pla_heplus_24hr_20070101_v06.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 274 timesteps. 

PLASTIC He+ Daily Fluxes by V/Vsw (from all.xml/instrument/description/@short)

STEREO Ahead PLASTIC Level 3 He+ Phase Space Density (PSD) Binned by V/Vsw, Hourly Resolution. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/plastic/heplus-f/01hr/2007/sta_l3_pla_heplus_f_vsw_01hr_20070101_v06.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 6599 timesteps. 

PLASTIC He+ Hourly Phase Space Densities (from all.xml/instrument/description/@short)

ReadMe for Singly-Charged Helium, He⁺, Phase Space Densities from the STEREO PLASTIC Instrument, hosted by UNH

Description of STEREO PLASTIC Pick Up, He⁺, Phase Space Densities, PSD, in the spacecraft frame of reference as a function of V/Vsw, hosted by the University of New Hampshire, UNH

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/plastic/heplus-f/10min/2007/sta_l3_pla_heplus_f_vsw_10min_20070101_v06.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 39599 timesteps. 

PLASTIC He+ 10-min Phase Space Densities (from all.xml/instrument/description/@short)

(Stacked time-series) He+ Phase Space Density for mean V/Vsw, 6 V/Vsw means: 2.09 - 1.64 (km/s)/(km/s)

(Stacked time-series) He+ Counts for V/Vsw range, 6 V/Vsw means: 2.09 - 1.64 (km/s)/(km/s)

STEREO Ahead PLASTIC Level 3 He+ Phase Space Density (PSD) Binned by V/Vsw

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/plastic/heplus-f/24hr/2007/sta_l3_pla_heplus_f_vsw_24hr_20070101_v06.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 274 timesteps. 

PLASTIC He+ Daily Phase Space Densities (from all.xml/instrument/description/@short)

Bower et al. (2019) Solar Wind PickUp Ion, PUI, Velocity Distributions, Journal of Geophysics, Space Physics Publication

Bower, J.S., Moebius, E., Berger, L., Farrugia, C., Keilbach, D., Lee, M. A., Quinn, P.R., Schwadron, N., and A. Taut, Effect of rapid changes of solar wind conditions on the pickup ion velocity distribution, J. Geophys. Res. Space Phys., 124, 6418-6437, 2019, DOI: 10.1029/2019JA026781

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/plastic/heplus-sw/5min/2007/sta_l3_pla_heplus_sw_velctdist_5min_20070101_v02.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 92447 timesteps. 

PLASTIC He+ 5min SW Frame Vel Ct Dist (from all.xml/instrument/description/@short)

This file includes radio measurements recorded by the STEREO-A/WAVES instrument. Time resolution varies with instrument mode ranging from 15 seconds to 1 minute.

Bougeret, J.L., Goetz, K., Kaiser, M.L. et al. S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission. Space Sci Rev 136, 487–528 (2008).
                

Cecconi, B., Bonnin, X., Hoang, S. et al. STEREO/Waves Goniopolarimetry. Space Sci Rev 136, 549–563 (2008).

Krupar, V., O. Santolik, B. Cecconi, M. Maksimovic, X. Bonnin, M. Panchenko, and A. Zaslavsky (2012), Goniopolarimetric inversion using SVD: An application to type III radio bursts observed by STEREO, J. Geophys. Res., 117, A06101.

 Data provided are publicly available. If used in presentations or publications, please acknowledge STEREO/Waves Investigation (M. Maksimovic and S. D. Bale, PIs). Please read carefully the caveats attached to the data. For reporting purposes, we request bibliography information for any publication, etc., using these data. Please send information on the use of this data to M. Maksimovic and S. D. Bale (PIs).

SPDF/CDAWeb. Please also acknowledge the data producer: Milan Maksimovic (milan.maksimovic@obspm.fr) and Stuart D. Bale (bale@berkeley.edu) at LESIA, Observatoire de Paris-PSL, CNRS and UC Berkeley Space Sciences Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Milan Maksimovic (milan.maksimovic@obspm.fr) and Stuart D. Bale (bale@berkeley.edu) at LESIA, Observatoire de Paris-PSL, CNRS and UC Berkeley Space Sciences Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Milan Maksimovic (milan.maksimovic@obspm.fr) and Stuart D. Bale (bale@berkeley.edu) at LESIA, Observatoire de Paris-PSL, CNRS and UC Berkeley Space Sciences Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/waves/hfr/2006/sta_l3_wav_hfr_20061028_v01.cdf. The most common cadence, 24179993570 [ns] = PT24.179994S, occurred for 3.1638% of the 107 timesteps. 

STEREO (Solar TErrestrial RElations Observatory) Ahead (from all.xml/observatory/description/@short)

STEREO-A/WAVES High Frequency Receiver (from all.xml/instrument/description/@short)

STEREO (Solar TErrestrial RElations Observatory) Ahead (from Master/CDFglobalAttributes/Source_name)

Power spectral density after 1% background subtraction and antenna calibration

Power spectral density after 1% background subtraction and antenna calibration in solar radio flux unit normalized to 1 au

Normalized linear polarization [Data available after 04-May-2007] 

Normalized circular polarization [Data available after 04-May-2007] 

The angular half aperture of the source as seen by a spacecraft (uniform profile) [Data available after 04-May-2007] 

Wave vector colatitude in the Radial-Tangential-Normal (RTN) system [Data available after 04-May-2007] 

Wave vector azimuth in the Radial-Tangential-Normal (RTN) system [Data available after 04-May-2007] 

Wave vector colatitude in the Heliocentric Inertial (HCI) system [Data available after 04-May-2007] 

Wave vector azimuth in the Heliocentric Inertial (HCI) system [Data available after 04-May-2007] 

Wave vector colatitude in the Heliocentric Earth Ecliptic (HEE) system [Data available after 04-May-2007] 

Wave vector azimuth in the Heliocentric Earth Ecliptic (HEE) system [Data available after 04-May-2007] 

Wave vector colatitude in the Heliocentric Earth Equatorial (HEEQ) system [Data available after 04-May-2007] 

Wave vector azimuth in the Heliocentric Earth Equatorial (HEEQ) system [Data available after 04-May-2007] 

STEREO spacecraft position in the Heliocentric Inertial (HCI) system in km

STEREO spacecraft position in the Heliocentric Earth Ecliptic (HEE) system in km

STEREO spacecraft position in the Heliocentric Earth Equatorial (HEEQ) system in km

Data provided are publicly available. If used in presentations or publications, please acknowledge STEREO/Waves Investigation (M. Maksimovic, PIs). Please read carefully the caveats attached to the data. For reporting purposes, we request bibliography information for any publication, etc., using these data. Please send information on the use of this data to: M. Maksimovic (PI).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/l3/waves/lfr/2006/sta_l3_wav_lfr_20061028_v01.cdf. The most common cadence, 24679005146 [ns] = PT24.679005S, occurred for 5.5934% of the 189 timesteps. 

STEREO-A/WAVES Low Frequency Receiver (from all.xml/instrument/description/@short)

Normalized linear polarization [Data available after 03-Dec-2012] 

Normalized circular polarization [Data available after 03-Dec-2012] 

The angular half aperture of the source as seen by a spacecraft (uniform profile) [Data available after 03-Dec-2012] 

Wave vector colatitude in the Radial-Tangential-Normal (RTN) system [Data available after 03-Dec-2012] 

Wave vector azimuth in the Radial-Tangential-Normal (RTN) system [Data available after 03-Dec-2012] 

Wave vector colatitude in the Heliocentric Inertial (HCI) system [Data available after 03-Dec-2012] 

Wave vector azimuth in the Heliocentric Inertial (HCI) system [Data available after 03-Dec-2012] 

Wave vector colatitude in the Heliocentric Earth Ecliptic (HEE) system [Data available after 03-Dec-2012]

Wave vector azimuth in the Heliocentric Earth Ecliptic (HEE) system [Data available after 03-Dec-2012]

Wave vector colatitude in the Heliocentric Earth Equatorial (HEEQ) system [Data available after 03-Dec-2012]

Wave vector azimuth in the Heliocentric Earth Equatorial (HEEQ) system [Data available after 03-Dec-2012]

This file contains Beacon data from the IMPACT experiment on the STEREO Ahead spacecraft.Note: The onboard SWEA calculation of moments and PADs are compromised by a charging effect at low energies. STE-U is not providing any science data as the instrument is blinded by sunlight and thus these variables are not accessible via CDAWeb

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_MAG, @1 => Epoch, @2 => Epoch_SEP.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_MAG, @1 => Epoch, @2 => Epoch_SEP.)

SolarTerrestrial Relations Observatory Ahead of the Sun-Earth Line (from all.xml/observatory/description/@short)

SolarTerrestrial Relations Observatory Ahead of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Magnetic field vector in STEREO-A Heliocentric Radial Tangential Normal coordinates

Counts based on variable 'Epoch_MAG' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/beacon/2007/sta_lb_impact_20070320_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 91.8261% of the 528 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/beacon/2007/sta_lb_impact_20070320_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 50.5263% of the 48 timesteps. 

---> Spacecraft Status code. Note: CDF_UINT4 data was converted to HAPI double.

---> Instrument Activity Code. Note: CDF_UINT4 data was converted to HAPI double.

---> SWEA Mode ID. Note: CDF_UINT4 data was converted to HAPI double.

---> STE Mode ID. Note: CDF_UINT4 data was converted to HAPI double.

---> MAG HKP Status Code. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'Epoch_SEP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/beacon/2007/sta_lb_impact_20070320_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 51.5789% of the 49 timesteps. 

---> LET Number of Front-end Triggers. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Number of events with hazard flag. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Number of accepted events. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Code OK. Internal code check, 1=good, 0=bad. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Heater Duty Cycle. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Leakage Current Balance, 1=ok, 0=bad. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Dynamic Thresholding State, 0=normal, 1,2,3=higher threshold setting. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Minute Counter - rolls over at 60. Note: CDF_UINT4 data was converted to HAPI double.

---> SEPT Status Code. Note: CDF_UINT4 data was converted to HAPI double.

LET Proton Flux in 4 bins (middle 2 have same energy, but different angular coverage)

---> LET 4He Flux in 5 bins. Bins 1,2 and 3,4 have same energy coverage but different angular coverage

HET Electron Counts (0.7 - 4 MeV). Note: CDF_UINT4 data was converted to HAPI double.

---> HET Proton Counts (in 3 energy bins). Note: CDF_UINT4 data was converted to HAPI double.

---> HET CNO Counts (in 2 energy bins). Note: CDF_UINT4 data was converted to HAPI double.

---> HET Fe Cnts (52 - 74 MeV/nuc). Note: CDF_UINT4 data was converted to HAPI double.

SIT He Counts. Note: CDF_UINT4 data was converted to HAPI double.

---> SIT CNO Counts. Note: CDF_UINT4 data was converted to HAPI double.

---> SIT Fe Counts. Note: CDF_UINT4 data was converted to HAPI double.

LET Proton Counts. Note: CDF_UINT4 data was converted to HAPI double.

---> LET 4He Counts. Note: CDF_UINT4 data was converted to HAPI double.

---> LET 3He Counts. Note: CDF_UINT4 data was converted to HAPI double.

---> LET CNO Counts. Note: CDF_UINT4 data was converted to HAPI double.

---> LET Fe Counts. Note: CDF_UINT4 data was converted to HAPI double.

SEPT Electron Counts. Note: CDF_UINT4 data was converted to HAPI double.

SEPT Ion Counts. Note: CDF_UINT4 data was converted to HAPI double.

HET He Counts. Note: CDF_UINT4 data was converted to HAPI double.

Summary Flux SEPT Electrons from 0.035 to 0.065 MeV summed in all directions

Summary Counts SEPT Electrons from 0.035 to 0.065 MeV. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts HET Electrons from 0.7 to 4 MeV. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts SEPT Ions from 0.137 to 0.623 MeV. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts SEPT Ions from 0.623 to 2.22 MeV. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts LET Protons from 2.2 to 12 MeV. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts HET Protons from 13 to 100 MeV. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts SIT Helium from 0.12 to 1.08 MeV/nuc. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts SIT CNO from 0.12 to 1.08 MeV/nuc. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts SIT Fe from 0.12 to 1.08 MeV/nuc. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts LET Helium from 4 to 12 MeV/nuc. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts LET CNO from 4 to 12 MeV/nuc. Note: CDF_UINT4 data was converted to HAPI double.

---> Summary Counts LET Fe from 4 to 12 MeV/nuc. Note: CDF_UINT4 data was converted to HAPI double.

STEREO Ahead IMPACT Reprocessed Beacon MAG Magnetic Field Vectors around 2015 Solar Conjunction

The file contains Level Beacon magnetic field vectors from the IMPACT/MAG instrument on the STEREO Ahead spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/beacon_mag/2014/sta_lb_mag_rtn_20140801_v06.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 99.9421% of the 8634 timesteps. 

PLASTIC - Plasma and Suprathermal Ion and Composition.References: http://stereo.sr.unh.edu/stereo.html.PLASTIC Beacon data has not been validated and should not be used for publication purposes.

Counts based on variable 'Epoch1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/ahead/beacon_plastic/2011/sta_lb_pla_browse_20110706_v10.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 98.1233% of the 366 timesteps. 

Plasma and Suprathermal Ion and Composition (from all.xml/instrument/description/@short)

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs).  These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations. About STEREO data in COHOWEB STEREO-A and -B data are from the magnetometer of the IMPACT package and from the PLASTIC plasma detector.  Principal Investigators for these packages are Janet Luhmann (UCB) and Antoinette Galvin (UNH), respectively.  Magnetic field  data were obtained as 10-min averages from the UCLA web site at http://aten.igpp.ucla.edu/forms/stereo/ascii_PLASTIC_10m_new.html, courtesy of C.T. Russell. Proton Fluxes from http://www.srl.caltech.edu/STEREO/.  COHOWeb's magnetic field hourly averages were created at GSFC/SPDF by averaging over the six 10-min averages falling within each hour.  Hourly plasma parameter data, including plasma flow direction angles for STEREO-A but not yet for STEREO B (as of 7/11/2010), were obtained from UNH via http://fiji.sr.unh.edu/1dmax_ascii/.

General information concerning the STEREO B, In-Situ Measurements of Particles and CME Transients, IMPACT, instrument

General information concerning the STEREO B, Plasma and Supra-Thermal Ion Composition, PLASTIC, instrument

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/coho1hr_magplasma/2007/stb_coho1hr_merged_mag_plasma_20070101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Solar Terrestrial Relations Observatory Behind the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory Behind the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/helio1day/stb_helio1day_position_20061027_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 8268 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/helio1hr/stb_helio1hr_position_20061027_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 157775 timesteps. 

The file contains Level 1 IMPACT/HET data from the STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/het/2006/stb_l1_het_20061201_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.8592% of the 1418 timesteps. 

Solar Terrestrial Relations Observatory Behind of the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory Behind of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

The file contains burst criteria values from the IMPACT instrument on the STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/burst/2006/stb_l1_impact_burst_20061028_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.3391% of the 8868 timesteps. 

The file contains state of health data from the IMPACT instrument on the STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/hkp/2006/stb_l1_impact_hkp_20061028_v02.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 98.7189% of the 8862 timesteps. 

The file contains Level 1 IMPACT/LET data from the STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/let/2006/stb_l1_let_20061114_v07.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.8609% of the 1436 timesteps. 

STEREO Behind IMPACT/MAG Burst Mode (~0.03 sec) Magnetic Field Vectors

The file contains Level 1 magnetic field vectors from the IMPACT/MAG instrument on the STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/rtn/magb/2006/stb_l1_magb_rtn_20061107_v06.cdf. The most common cadence, 31 [ms] = PT0.031S, occurred for 74.1588% of the 149565 timesteps. 

STEREO Behind IMPACT/MAG Burst Mode (~0.03 sec) Magnetic Field Vectors (SC)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/sc/magb/2006/stb_l1_magb_sc_20061107_v06.cdf. The most common cadence, 31 [ms] = PT0.031S, occurred for 74.1588% of the 149565 timesteps. 

Solar Terrestrial Relations Observatory @ of the Sun-Earth Line (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory @ of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/rtn/mag/2006/stb_l1_mag_rtn_20061107_v06.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 99.9822% of the 689431 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/sc/mag/2006/stb_l1_mag_sc_20061107_v06.cdf. The most common cadence, 125 [ms] = PT0.125S, occurred for 99.9822% of the 689431 timesteps. 

The file contains Level 1 IMPACT(In-situ Measurements of Particles and CME Transients)/SEPT data from the STEREO Behind spacecraft.

Counts based on variable 'Epoch_NS' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/sept/2006/stb_l1_sept_20061113_v06.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.1597% of the 236 timesteps. 

Counts based on variable 'Epoch_E' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/sept/2006/stb_l1_sept_20061113_v06.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.1597% of the 236 timesteps. 

The file contains Level 1 IMPACT(In-situ Measurements of Particles and CME Transients)/SIT data from the STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/sit/2007/stb_l1_sit_20070315_v03.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

The file contains Level 1 electron spectra from the IMPACT/STE instrument on the STEREO Behind spacecraft.***NOTICE: Values for Detectors #1-4 (=STE-U #0-3) are saturated and should not be used***

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/ste/2006/stb_l1_ste_20061101_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 98.8324% of the 1439 timesteps. 

The file contains Level 1 3D burst mode electron distributions from the IMPACT(In-situ Measurements of Particles and CME Transients)/SWEA instrument on the STEREO Behind spacecraft.  For important usage caveatssee, https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/swea_disb/2006/stb_l1_swea_disb_20061028_v01.cdf. The most common cadence, 2000 [ms] = PT2S, occurred for 99.4671% of the 560 timesteps. 

Solar Wind Electron Analyzer Energy-Angle Burst Mode Distribution (from all.xml/instrument/description/@short)

The file contains Level 1 3D electron distributions from the IMPACT(In-situ Measurements of Particles and CME Transients)/SWEA instrument on the STEREO Behind spacecraft.  For important usage caveats see, https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/swea_dist/2006/stb_l1_swea_dist_20061028_v02.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 96.1538% of the 450 timesteps. 

The file contains Level 1 spectra from the IMPACT/SWEA instrument on the STEREO Behind spacecraft.

Counts based on variable 'Epoch_Spectra' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/swea_spec/2012/stb_l1_swea_spec_20121201_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 98.9842% of the 8185 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l1/impact/swea_spec/2012/stb_l1_swea_spec_20121201_v01.cdf. The most common cadence, 50000 [ms] = PT50S, occurred for 91.2281% of the 1508 timesteps. 

STEREO Behind IMPACT/MAG Magnetic Field and PLASTIC Solar Wind Plasma Data

The file contains Level 2 magnetic field vectors from the IMPACT/MAG, solar wind parameters and space craft position data from the PLASTIC STEREO Behind spacecraft.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/impact/magplasma/1min/2006/stb_l2_magplasma_1m_20060101_v02.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.9871% of the 77534 timesteps. 

Counts based on variable 'epoch_10min' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/plastic/1dmax/10min/2007/stb_l2_pla_1dmax_10min_20070301_v09.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 52.4476% of the 75 timesteps. 

Proton E/W Flow Angle. Instrument Coordinates.[Available for 2007 only]

Proton N/S Flow Angle. 1D Maxwellian Fit. HERTN [Available for 2007 only]

Proton N/S Flow Angle. 1D Maxwellian Fit. RTN [Available for 2007 only]

Counts based on variable 'epoch_1hr' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/plastic/1dmax/1hr/2007/stb_l2_pla_1dmax_1hr_20070301_v09.cdf. The most common cadence, 3599988 [ms] = PT59M59.988S, occurred for 60.8696% of the 14 timesteps. 

Proton E/W Flow Angle. Instrument Coordinates. [Available for 2007 only]

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/plastic/1dmax/1min/2007/stb_l2_pla_1dmax_1min_20070301_v09.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 95.1816% of the 1363 timesteps. 

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/plastic/alpha-1dmax/10min/2007/stb_l2_pla_alpha_ra_1dmax_10min_20070301_v04.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 99.9552% of the 4461 timesteps.

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/plastic/alpha-1dmax/1hr/2007/stb_l2_pla_alpha_ra_1dmax_1hr_20070101_v04.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for 99.5914% of the 7313 timesteps.

Alpha Data. 1 hour averages (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/plastic/iron/2hr/2007/stb_l2_pla_iron_q_2hr_20070101_v02.cdf. The most common cadence, 7200000 [ms] = PT2H, occurred for all 4379 timesteps. 

The file contains Level 2 PAD electron from the IMPACT SWEA instrument on the STEREO Behind spacecraft

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l2/impact/swea/pad/2006/stb_l2_swea_pad_20061106_v04.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 95.9375% of the 2763 timesteps. 

Solar Terrestrial Relations Observatory Behind (from all.xml/observatory/description/@short)

Solar Terrestrial Relations Observatory Behind (from Master/CDFglobalAttributes/Source_name)

Pitch angle distribution in Phase Space Density (@ energies 1-10)

This file includes radio measurements recorded by the STEREO-B/WAVES instrument. Time resolution varies with instrument mode ranging from 15 seconds to 1 minute.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l3/waves/hfr/2006/stb_l3_wav_hfr_20061030_v01.cdf. The most common cadence, 24179993570 [ns] = PT24.179994S, occurred for 3.6788% of the 126 timesteps. 

STEREO (Solar TErrestrial RElations Observatory) Behind (from all.xml/observatory/description/@short)

STEREO-B/WAVES High Frequency Receiver (from all.xml/instrument/description/@short)

STEREO (Solar TErrestrial RElations Observatory) Behind (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/l3/waves/lfr/2006/stb_l3_wav_lfr_20061030_v01.cdf. The most common cadence, 24679005146 [ns] = PT24.679005S, occurred for 5.7552% of the 197 timesteps. 

STEREO-B/WAVES Low Frequency Receiver (from all.xml/instrument/description/@short)

Normalized linear polarization [Data available after 11-Dec-2012] 

Normalized circular polarization [Data available after 11-Dec-2012] 

The angular half aperture of the source as seen by a spacecraft (uniform profile) [Data available after 11-Dec-2012] 

Wave vector colatitude in the Radial-Tangential-Normal (RTN) system [Data available after 11-Dec-2012] 

Wave vector azimuth in the Radial-Tangential-Normal (RTN) system [Data available after 11-Dec-2012] 

Wave vector colatitude in the Heliocentric Inertial (HCI) system [Data available after 11-Dec-2012] 

Wave vector azimuth in the Heliocentric Inertial (HCI) system [Data available after 11-Dec-2012] 

Wave vector colatitude in the Heliocentric Earth Ecliptic (HEE) system [Data available after 11-Dec-2012] 

Wave vector azimuth in the Heliocentric Earth Ecliptic (HEE) system [Data available after 11-Dec-2012] 

Wave vector colatitude in the Heliocentric Earth Equatorial (HEEQ) system [Data available after 11-Dec-2012] 

Wave vector azimuth in the Heliocentric Earth Equatorial (HEEQ) system [Data available after 11-Dec-2012] 

This file contains Beacon data from the IMPACT experiment on the STEREO Behind spacecraft.Note: The onboard SWEA calculation of moments and PADs are compromised by a charging effect at low energies. STE-U is not providing any science data as the instrument is blinded by sunlight and thus these variables are not accessible via CDAWeb

SolarTerrestrial Relations Observatory Behind of the Sun-Earth Line (from all.xml/observatory/description/@short)

SolarTerrestrial Relations Observatory Behind of the Sun-Earth Line (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch_MAG' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/beacon/2007/stb_lb_impact_20070320_v01.cdf. The most common cadence, 10000 [ms] = PT10S, occurred for 97.9402% of the 1474 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/beacon/2007/stb_lb_impact_20070320_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 87.6000% of the 219 timesteps. 

Counts based on variable 'Epoch_SEP' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/beacon/2007/stb_lb_impact_20070320_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 94.4000% of the 236 timesteps. 

Counts based on variable 'Epoch1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/behind/beacon_plastic/2011/stb_lb_pla_browse_20110706_v10.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 97.1360% of the 407 timesteps. 

STEREO WAVES (SWAVES) Radio Intensity Spectra, both Ahead and Behind s/c

STEREO/WAVES instrument page maintained by NASA GSFC with science and instrument descriptions, data, personnel, publications, and related links sections

STEREO mission page with spacecraft and instrument descriptions, news, links to data (STEREO Science Center), and image gallerys

SPDF/CDAWeb. Please also acknowledge the data producer: M. Kaiser at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: M. Kaiser at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M. Kaiser at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stereo/combined/swaves/level2_cdf/2006/stereo_level2_swaves_20061027_v02.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Solar TErrestrial RElations Observatory (from all.xml/observatory/description/@short)

Solar TErrestrial RElations Observatory (from Master/CDFglobalAttributes/Source_name)

Ahead:  Electric field avg intensity (dB above bgnd, 367 freqs 2.6 kHz - 16.025 MHz, inverted frequency order)

Behind:  Electric field avg intensity (dB above bgnd, 367 log-spaced freqs 2.6 kHz - 16.025 MHz, normal frequency order)

Electron flux energy levels :1024 linearly spaced channels ranging between 15 keV and 146 keV.Dosimeter Daily Dose :Temporal resolution of 1 s, Integral energy range of 100 keV - 15 MeV.

SPDF/CDAWeb. Please also acknowledge the data producer: G. McHarg at United States Air Force Academy

SPDF/SSCWeb. Please also acknowledge the data producer: G. McHarg at United States Air Force Academy

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. McHarg at United States Air Force Academy

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => SEED_Time_Dt15_Good, @2 => SEED_Dosimeter_Time.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => SEED_Time_Dt15_Good, @2 => SEED_Dosimeter_Time.)

Solid-state Energetic Electron Detector (from all.xml/instrument/description/@short)

Default time in TT2000.  This time is used for the raw SEED electron data. 

SEED Electron Counts for energy between 13.743 and 146.18 keV. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stp/stpsat-6/falconseed/2022/stpsat-6_falcon_seed-l1_20220115_v01.cdf. The most common cadence, 14999999106 [ns] = PT14.999999S, occurred for 70.8197% of the 648 timesteps. 

Time stamp for all delta time = 15 seconds.  This time vector contains the starting times for each 15 second interval.

SEED Electron Counts Dt15(Dt15 -> Delta t = 15 seconds). Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'SEED_Time_Dt15_Good' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stp/stpsat-6/falconseed/2022/stpsat-6_falcon_seed-l1_20220115_v01.cdf. The most common cadence, 14999999106 [ns] = PT14.999999S, occurred for 70.8945% of the 531 timesteps. 

SEED Electron Flux for time intervals of delta t = 15 seconds.  Electron Flux at 904 energies (20 - 146 keV), scalar

SEED Dosimeter Counts. Note: CDF_UINT4 data was converted to HAPI double.

Counts based on variable 'SEED_Dosimeter_Time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/stp/stpsat-6/falconseed/2022/stpsat-6_falcon_seed-l1_20220115_v01.cdf. The most common cadence, 999994576 [ns] = PT0.999995S, occurred for 33.9056% of the 1896 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/suisei/helio1day/suisei_helio1day_position_19890101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 4016 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/suisei/helio1hr/suisei_helio1hr_position_19890101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 96407 timesteps. 

Additional and higher-resolution data products now available at the

SPDF/CDAWeb. Please also acknowledge the data producer: Glenn Mason at JHU/APL

SPDF/SSCWeb. Please also acknowledge the data producer: Glenn Mason at JHU/APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Glenn Mason at JHU/APL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sampex/combined_cdaweb/30f/1992/sx_k0_30f_19920706_v02.cdf. The most common cadence, 30000 [ms] = PT30S, occurred for 99.7914% of the 2870 timesteps. 

Solar Anomalous Magnetic Particle Explorer (from all.xml/observatory/description/@short)

Solar Anomalous Magnetic Particle Explorer (from Master/CDFglobalAttributes/Source_name)

GEI X,Y,Z coordinates (km);X-Y in equatorial plane;X to vernal equinox

losscome 1: Pitch half-angle of cone withparticles that mirror at <100 km,same hemisphere

losscone 2:Pitch-angle cone containing particles mirroring at <100 km,at either(other ??) hemisphere

Mag vector, geographic: magnetic components,radial,south (theta), and east (phi)

 mag radial distance of ECD B-field line top point,km; akin to dipole L.

magnetic equator: B-field magnitude,alt.,geogr_long. and lat. at mag_equator pass

parameters at N100 mirror: B-magnitude,alt.,geogr_long,lat at north '100 km' level of field line

parameters at S100 mirror: B-magnitude,alt., geogr_long,lat. at south '100 km' point on B-line

zenith-bore angle: angle between zenith and S/C z-axis,i.e, instrument bore. axis

azimuth:  angle of s/c z-axis projected on horizontal plane;0=east,90=north

Sun-B angle: cos of angle between sun line and local magnetic field vector

Z>2 dif fluxes, 9 channels (0.5-220 MeV/nu)from LICA,HILT,and MAST detectors

He Dif Fluxes, 4 channels (0.5-38 MeV/nu): from LICA, HILT, and MAST detectors

Integral Flux, E- or H from LICA.E>0.6 MeV electrons and/or E>0.8 MeV protons

Sigma:Z>2 dif fluxes, 9 channels (0.5-220 MeV/nu)from LICA,HILT,and MAST detectors

Sigma: He Dif Fluxes, 4 channels;(0.5-38 MeV/nu):from LICA, HILT, and MAST detectors

Sigma: H+ (mainly) Dif Fluxes, 2 channels:from MAST and PET detectors

Sigma: Electr Dif Fluxes, 2 channels;(2-16 MeV) from PET instrument.

Sigma: Integral Flux, E- or H from LICA.E>0.6 MeV electrons and/orE>0.8 MeV protons

Extensive PDF document prepared by M. Lennard, J. Mazur, and G. Mason originally in 1996 and most recently updated in 2007 to describe the many NSSDC-resident SAMPEX data sets, including the polar cap averaged fluxes. This document also identifies a series of mission and instrument papers at IEEE Transactions on Geoscience and Remote Sensing, Vol. 31, No. 3, May 1993

SPDF/CDAWeb. Please also acknowledge the data producer: G.MASON at JHU/APL

SPDF/SSCWeb. Please also acknowledge the data producer: G.MASON at JHU/APL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G.MASON at JHU/APL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sampex/combined_cdaweb/pof/1992/sx_k0_pof_19920706_v01.cdf. The most common cadence, 2970000 [ms] = PT49M30S, occurred for 9.1678% of the 65 timesteps. 

Solar Anomalous Magnetospheric Particle Explorer (from all.xml/observatory/description/@short)

Solar Anomalous Magnetospheric Particle Explorer (from Master/CDFglobalAttributes/Source_name)

Z>2 dif fluxes, 9 channels (0.5-220 MeV/nu)from LICA, HILT,and MAST detectors

He Dif Fluxes, 4 channels (0.5-38 MeV/nu); from LICA, HILT, and MAST detectors

Sigma:Z>2 dif fluxes, 9 channels (0.5-MeV/nu)from LICA,HILT,and MAST detectors

Sigma: Electr Dif Fluxes, 2 channels;(1.5-14 MeV) from PET instrument.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/tha/ssc_pre/2008/thapred_or_ssc_20080101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 240450 timesteps. 

Produced by Mission Ops, Science Ops and Science Team..V00: Predictive on all, pre-pass.V01: Intermediate: added definitive spinper, spinphase others predictive, expected shortly after pass.V02: Preliminary: added definitive position, expected shortly after OD update (1 day after pass).V03: Definitive: added science attitude determination using perigee data post-processing

Details on THEMIS data policy and giving proper credits in publications.

Ephemeris file format and quantity details including RoI descriptions.

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos at UCB, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos at UCB, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos at UCB, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_state_epoch, @1 => tha_spin_epoch, @2 => tha_spin_ecl_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_state_epoch, @1 => tha_spin_epoch, @2 => tha_spin_ecl_epoch.)

[Not populated yet] Initial angle offset between IDPU model and eclipse model in this segment.

[Not populated yet] Marker for eclipse segments. Note: CDF_UINT4 data was converted to HAPI double.

Initial angle offset between IDPU model and eclipse model in this segment (eclipse spin model).

Marker for eclipse segments (eclipse spin model). Note: CDF_UINT4 data was converted to HAPI double.

THEMIS-A: Electric Field Instrument (EFI) Electric field measurements. The L2 product is a 3D estimate of Eperp derived from the spin plane E-field measurements assuming E dot B = 0, using relevant FGM (Flux-Gate Magnetometer) data.Includes spin-averaged, and Fast-survey field data.Spin-averaged (EFS_DOT0) data has approximately 3 second time resolution. Fast-survey (EFF_DOT0) data has 1/8 second time resolution.

THEMIS Electric Field Instrument, EFI, Instrument Description with Links to Information concerning Data Modes, Data Products, and Caveats

THEMIS Electric Field Instrument, EFI, Processing History with a Link To Data Variable Descriptions

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, J. Bonnell & F. Mozer at UCB, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, J. Bonnell & F. Mozer at UCB, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, J. Bonnell & F. Mozer at UCB, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_efs_dot0_epoch, @1 => tha_eff_dot0_epoch, @2 => tha_eff_q_mag_epoch, @3 => tha_eff_q_pha_epoch, @4 => tha_eff_e12_efs_epoch, @5 => tha_eff_e34_efs_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_efs_dot0_epoch, @1 => tha_eff_dot0_epoch, @2 => tha_eff_q_mag_epoch, @3 => tha_eff_q_pha_epoch, @4 => tha_eff_e12_efs_epoch, @5 => tha_eff_e34_efs_epoch.)

tha_efs_dot0_epoch: Electric field Instrument Spin-fit (EFS_DOT0, approx. 3 sec time resolution) epoch variable

EFS_DOT0 (spin-fit, using E dot B=0) electric field vector in GSE coordinates 

EFS_DOT0 (spin-fit, using E dot B=0) electric field vector in GSM coordinates 

EFS_DOT0 (spin-fit, using E dot B=0) electric field vector in XYZ despun spacecraft coordinates (DSL)

tha_eff_dot0_epoch: Electric field Instrument Fast-survey (EFF_DOT0, 1/8 sec time resolution) epoch variable

EFF_DOT0 (fast-survey, 1/8 sec time resolution, using E dot B=0) electric field vector in GSE coordinates 

EFF_DOT0 (fast-survey, 1/8 sec time resolution, using E dot B=0) electric field vector in GSM coordinates 

EFF_DOT0 (fast-survey, 1/8 sec time resolution, , using E dot B=0) electric field vector in XYZ despun spacecraft coordinates (DSL)

tha_eff_q_mag_epoch: Electric field Instrument Spin-averaged (EFF_Q_MAG, approx. 3 sec time resolution) epoch variable

EFF_Q_MAG (Data Quality Parameter: equal to the spin-fit E34 electric field magnitude divided by the spin-fit E12 electric field magnitude. Good values are near 1.0) 

tha_eff_q_pha_epoch: Electric field Instrument Spin-averaged (EFF_Q_PHA, approx. 3 sec time resolution) epoch variable

EFF_Q_PHA (Data Quality Parameter: equal to the cosine of the angle between the spin-fit E34 electric field and the spin-fit E12 electric field. Good values are near 1.0) 

tha_eff_e12_efs_epoch: Electric field Instrument Spin-averaged (EFF_E12_EFS, approx. 3 sec time resolution) epoch variable

E12_EFS, Ground Spin-fit (using E12), spin plane electric field vector in XYZ despun spacecraft coordinates (DSL)

tha_eff_e34_efs_epoch: Electric field Instrument Spin-averaged (EFF_E34_EFS, approx. 3 sec time resolution) epoch variable

E34_EFS, Ground Spin-fit (using E34), spin plane electric field vector in XYZ despun spacecraft coordinates (DSL)

THEMIS-A: Electric Field Instrument Particle Burst Mode (EFP) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/128 to 1/512 second time resolution.

tha_efp_epoch: Electric field Instrument Fast-survey (EFP, 1/8 sec time resolution) epoch variable

EFP (Particle Burst, 1/128 to 1/512 sec time resolution) electric field vector in GSE coordinates 

EFP (Particle Burst, 1/128 to 1/512 sec time resolution) electric field vector in GSM coordinates 

EFP (Particle Burst, 1/128 to 1/512 sec time resolution) electric field vector in XYZ despun spacecraft coordinates (DSL)

THEMIS-A: Electric Field Instrument Wave Burst Mode (EFW) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/16384 second time resolution.

tha_efw_epoch: Electric field Instrument Fast-survey (EFW, 1/8 sec time resolution) epoch variable

EFW (Wave Burst, 1/128 to 1/16384 sec time resolution) electric field vector in GSE coordinates 

EFW (Wave Burst, 1/128 to 1/16384 sec time resolution) electric field vector in GSM coordinates 

EFW (Wave Burst, 1/128 to 1/16384 sec time resolution) electric field vector in XYZ despun spacecraft coordinates (DSL)

THEMIS-A (P5): Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution.

THEMIS-A: Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 2: Counter saturation, 4: Solar Wind not in Solar Wind Mode, or Solar Wind Mode, not in Solar Wind, 8: (Reduced Mode only) slow survey mode+flows, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Instrument description including data modes, products and caveats

Processing history and the THEMIS mission website including TDAS s/w

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, C.W. Carlson & J. McFadden at UCB, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, C.W. Carlson & J. McFadden at UCB, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, C.W. Carlson & J. McFadden at UCB, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_peif_epoch, @1 => tha_peef_epoch, @2 => tha_peir_epoch, @3 => tha_peer_epoch, @4 => tha_peib_epoch, @5 => tha_peeb_epoch, @6 => tha_eesa_solarwind_flag_epoch, @7 => tha_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_peif_epoch, @1 => tha_peef_epoch, @2 => tha_peir_epoch, @3 => tha_peer_epoch, @4 => tha_peib_epoch, @5 => tha_peeb_epoch, @6 => tha_eesa_solarwind_flag_epoch, @7 => tha_iesa_solarwind_flag_epoch.)

ESA Full Mode Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/esa_flag.shtml.) 

(Good data only) ESA Full (High Angular Resolution, few minute time res.) Mode, Ion Density 

Ion Symmetry Vector (direction of pressure tensor symmetry (DSL)) 

-----Ion Symmetry Vector (direction of pressure tensor symmetry (DSL)) 

Magnetic Field Vector in DSL (Same time array as Full Ion ESA data)

-----Magnetic Field Vector in DSL (Same time array as Full Ion ESA data) 

(All qualities data) ESA Full (High Angular Resolution, few minute time res.) Mode, Ion Density

Ion Diagonalized Temperature (Tprp1, Tprp2, Tpar)(all qualities)

Temperature, Field Aligned (TprpFA1, TprpFA2, TparFA)(all qualities)

Ion Symmetry Vector (direction of pressure tensor symmetry (DSL))(all qualities)

Magnetic Field Vector in DSL (Same time array as Full Ion ESA data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Full Ion ESA data)

ESA Full Mode, Electron Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/esa_flag.shtml.) 

(Good data only) ESA Full (High Angular Resolution, few minute time res.) Mode, Electron Density

-----Electron Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA) 

Electron Symmetry Vector (direction of pressure tensor symmetry (DSL)) 

-----Electron Symmetry Vector (direction of pressure tensor symmetry (DSL)) 

-----Electron Symmetry Angle (between symmetry direction and B) 

Magnetic Field Vector in DSL (Same time array as Full Electron ESA data) 

-----Magnetic Field Vector in DSL (Same time array as Full Electron ESA data) 

(All qualities data) ESA Full (High Angular Resolution, few minute time res.) Mode, Electron Density

Electron Diagonalized Temperature (Tprp1, Tprp2, Tpar)(all qualities)

Electron Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA)(all qualities)

-----Electron Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA)

Electron Symmetry Vector (direction of pressure tensor symmetry (DSL))(all qualities) 

Magnetic Field Vector in DSL (Same time array as Full Electron ESA data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Full Electron ESA data)

ESA Reduced Mode, Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/esa_flag.shtml.) 

(Good data only) ESA Reduced (Low Angular Res., 3-s Time Res.) Mode, Ion Density

Magnetic Field Vector in DSL (Same time array as Reduced Ion ESA data)

-----Magnetic Field Vector in DSL (Same time array as Reduced Ion ESA data) 

(All qualities data) ESA Reduced (Low Angular Res., 3-s Time Res.) Mode, Ion Density

Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA)(all qualities)

Ion Symmetry Vector (direction of pressure tensor symmetry (DSL))(all qualities) 

Magnetic Field Vector in DSL (Same time array as Reduced Ion ESA data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Reduced Ion ESA data)

ESA Reduced Mode, Electron Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/esa_flag.shtml.) 

ESA Reduced (Low Angular Res., 3-s Time Res.) Mode, Electron Density

(Good data only) ESA Reduced (Low Angular Res., 3-s Time Res.) Mode, Electron Density

-----SC Potential (Same time array as Reduced Electron ESA data) 

Magnetic Field Vector in DSL (Same time array as Reduced Electron ESA data)

-----Magnetic Field Vector in DSL (Same time array as Reduced Electron ESA data) 

ESA Reduced (Low Angular Res., 3-s Time Res.) Mode, Electron Density(all qualities)

(All qualities data) ESA Reduced (Low Angular Res., 3-s Time Res.) Mode, Electron Density

-----SC Potential (Same time array as Reduced Electron ESA data)

Magnetic Field Vector in DSL (Same time array as Reduced Electron ESA data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Reduced Electron ESA data)

ESA Burst Mode, Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/esa_flag.shtml.) 

(Good data only) ESA Burst (High Time and Angular Resolution) Mode, Ion Density

-----Ion Symmetry Vector (direction of pressure tensor symmetry (DSL))  

Magnetic Field Vector in DSL (Same time array as Burst Ion ESA data)

-----Magnetic Field Vector in DSL (Same time array as Burst Ion ESA data) 

(All qualities data) ESA Burst (High Time and Angular Resolution) Mode, Ion Density

Magnetic Field Vector in DSL (Same time array as Burst Ion ESA data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Burst Ion ESA data)

ESA Burst Mode, Electron Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/esa_flag.shtml.) 

(Good data only) ESA Burst (High Time and Angular Resolution) Mode, Electron Density

-----Electron Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA)  

Magnetic Field Vector in DSL (Same time array as Burst Electron ESA data)

-----Magnetic Field Vector in DSL (Same time array as Burst Electron ESA data) 

(All qualities data) ESA Burst (High Time and Angular Resolution) Mode, Electron Density

Electron Symmetry Vector (direction of pressure tensor symmetry (DSL))(all qualities)

Magnetic Field Vector in DSL (Same time array as Burst Electron ESA data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Burst Electron ESA data)

ESA electron solar wind mode flag; 0: Not in Solar Wind mode, 1: in Solar Wind mode

ESA ion solar wind mode flag; 0: Not in Solar Wind mode, 1: in Solar Wind mode

Probe Electric Field Instrument and Search Coil Magnetometer Instrument, Digital Fields Board- digitally computed Filter Bank spectra and E12 peak and average in HF band.

Sensor and electronics design provided by UCB (J. W. Bonnell, F. S. Mozer), Digital Fields Board provided by LASP (R. Ergun), Search coil data provided by CETP (A. Roux).

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, J. W. Bonnell & F. S. Mozer; A. Roux and R. E. Ergun at UCB; CETP and LASP respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, J. W. Bonnell & F. S. Mozer; A. Roux and R. E. Ergun at UCB; CETP and LASP respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, J. W. Bonnell & F. S. Mozer; A. Roux and R. E. Ergun at UCB; CETP and LASP respectively, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fb_hff_epoch, @1 => tha_fb_v1_epoch, @2 => tha_fb_v2_epoch, @3 => tha_fb_v3_epoch, @4 => tha_fb_v4_epoch, @5 => tha_fb_v5_epoch, @6 => tha_fb_v6_epoch, @7 => tha_fb_edc12_epoch, @8 => tha_fb_edc34_epoch, @9 => tha_fb_edc56_epoch, @10 => tha_fb_scm1_epoch, @11 => tha_fb_scm2_epoch, @12 => tha_fb_scm3_epoch, @13 => tha_fb_eac12_epoch, @14 => tha_fb_eac34_epoch, @15 => tha_fb_eac56_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fb_hff_epoch, @1 => tha_fb_v1_epoch, @2 => tha_fb_v2_epoch, @3 => tha_fb_v3_epoch, @4 => tha_fb_v4_epoch, @5 => tha_fb_v5_epoch, @6 => tha_fb_v6_epoch, @7 => tha_fb_edc12_epoch, @8 => tha_fb_edc34_epoch, @9 => tha_fb_edc56_epoch, @10 => tha_fb_scm1_epoch, @11 => tha_fb_scm2_epoch, @12 => tha_fb_scm3_epoch, @13 => tha_fb_eac12_epoch, @14 => tha_fb_eac34_epoch, @15 => tha_fb_eac56_epoch.)

Filter BanK and HF data (from Master/CDFglobalAttributes/Data_type)

THEMIS-A:  On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field, for particle and wave burst survey modes.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fff_16_epoch, @1 => tha_fff_64_epoch, @2 => tha_ffp_16_epoch, @3 => tha_ffp_32_epoch, @4 => tha_ffp_64_epoch, @5 => tha_ffw_16_epoch, @6 => tha_ffw_32_epoch, @7 => tha_ffw_64_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fff_16_epoch, @1 => tha_fff_64_epoch, @2 => tha_ffp_16_epoch, @3 => tha_ffp_32_epoch, @4 => tha_ffp_64_epoch, @5 => tha_ffw_16_epoch, @6 => tha_ffw_32_epoch, @7 => tha_ffw_64_epoch.)

FFT Power Spectrum in Fast Survey, 16 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Fast Survey, 16 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Fast Survey, 16 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Fast Survey, 16 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Fast Survey, 16 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Fast Survey, 16 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Fast Survey, 16 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Fast Survey, 16 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI E (perp to B)

FFT Power Spectrum in Fast Survey, 16 frequencies for SCM, Axis 1

FFT Power Spectrum in Fast Survey, 16 frequencies for SCM, Axis 2

FFT Power Spectrum in Fast Survey, 16 frequencies for SCM, Axis 3

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Fast Survey, 16 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Fast Survey, 64 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Fast Survey, 64 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Fast Survey, 64 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Fast Survey, 64 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Fast Survey, 64 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Fast Survey, 64 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Fast Survey, 64 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Fast Survey, 64 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI E (perp to B)

FFT Power Spectrum in Fast Survey, 64 frequencies for SCM, Axis 1

FFT Power Spectrum in Fast Survey, 64 frequencies for SCM, Axis 2

FFT Power Spectrum in Fast Survey, 64 frequencies for SCM, Axis 3

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Fast Survey, 64 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Particle Burst, 16 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Particle Burst, 16 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Particle Burst, 16 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Particle Burst, 16 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Particle Burst, 16 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Particle Burst, 16 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Particle Burst, 16 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Particle Burst, 16 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI E (perp to B)

FFT Power Spectrum in Particle Burst, 16 frequencies for SCM, Axis 1

FFT Power Spectrum in Particle Burst, 16 frequencies for SCM, Axis 2

FFT Power Spectrum in Particle Burst, 16 frequencies for SCM, Axis 3

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Particle Burst, 16 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI E (perp to B)

FFT Power Spectrum in Particle Burst, 32 frequencies for SCM, Axis 1

FFT Power Spectrum in Particle Burst, 32 frequencies for SCM, Axis 2

FFT Power Spectrum in Particle Burst, 32 frequencies for SCM, Axis 3

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Particle Burst, 32 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Particle Burst, 64 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Particle Burst, 64 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Particle Burst, 64 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Particle Burst, 64 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Particle Burst, 64 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Particle Burst, 64 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Particle Burst, 64 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Particle Burst, 64 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI E (perp to B)

FFT Power Spectrum in Particle Burst, 64 frequencies for SCM, Axis 1

FFT Power Spectrum in Particle Burst, 64 frequencies for SCM, Axis 2

FFT Power Spectrum in Particle Burst, 64 frequencies for SCM, Axis 3

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Particle Burst, 64 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Wave Burst, 16 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Wave Burst, 16 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Wave Burst, 16 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Wave Burst, 16 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Wave Burst, 16 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Wave Burst, 16 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Wave Burst, 16 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Wave Burst, 16 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI E (perp to B)

FFT Power Spectrum in Wave Burst, 16 frequencies for SCM, Axis 1

FFT Power Spectrum in Wave Burst, 16 frequencies for SCM, Axis 2

FFT Power Spectrum in Wave Burst, 16 frequencies for SCM, Axis 3

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Wave Burst, 16 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Wave Burst, 32 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Wave Burst, 32 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Wave Burst, 32 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Wave Burst, 32 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Wave Burst, 32 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Wave Burst, 32 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Wave Burst, 32 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Wave Burst, 32 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI E (perp to B)

FFT Power Spectrum in Wave Burst, 32 frequencies for SCM, Axis 1

FFT Power Spectrum in Wave Burst, 32 frequencies for SCM, Axis 2

FFT Power Spectrum in Wave Burst, 32 frequencies for SCM, Axis 3

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Wave Burst, 32 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Wave Burst, 64 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Wave Burst, 64 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Wave Burst, 64 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Wave Burst, 64 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Wave Burst, 64 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Wave Burst, 64 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Wave Burst, 64 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Wave Burst, 64 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI E (perp to B)

FFT Power Spectrum in Wave Burst, 64 frequencies for SCM, Axis 1

FFT Power Spectrum in Wave Burst, 64 frequencies for SCM, Axis 2

FFT Power Spectrum in Wave Burst, 64 frequencies for SCM, Axis 3

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Wave Burst, 64 frequencies for EFI Potential, Sensor 6

Spacecraft-collected fluxgate magnetometer, Decimated TeleMetry High, DSL, GSE and GSM coordinates

Sensor and electronics design provided by TUBS (Glassmeier, Auster) and IWF (Baumjohann, Magnes)

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, U. Auster & K.H. Glassmeier and W. Baumjohann at UCB, TUBS and IWF respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, U. Auster & K.H. Glassmeier and W. Baumjohann at UCB, TUBS and IWF respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, U. Auster & K.H. Glassmeier and W. Baumjohann at UCB, TUBS and IWF respectively, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fgs_epoch, @1 => tha_fgl_epoch16, @2 => tha_fgh_epoch16, @3 => tha_fge_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fgs_epoch, @1 => tha_fgl_epoch16, @2 => tha_fgh_epoch16, @3 => tha_fge_epoch16.)

FGM-FGS Data Quality (0: Good data, 1:boom not deployed, 2:in shadow, 3:uncorrected shadow, 4:noisy waveforms)

---- FGS (spin-resolution/~3 sec) magnetic  field B in XYZ GSE Coordinates

---- FGS (spin-resolution/~3 sec) magnetic  field B in XYZ GSM Coordinates

---- FGS magnetic field B in DSL (Despun Spacecraft) Coordinates 

---- FGS magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates 

FGM-FGL Data Quality (0: Good data, 1:boom not deployed, 2:in shadow, 3:uncorrected shadow, 4:noisy waveforms)

---- FGL (low-resolution/~0.25 sec) magnetic field B in XYZ GSE Coordinates

---- FGL (low-resolution/~0.25 sec) magnetic field B in XYZ GSM Coordinates

---- FGL magnetic field B in DSL (Despun Spacecraft) Coordinates 

---- FGL magnetic field B in SSL (Spinning Spacecraft) Coordinates 

---- FGL (low-resolution/~0.25 sec) field B in XYZ GSE Coordinates

---- FGL magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates 

---- FGL magnetic field B in XYZ SSL (Spinning Spacecraft) Coordinates

FGM-FGH Data Quality (0: Good data, 1:boom not deployed, 2:in shadow, 3:uncorrected shadow, 4:noisy waveforms)

---- FGH (high-resolution/~0.008 sec) magnetic field B in XYZ GSE Coordinates

---- FGH (high-resolution/~0.008 sec) magnetic field B in XYZ GSM Coordinates

---- FGH magnetic field B in DSL (Despun Spacecraft) Coordinates 

---- FGH magnetic field B in SSL (Spinning Spacecraft) Coordinates 

---- FGH magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates

----FGH magnetic field B in XYZ SSL (Spinning Spacecraft) Coordinates

FGM-FGE Data Quality (0: Good data, 1:boom not deployed, 2:in shadow, 3:uncorrected shadow, 4:noisy waveforms)

---- FGE (engineering mode) magnetic field B in XYZ GSE Coordinates

---- FGE (engineering mode) magnetic field B in XYZ GSM Coordinates

---- FGE magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates 

---- FGE magnetic field B in XYZ SSL (Spinning Spacecraft) Coordinates 

THEMIS-A:  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fgs_epoch, @1 => tha_efs_epoch, @2 => tha_fit_bfit_epoch, @3 => tha_fit_efit_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_fgs_epoch, @1 => tha_efs_epoch, @2 => tha_fit_bfit_epoch, @3 => tha_fit_efit_epoch.)

FGS (spin-fit) magnetic field vector in XYZ despun spacecraft coordinates (DSL)

Standard Deviation of onboard EFS (spin-fit) electric field spin-fit

EFS (spin-fit) electric field vector in XYZ despun spacecraft coordinates (DSL)

EFS_0 (spin-fit, using E_z=0) electric field E in XYZ despun spacecraft coordinates (DSL)

EFS_0 (spin-fit, using E_z=0) electric field E in GSE coordinates 

EFS_0 (spin-fit, using E_z=0) electric field E in GSM coordinates 

THEMIS-A:  Solid State Telescope (ESA+SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (ions: 5 eV - 4 MeV,electrons: 6 eV - 700 keV)

THEMIS-A:  Solid State Telescope (SST) & Electrostatic Analyzer (ESA): ground calculatedenergy fluxes & moments.(density, velocity, pressure, and temperature) Generated from ESA+SST combined distributions

Detailed Description of the Solid State Telescope (SST) Instrument

Detailed Description of the Electrostatic Analyzer (ESA) Instrument

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, D. Larson & R.P. Lin, C.W. Carlson & J. McFadden at UCB, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, D. Larson & R.P. Lin, C.W. Carlson & J. McFadden at UCB, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, D. Larson & R.P. Lin, C.W. Carlson & J. McFadden at UCB, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_ptiff_epoch, @1 => tha_pteff_epoch, @2 => tha_ptirf_epoch, @3 => tha_pterf_epoch, @4 => tha_ptibb_epoch, @5 => tha_ptebb_epoch, @6 => tha_eesa_solarwind_flag_epoch, @7 => tha_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_ptiff_epoch, @1 => tha_pteff_epoch, @2 => tha_ptirf_epoch, @3 => tha_pterf_epoch, @4 => tha_ptibb_epoch, @5 => tha_ptebb_epoch, @6 => tha_eesa_solarwind_flag_epoch, @7 => tha_iesa_solarwind_flag_epoch.)

ESA+SST Full+Full Mode Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/gmom_flag.shtml.) 

-----SC Potential (Same time array as Full Ion ESA-SST data) (Good Data Only)

Ion Diagonalized Temperature (Tprp1, Tprp2, Tpar)(Good Data Only)

-----Ion Diagonalized Temperature (Tprp1, Tprp2, Tpar)(Good Data Only)

Temperature, Field Aligned (TprpFA1, TprpFA2, TparFA)(Good Data Only)

-----Temperature, Field Aligned (TprpFA1, TprpFA2, TparFA) (Good Data Only)

Ion Symmetry Vector (direction of pressure tensor symmetry (DSL))(Good Data Only)

-----Ion Symmetry Vector (direction of pressure tensor symmetry (DSL)) (Good Data Only)

-----Ion Symmetry Angle (between symmetry direction and B)(Good Data Only)

Magnetic Field Vector in DSL (Same time array as Full Ion ESA-SST data)(Good Data Only)

-----Magnetic Field Vector in DSL (Same time array as Full Ion ESA-SST data) (Good Data Only)

Magnetic Field Vector in DSL (Same time array as Full Ion ESA-SST data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Full Ion ESA-SST data)

ESA+SST Full+Full Mode Elec Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/gmom_flag.shtml.) 

-----SC Potential (Same time array as Full Elec ESA-SST data) (Good Data Only)

Elec Diagonalized Temperature (Tprp1, Tprp2, Tpar)(Good Data Only)

-----Elec Diagonalized Temperature (Tprp1, Tprp2, Tpar)(Good Data Only)

Elec Symmetry Vector (direction of pressure tensor symmetry (DSL))(Good Data Only)

-----Elec Symmetry Vector (direction of pressure tensor symmetry (DSL)) (Good Data Only)

-----Elec Symmetry Angle (between symmetry direction and B)(Good Data Only)

Magnetic Field Vector in DSL (Same time array as Full Elec ESA-SST data)(Good Data Only)

-----Magnetic Field Vector in DSL (Same time array as Full Elec ESA-SST data) (Good Data Only)

(All qualities data) ESA-SST Full (High Angular Resolution, few minute time res.) Mode, Electron Density

-----SC Potential (Same time array as Full Electron ESA-SST data)

Magnetic Field Vector in DSL (Same time array as Full Electron ESA-SST data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Full Electron ESA-SST data)

ESA+SST Reduced+Full Mode Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/gmom_flag.shtml.) 

(Good Data Only) ESA Reduced (Low Angular Res., 3-s Time Res.) SST Full(High Angular Res, Variable Time Res) Mode, Ion Density

-----SC Potential (Same time array as Reduced-Full Ion ESA-SST data) (Good Data Only)

Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA)(Good Data Only)

-----Temperature, Field Aligned (Tprp1FA, Tprp2FA, TparFA)(Good Data Only)

Ion Symmetry Vector (direction of pressure tensor symmetry (DSL)) (Good Data Only)

-----Ion Symmetry Vector (direction of pressure tensor symmetry (DSL))(Good Data Only) 

Magnetic Field Vector in DSL (Same time array as Reduced-Full Ion ESA-SST data)(Good Data Only)

-----Magnetic Field Vector in DSL (Same time array as Reduced-Full Ion ESA-SST data)(Good Data Only)

(All qualities data) ESA Reduced (Low Angular Res., 3-s Time Res.) SST Full(High Angular Res, Variable Time Res) Mode, Ion Density

-----SC Potential (Same time array as Reduced-Full Ion ESA-SST data)

Magnetic Field Vector in DSL (Same time array as Reduced-Full Ion ESA-SST data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Reduced-Full Ion ESA-SST data)

ESA+SST Reduced+Full Mode Elec Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/gmom_flag.shtml.) 

(Good Data Only) ESA Reduced (Low Angular Res., 3-s Time Res.) SST Full(High Angular Res, Variable Time Res) Mode, Elec Density

-----SC Potential (Same time array as Reduced-Full Elec ESA-SST data) (Good Data Only)

Elec Symmetry Vector (direction of pressure tensor symmetry (DSL)) (Good Data Only)

-----Elec Symmetry Vector (direction of pressure tensor symmetry (DSL))(Good Data Only) 

Magnetic Field Vector in DSL (Same time array as Reduced-Full Elec ESA-SST data)(Good Data Only)

-----Magnetic Field Vector in DSL (Same time array as Reduced-Full Elec ESA-SST data)(Good Data Only)

(All qualities data) ESA Reduced (Low Angular Res., 3-s Time Res.) SST Full(High Angular Res, Variable Time Res) Mode, Electron Density

-----SC Potential (Same time array as Reduced-Full Electron ESA-SST data)

Magnetic Field Vector in DSL (Same time array as Reduced-Full Electron ESA-SST data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Reduced-Full Electron ESA-SST data)

ESA+SST Burst+Burst Mode Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/gmom_flag.shtml.) 

(Good Data Only) ESA-SST Burst (High Time and Angular Resolution) Mode, Ion Density

-----SC Potential (Same time array as Burst Ion ESA-SST data)(Good Data Only)

Magnetic Field Vector in DSL (Same time array as Burst Ion ESA-SST data) (Good Data Only)

-----Magnetic Field Vector in DSL (Same time array as Burst Ion ESA-SST data)(Good Data Only)

(All qualities data) ESA-SST Burst (High Time and Angular Resolution) Mode, Ion Density

Magnetic Field Vector in DSL (Same time array as Burst Ion ESA-SST data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Burst Ion ESA-SST data)

ESA+SST Burst+Burst Mode Elec Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/gmom_flag.shtml.) 

(Good Data Only) ESA-SST Burst (High Time and Angular Resolution) Mode, Elec Density

-----SC Potential (Same time array as Burst Elec ESA-SST data)(Good Data Only)

Magnetic Field Vector in DSL (Same time array as Burst Elec ESA-SST data) (Good Data Only)

-----Magnetic Field Vector in DSL (Same time array as Burst Elec ESA-SST data)(Good Data Only)

(All qualities data) ESA-SST Burst (High Time and Angular Resolution) Mode, Electron Density

-----SC Potential (Same time array as Burst Electron ESA-SST data)

Magnetic Field Vector in DSL (Same time array as Burst Electron ESA-SST data)(all qualities)

-----Magnetic Field Vector in DSL (Same time array as Burst Electron ESA-SST data)

ESA-SST electron solar wind mode flag; 0: Not in Solar Wind mode, 1: in Solar Wind mode

ESA-SST ion solar wind mode flag; 0: Not in Solar Wind mode, 1: in Solar Wind mode

THEMIS-A (P5):  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.

THEMIS-A:  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_peim_epoch, @1 => tha_peem_epoch, @2 => tha_pxxm_epoch, @3 => tha_eesa_solarwind_flag_epoch, @4 => tha_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_peim_epoch, @1 => tha_peem_epoch, @2 => tha_pxxm_epoch, @3 => tha_eesa_solarwind_flag_epoch, @4 => tha_iesa_solarwind_flag_epoch.)

Ion Moment Data Quality (0: good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/mom_flag.shtml.) 

(Good data only) ESA On Board Moment (MOM) Ion Density, THEMIS-A

-----Magnetic Field Vector DSL (Same time array as MOM Ion ESA data)

(All qualities data) ESA On Board Moment (MOM) Ion Density, THEMIS-A

Electron Moment Data Quality (0: good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/mom_flag.shtml.) 

(Good data only) ESA On Board Moment (MOM) Electron Density, THEMIS-A

-----Magnetic Field Vector DSL (Same time array as MOM Electron ESA data)

-----Electron Temperature, Field Aligned (TprpFA1, TprpFA2, TparFA)

(All Qualities data) ESA On Board Moment (MOM) Electron Density, THEMIS-A

Spacecraft-collected search-coil magnetometer (SCM) Magnetic field

THEMIS-A: Search Coil Magnetometer (SCM) Magnetic Field Measurements. Includes FAST SURVEY, PARTICLE BURST and WAVE BURST data. FAST SURVEY (SCF): 1/8 second time resolution. PARTICLE BURST (SCP): 1/128 second time resolution; only short bursts of data. WAVE BURST (SCW): 1/8192 second time resolution; only short bursts of data. Sensor and electronics design provided by LPP, Roux and Le Contel

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, A. Roux and O. LeContel at UCB, LPP NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, A. Roux and O. LeContel at UCB, LPP NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, A. Roux and O. LeContel at UCB, LPP NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_scf_epoch, @1 => tha_scp_epoch16, @2 => tha_scw_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_scf_epoch, @1 => tha_scp_epoch16, @2 => tha_scw_epoch16.)

tha_scf_epoch: Search Coil Fast-survey (SCF, 1/8 sec time resolution) epoch variable

SCF (fast-survey, 1/8 sec time resolution) SCM magnetic field B magnitude 

SCF (fast-survey, 1/8 sec time resolution) SCM magnetic field B in XYZ GSE Coordinates

SCF (fast-survey, 1/8 sec time resolution) SCM magnetic field B in XYZ GSM Coordinates

SCF (fast-survey, 1/8 sec time resolution) SCM magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates 

tha_scp_epoch16: Search Coil Particle-burst (SCP, 1/128 sec time resolution) epoch variable

SCP (particle burst, 1/128 second time resolution) SCM magnetic field B magnitude 

SCP (particle burst, 1/128 second time resolution) SCM magnetic field B in XYZ GSE Coordinates

SCP (particle burst, 1/128 second time resolution) SCM magnetic field B in XYZ GSM Coordinates

SCP (particle burst, 1/128 second time resolution) SCM magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates 

tha_scw_epoch16: Search Coil Wave-burst (SCW, 1/8192 sec time resolution) epoch variable

SCW (wave burst, 1/8192 second time resolution) SCM magnetic field B magnitude 

SCW (wave burst, 1/8192 second time resolution) SCM magnetic field B in XYZ GSE Coordinates

SCW (wave burst, 1/8192 second time resolution) SCM magnetic field B in XYZ GSM Coordinates

SCW (wave burst, 1/8192 second time resolution) SCM magnetic field B in XYZ DSL (Despun Spacecraft) Coordinates

THEMIS-A:  Solid State Telescope (SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (30 keV - 300 keV).

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, D. Larson & R.P. Lin at UCB, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, D. Larson & R.P. Lin at UCB, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, D. Larson & R.P. Lin at UCB, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_psif_epoch, @1 => tha_psef_epoch, @2 => tha_psib_epoch, @3 => tha_pseb_epoch, @4 => tha_eesa_solarwind_flag_epoch, @5 => tha_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => tha_psif_epoch, @1 => tha_psef_epoch, @2 => tha_psib_epoch, @3 => tha_pseb_epoch, @4 => tha_eesa_solarwind_flag_epoch, @5 => tha_iesa_solarwind_flag_epoch.)

SST Full Mode Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/sst_flag.shtml.) 

SST full mode derived average ion thermal velocity(Good data only)

Spacecraft potential used in generation of tha_psif moments(Good data only)

Ion Diagonalized Temperature(Tprp1, Tprp2, Tpar)(Good data only)

SST full mode ion diagonalized temperature (Tprp1, Tprp2, Tpar)(Good data only)

Ion Temperature, Field Aligned(Tprp1FA, Tprp2FA, TparFA)(Good data only)

SST full mode ion temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(Good data only)

SST full distribution derived ion pressure tensor(Good data only)

SST full distribution derived ion momentum flux tensor(Good data only)

SST full mode ion direction of pressure tensor symmetry. In DSL Coordinates(Good data only)

SST full distribution derived ion symmetry angle (Angle between Symmetry Direction and Magnetic Field(B))(Good data only)

Magnetic field vector used for generation of psif moments in DSL coordinates(Good data only)

SST full distribution derived ion velocity vector in DSL coordinates(Good data only)

SST full distribution derived ion velocity vector in GSE coordinates(Good data only)

SST full distribution derived ion velocity vector in GSM coordinates(Good data only)

SST full mode derived average ion thermal velocity(All qualities)

Spacecraft potential used in generation of tha_psif moments(All qualities)

SST full mode ion diagonalized temperature (Tprp1, Tprp2, Tpar)(All qualities)

Ion Temperature, Field Aligned(Tprp1FA, Tprp2FA, TparFA)(All qualities

SST full mode ion temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(All qualities)

SST full distribution derived ion pressure tensor(All qualities)

SST full distribution derived ion momentum flux tensor(All qualities)

SST full mode ion direction of pressure tensor symmetry. In DSL Coordinates(All qualities)

SST full distribution derived ion symmetry angle (Angle between Symmetry Direction and Magnetic Field(B)). (All qualities)

Magnetic field vector used for generation of psif moments in DSL coordinates(All qualities)

SST full distribution derived ion velocity vector in DSL coordinates. (All qualities)

SST full distribution derived ion velocity vector in GSE coordinates(All qualities)

SST full distribution derived ion velocity vector in GSM coordinates(All qualities)

SST Full Mode Electron Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/sst_flag.shtml.) 

SST full mode derived average electron temperature(Good data only)

SST full mode derived average electron thermal velocity(Good data only)

Spacecraft potential used in generation of tha_psef moments(Good data only)

Electron Diagonalized Temperature(Tprp1, Tprp2, Tpar)(Good data only)

SST full mode electron diagonalized temperature (Tprp1, Tprp2, Tpar)(Good data only)

Electron Temperature, Field Aligned(Tprp1FA, Tprp2FA, TparFA) (Good data only)

SST full mode electron temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(Good data only)

SST full distribution derived electron pressure tensor(Good data only)

SST full distribution derived electron momentum flux tensor(Good data only)

SST full mode electron direction of pressure tensor symmetry. In DSL Coordinates(Good data only)

SST full distribution derived electron symmetry angle (Angle between Symmetry Direction and Magnetic Field(B))(Good data only)

Magnetic field vector used for generation of psef moments in DSL coordinates(Good data only)

SST full distribution derived electron velocity vector in DSL coordinates(Good data only)

SST full distribution derived electron velocity vector in GSE coordinates(Good data only)

SST full distribution derived electron velocity vector in GSM coordinates(Good data only)

SST full mode derived average electron temperature(All qualities)

SST full mode derived average electron thermal velocity(All qualities)

Spacecraft potential used in generation of tha_psef moments(All qualities)

Electron Diagonalized Temperature(Tprp1, Tprp2, Tpar)(All qualities)

SST full mode electron diagonalized temperature (Tprp1, Tprp2, Tpar)(All qualities)

Electron Temperature, Field Aligned(Tprp1FA, Tprp2FA, TparFA)(All qualities

SST full mode electron temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(All qualities)

SST full distribution derived electron pressure tensor(All qualities)

SST full distribution derived electron momentum flux tensor(All qualities)

SST full mode electron direction of pressure tensor symmetry. In DSL Coordinates(All qualities)

SST full distribution derived electron symmetry angle (Angle between Symmetry Direction and Magnetic Field(B))(All qualities)

Magnetic field vector used for generation of psef moments in DSL coordinates(All Qualities)

SST full distribution derived electron velocity vector in DSL coordinates(All Qualities)

SST full distribution derived electron velocity vector in GSE coordinates(All Qualities)

SST full distribution derived electron velocity vector in GSM coordinates(All Qualities)

SST Burst Mode Ion Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/sst_flag.shtml.) 

SST burst mode derived average ion thermal velocity(Good data only)

Spacecraft potential used in generation of tha_psib moments(Good data only)

SST burst mode ion diagonalized temperature (Tprp1, Tprp2, Tpar)(Good data only)

SST burst mode ion temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(Good data only)

SST burst distribution derived ion pressure tensor(Good data only)

SST burst distribution derived ion momentum flux tensor(Good data only)

SST burst mode ion direction of pressure tensor symmetry. In DSL Coordinates(Good data only)

SST burst distribution derived ion symmetry angle (Angle between Symmetry Direction and Magnetic Field(B))(Good data only)

Magnetic field vector used for generation of psib moments in DSL coordinates(Good data only)

SST burst distribution derived ion velocity vector in DSL coordinates(Good data only)

SST burst distribution derived ion velocity vector in GSE coordinates(Good data only)

SST burst distribution derived ion velocity vector in GSM coordinates(Good data only)

SST burst mode derived average ion thermal velocity(All qualities)

Spacecraft potential used in generation of tha_psib moments(All qualities)

SST burst mode ion diagonalized temperature (Tprp1, Tprp2, Tpar)(All qualities)

SST burst mode ion temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(All qualities)

SST burst distribution derived ion pressure tensor(All qualities)

SST burst distribution derived ion momentum flux tensor(All qualities)

SST burst mode ion direction of pressure tensor symmetry. In DSL Coordinates(All qualities)

SST burst distribution derived ion symmetry angle (Angle between Symmetry Direction and Magnetic Field(B)). (All qualities)

Magnetic field vector used for generation of psib moments in DSL coordinates(All qualities)

SST burst distribution derived ion velocity vector in DSL coordinates. (All qualities)

SST burst distribution derived ion velocity vector in GSE coordinates(All qualities)

SST burst distribution derived ion velocity vector in GSM coordinates(All qualities)

SST Burst Mode Electron Moment Data Quality (0: Good data, non-zero: Data may not be suitable, see: http://themis.ssl.berkeley.edu/sst_flag.shtml.) 

SST burst mode derived average electron temperature(Good data only)

SST burst mode derived average electron thermal velocity(Good data only)

Spacecraft potential used in generation of tha_pseb moments(Good data only)

SST burst mode electron diagonalized temperature (Tprp1, Tprp2, Tpar)(Good data only)

SST burst mode electron temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(Good data only)

SST burst distribution derived electron pressure tensor(Good data only)

SST burst distribution derived electron momentum flux tensor(Good data only)

SST burst mode electron direction of pressure tensor symmetry. In DSL Coordinates(Good data only)

SST burst distribution derived electron symmetry angle (Angle between Symmetry Direction and Magnetic Field(B))(Good data only)

Magnetic field vector used for generation of pseb moments in DSL coordinates(Good data only)

SST burst distribution derived electron velocity vector in DSL coordinates(Good data only)

SST burst distribution derived electron velocity vector in GSE coordinates(Good data only)

SST burst distribution derived electron velocity vector in GSM coordinates(Good data only)

SST burst mode derived average electron temperature(All qualities)

SST burst mode derived average electron thermal velocity(All qualities)

Spacecraft potential used in generation of tha_pseb moments(All qualities)

SST burst mode electron diagonalized temperature (Tprp1, Tprp2, Tpar)(All qualities)

SST burst mode electron temperature temperature magnetic field aligned. (Tprp1FA, Tprp2FA, TparFA)(All qualities)

SST burst distribution derived electron pressure tensor(All qualities)

SST burst distribution derived electron momentum flux tensor(All qualities)

SST burst mode electron direction of pressure tensor symmetry. In DSL Coordinates(All qualities)

SST burst distribution derived electron symmetry angle (Angle between Symmetry Direction and Magnetic Field(B))(All qualities)

Magnetic field vector used for generation of pseb moments in DSL coordinates(All Qualities)

SST burst distribution derived electron velocity vector in DSL coordinates(All Qualities)

SST burst distribution derived electron velocity vector in GSE coordinates(All Qualities)

SST burst distribution derived electron velocity vector in GSM coordinates(All Qualities)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/tha/ssc/2007/tha_or_ssc_20070217_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 15826 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thb/ssc_pre/2008/thbpred_or_ssc_20080101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 240450 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thb/helio1day/thb_helio1day_position_20070219_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 6491 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thb/helio1hr/thb_helio1hr_position_20070219_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 159671 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_state_epoch, @1 => thb_spin_epoch, @2 => thb_spin_ecl_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_state_epoch, @1 => thb_spin_epoch, @2 => thb_spin_ecl_epoch.)

THEMIS-B: Electric Field Instrument (EFI) Electric field measurements. The L2 product is a 3D estimate of Eperp derived from the spin plane E-field measurements assuming E dot B = 0, using relevant FGM (Flux-Gate Magnetometer) data.Includes spin-averaged, and Fast-survey field data.Spin-averaged (EFS_DOT0) data has approximately 3 second time resolution. Fast-survey (EFF_DOT0) data has 1/8 second time resolution.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_efs_dot0_epoch, @1 => thb_eff_dot0_epoch, @2 => thb_eff_q_mag_epoch, @3 => thb_eff_q_pha_epoch, @4 => thb_eff_e12_efs_epoch, @5 => thb_eff_e34_efs_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_efs_dot0_epoch, @1 => thb_eff_dot0_epoch, @2 => thb_eff_q_mag_epoch, @3 => thb_eff_q_pha_epoch, @4 => thb_eff_e12_efs_epoch, @5 => thb_eff_e34_efs_epoch.)

thb_efs_dot0_epoch: Electric field Instrument Spin-fit (EFS_DOT0, approx. 3 sec time resolution) epoch variable

thb_eff_dot0_epoch: Electric field Instrument Fast-survey (EFF_DOT0, 1/8 sec time resolution) epoch variable

thb_eff_q_mag_epoch: Electric field Instrument Spin-averaged (EFF_Q_MAG, approx. 3 sec time resolution) epoch variable

thb_eff_q_pha_epoch: Electric field Instrument Spin-averaged (EFF_Q_PHA, approx. 3 sec time resolution) epoch variable

thb_eff_e12_efs_epoch: Electric field Instrument Spin-averaged (EFF_E12_EFS, approx. 3 sec time resolution) epoch variable

thb_eff_e34_efs_epoch: Electric field Instrument Spin-averaged (EFF_E34_EFS, approx. 3 sec time resolution) epoch variable

THEMIS-B: Electric Field Instrument Particle Burst Mode (EFP) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/128 to 1/512 second time resolution.

thb_efp_epoch: Electric field Instrument Fast-survey (EFP, 1/8 sec time resolution) epoch variable

THEMIS-B: Electric Field Instrument Wave Burst Mode (EFW) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/16384 second time resolution.

thb_efw_epoch: Electric field Instrument Fast-survey (EFW, 1/8 sec time resolution) epoch variable

THEMIS-B (P1/ARTEMIS-P1): Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution.

THEMIS-B: Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 2: Counter saturation, 4: Solar Wind not in Solar Wind Mode, or Solar Wind Mode, not in Solar Wind, 8: (Reduced Mode only) slow survey mode+flows, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_peif_epoch, @1 => thb_peef_epoch, @2 => thb_peir_epoch, @3 => thb_peer_epoch, @4 => thb_peib_epoch, @5 => thb_peeb_epoch, @6 => thb_eesa_solarwind_flag_epoch, @7 => thb_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_peif_epoch, @1 => thb_peef_epoch, @2 => thb_peir_epoch, @3 => thb_peer_epoch, @4 => thb_peib_epoch, @5 => thb_peeb_epoch, @6 => thb_eesa_solarwind_flag_epoch, @7 => thb_iesa_solarwind_flag_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fb_hff_epoch, @1 => thb_fb_v1_epoch, @2 => thb_fb_v2_epoch, @3 => thb_fb_v3_epoch, @4 => thb_fb_v4_epoch, @5 => thb_fb_v5_epoch, @6 => thb_fb_v6_epoch, @7 => thb_fb_edc12_epoch, @8 => thb_fb_edc34_epoch, @9 => thb_fb_edc56_epoch, @10 => thb_fb_scm1_epoch, @11 => thb_fb_scm2_epoch, @12 => thb_fb_scm3_epoch, @13 => thb_fb_eac12_epoch, @14 => thb_fb_eac34_epoch, @15 => thb_fb_eac56_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fb_hff_epoch, @1 => thb_fb_v1_epoch, @2 => thb_fb_v2_epoch, @3 => thb_fb_v3_epoch, @4 => thb_fb_v4_epoch, @5 => thb_fb_v5_epoch, @6 => thb_fb_v6_epoch, @7 => thb_fb_edc12_epoch, @8 => thb_fb_edc34_epoch, @9 => thb_fb_edc56_epoch, @10 => thb_fb_scm1_epoch, @11 => thb_fb_scm2_epoch, @12 => thb_fb_scm3_epoch, @13 => thb_fb_eac12_epoch, @14 => thb_fb_eac34_epoch, @15 => thb_fb_eac56_epoch.)

THEMIS-B:  On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field, for particle and wave burst survey modes.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fff_16_epoch, @1 => thb_fff_32_epoch, @2 => thb_fff_64_epoch, @3 => thb_ffp_16_epoch, @4 => thb_ffp_32_epoch, @5 => thb_ffp_64_epoch, @6 => thb_ffw_16_epoch, @7 => thb_ffw_32_epoch, @8 => thb_ffw_64_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fff_16_epoch, @1 => thb_fff_32_epoch, @2 => thb_fff_64_epoch, @3 => thb_ffp_16_epoch, @4 => thb_ffp_32_epoch, @5 => thb_ffp_64_epoch, @6 => thb_ffw_16_epoch, @7 => thb_ffw_32_epoch, @8 => thb_ffw_64_epoch.)

FFT Power Spectrum in Fast Survey, 32 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Fast Survey, 32 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Fast Survey, 32 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Fast Survey, 32 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Fast Survey, 32 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Fast Survey, 32 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Fast Survey, 32 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Fast Survey, 32 frequencies for E Field DC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI E (parallel to B)

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI E (perp to B)

FFT Power Spectrum in Fast Survey, 32 frequencies for SCM, Axis 1

FFT Power Spectrum in Fast Survey, 32 frequencies for SCM, Axis 2

FFT Power Spectrum in Fast Survey, 32 frequencies for SCM, Axis 3

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI Potential, Sensor 1

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI Potential, Sensor 2

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI Potential, Sensor 3

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI Potential, Sensor 4

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI Potential, Sensor 5

FFT Power Spectrum in Fast Survey, 32 frequencies for EFI Potential, Sensor 6

FFT Power Spectrum in Particle Burst, 32 frequencies for SCM delta-B (parallel to B)

FFT Power Spectrum in Particle Burst, 32 frequencies for SCM delta-B (perp to B)

FFT Power Spectrum in Particle Burst, 32 frequencies for E Field AC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Particle Burst, 32 frequencies for E Field AC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Particle Burst, 32 frequencies for E Field AC Component, Sensors 5&6 (axial)

FFT Power Spectrum in Particle Burst, 32 frequencies for E Field DC Component, Sensors 1&2 (spin plane)

FFT Power Spectrum in Particle Burst, 32 frequencies for E Field DC Component, Sensors 3&4 (spin plane)

FFT Power Spectrum in Particle Burst, 32 frequencies for E Field DC Component, Sensors 5&6 (axial)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fgs_epoch, @1 => thb_fgl_epoch16, @2 => thb_fgh_epoch16, @3 => thb_fge_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fgs_epoch, @1 => thb_fgl_epoch16, @2 => thb_fgh_epoch16, @3 => thb_fge_epoch16.)

THEMIS-B (P1/ARTEMIS-P1):  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

THEMIS-B:  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fgs_epoch, @1 => thb_efs_epoch, @2 => thb_fit_bfit_epoch, @3 => thb_fit_efit_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_fgs_epoch, @1 => thb_efs_epoch, @2 => thb_fit_bfit_epoch, @3 => thb_fit_efit_epoch.)

THEMIS-B:  Solid State Telescope (ESA+SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (ions: 5 eV - 4 MeV,electrons: 6 eV - 700 keV)

THEMIS-B:  Solid State Telescope (SST) & Electrostatic Analyzer (ESA): ground calculatedenergy fluxes & moments.(density, velocity, pressure, and temperature) Generated from ESA+SST combined distributions

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_ptiff_epoch, @1 => thb_pteff_epoch, @2 => thb_ptirf_epoch, @3 => thb_pterf_epoch, @4 => thb_ptibb_epoch, @5 => thb_ptebb_epoch, @6 => thb_eesa_solarwind_flag_epoch, @7 => thb_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_ptiff_epoch, @1 => thb_pteff_epoch, @2 => thb_ptirf_epoch, @3 => thb_pterf_epoch, @4 => thb_ptibb_epoch, @5 => thb_ptebb_epoch, @6 => thb_eesa_solarwind_flag_epoch, @7 => thb_iesa_solarwind_flag_epoch.)

This data set contains ARTEMIS P1(THEMIS B) plasma parameters from the Electrostatic Analyzer (ESA), magnetic field data from the FGM instrument, and geocentric and selenocentric spacecraft position data. The data are at 96s or 384s resolution. For more details see 

THEMIS-B: Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 2: Counter saturation, 4: Solar Wind not in Solar Wind Mode, or Solar Wind Mode, not in Solar Wind, 8: (Reduced Mode only) slow survey mode+flows, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).1. Retrieval of CDF files from CDAWeb of of ESA L2 'good' quality, 'full mode, 'ion plasma data [density (N), thermal speed(W), flow velocity GSE Cartesian components (Vx,Vy, Vz)], starting 9/1/2010 when the spacecraft are mostly in the moon's vicinity.  'Full mode' means as determined from 3-sec high-angular-resolution distributions taken once every 96s (Fast Survey Scan - FSS) or 384s (Slow Survey Scan - SSS), where FSS and SSS are mutually exclusively used for several contiguous hours during each of most days.  Data retrieval was followed by creation of ASCII version with N, W, and Vi, and with |V|(flow speed) as computed by us from the Vi.1a.  Despike the plasma data.  A modest number of ESA L2 data points appear to be single-point spurious spikes.  We have attempted to delete these as follows.  We test a point using its two predecessors and two followers. We require that the 1st and last of these 5 points be within 60 mins of each other. The first two and last two points in a data segment separated from its neighbors by intervals of >60 min go untested by the algorithms discussed here.  We visually scanned output data looking for obvious spikes thereby missed, and deleted these.  Any record having a declared spike in any of its physical parameters is rejected. For a parameter value to be declared a spike, it must satisfy two criteria.   Let P represent the value of the physical parameter being tested. Define <P> as the mean value of parameter P over the 1st, 2nd, 4th, and 5th points of the current set, and let sigma(P) be the RMS deviation in this average.  The first test for a spike is to have |P-<P>| > 20 * sigma(P).  As the second test, for P = V, Vi (i = x, y, z), N, W, we require |P-<P>| > k * <P> where k = 0.1, 0.1, 0.3, 0.6 for P = V, Vi, N, W respectively.  For Themis B and C, these tests eliminated 64 and 51 96s or 384s ESA L2 points, respectively, over the interval September 3, 2010 - January 29, 2011.1b.  In addition to retrieving ESA N, W and Vi values from CDAWeb, we also retrieved the ESA ion mode flag, where the values are 0 and 1.  Zero denotes a magnetospheric mode and one a solar wind mode.  The magnetosphere mode involves taking measurements over much broader ranges in energy and look direction than for the solar wind mode.  This optimizes observations of hot, subsonic non-solar wind plasma and of cooler supersonically flowing solar wind plasma.  Usually, but not always, ESA is set to the solar wind mode when the spacecraft is in the solar wind.  Moments of ESA magnetosphere-mode data taken while in the solar wind are not reliable.  For further details, see the ESA documentation accessible through the UCB URL given above. 2. Retrieval of 1-min spacecraft position (GSE) data from SSCWeb3. Retrieval of 29-min lunar position (GSE) data from SSCWeb4. Calculation of moon-centered 1-min spacecraft positions by interpolating 29-min data to 1-min resolution, taking differences between the geocentric spacecraft and moon positions, and changing units from Re to Rm (Moon radii, = 1737 km).5. Merger of geocentric and selenocentric spacecraft position data and plasma data, interpolating the 1-min position data to the times of the plasma data6. Retrieval of CDF files of 3-sec magnetic field FGM data in GSE coordinates from CDAWeb and conversion to ASCII.7. Merger of plasma/position data and magnetic field data.  To each 96s or 384s plasma/position record, we add the 3-s magnetic field data whose time tag is closest to that of the plasma data (because, as noted above, the plasma parameters are based on high-angular-resolution ion plasma distributions each determined over three seconds.8. Creation of FTPBrowser interfaces to these data for (a) plots and listings [http://ftpbrowser.gsfc.nasa.gov/themisb_mrg.html] and (b) parameter value occurrence distributions and other statistics, with filtering [http://ftpbrowser.gsfc.nasa.gov/themisb_mrg_d.html].(These interfaces will soon be LunaSOX-accessible at https://lunasox.gsfc.nasa.gov/Data_browser.html.)

SPDF/CDAWeb. Please also acknowledge the data producer: N. Papatashvilli, J.H. King at SPDF, NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: N. Papatashvilli, J.H. King at SPDF, NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: N. Papatashvilli, J.H. King at SPDF, NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thb/l2/merged/cdf/2010/thb_l2_merged_20100101_v01.cdf. The most common cadence, 383849 [ms] = PT6M23.849S, occurred for 10.7379% of the 780 timesteps. 

THEMIS-B (P1/ARTEMIS-P1_):  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.

THEMIS-B:  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_peim_epoch, @1 => thb_peem_epoch, @2 => thb_pxxm_epoch, @3 => thb_eesa_solarwind_flag_epoch, @4 => thb_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_peim_epoch, @1 => thb_peem_epoch, @2 => thb_pxxm_epoch, @3 => thb_eesa_solarwind_flag_epoch, @4 => thb_iesa_solarwind_flag_epoch.)

(Good data only) ESA On Board Moment (MOM) Ion Density, THEMIS-B

(All qualities data) ESA On Board Moment (MOM) Ion Density, THEMIS-B

(Good data only) ESA On Board Moment (MOM) Electron Density, THEMIS-B

(All Qualities data) ESA On Board Moment (MOM) Electron Density, THEMIS-B

THEMIS-B: Search Coil Magnetometer (SCM) Magnetic Field Measurements. Includes FAST SURVEY, PARTICLE BURST and WAVE BURST data. FAST SURVEY (SCF): 1/8 second time resolution. PARTICLE BURST (SCP): 1/128 second time resolution; only short bursts of data. WAVE BURST (SCW): 1/8192 second time resolution; only short bursts of data. Sensor and electronics design provided by LPP, Roux and Le Contel

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_scf_epoch, @1 => thb_scp_epoch16, @2 => thb_scw_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_scf_epoch, @1 => thb_scp_epoch16, @2 => thb_scw_epoch16.)

thb_scf_epoch: Search Coil Fast-survey (SCF, 1/8 sec time resolution) epoch variable

thb_scp_epoch16: Search Coil Particle-burst (SCP, 1/128 sec time resolution) epoch variable

thb_scw_epoch16: Search Coil Wave-burst (SCW, 1/8192 sec time resolution) epoch variable

THEMIS-B:  Solid State Telescope (SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (30 keV - 300 keV).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_psif_epoch, @1 => thb_psef_epoch, @2 => thb_psib_epoch, @3 => thb_pseb_epoch, @4 => thb_eesa_solarwind_flag_epoch, @5 => thb_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thb_psif_epoch, @1 => thb_psef_epoch, @2 => thb_psib_epoch, @3 => thb_pseb_epoch, @4 => thb_eesa_solarwind_flag_epoch, @5 => thb_iesa_solarwind_flag_epoch.)

Spacecraft potential used in generation of thb_psif moments(Good data only)

Spacecraft potential used in generation of thb_psif moments(All qualities)

Spacecraft potential used in generation of thb_psef moments(Good data only)

Spacecraft potential used in generation of thb_psef moments(All qualities)

Spacecraft potential used in generation of thb_psib moments(Good data only)

Spacecraft potential used in generation of thb_psib moments(All qualities)

Spacecraft potential used in generation of thb_pseb moments(Good data only)

Spacecraft potential used in generation of thb_pseb moments(All qualities)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thb/ssc/2007/thb_or_ssc_20070217_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 15826 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thc/ssc_pre/2008/thcpred_or_ssc_20080101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 240450 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thc/helio1day/thc_helio1day_position_20070219_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 6491 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thc/helio1hr/thc_helio1hr_position_20070219_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 159671 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_state_epoch, @1 => thc_spin_epoch, @2 => thc_spin_ecl_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_state_epoch, @1 => thc_spin_epoch, @2 => thc_spin_ecl_epoch.)

THEMIS-C: Electric Field Instrument (EFI) Electric field measurements. The L2 product is a 3D estimate of Eperp derived from the spin plane E-field measurements assuming E dot B = 0, using relevant FGM (Flux-Gate Magnetometer) data.Includes spin-averaged, and Fast-survey field data.Spin-averaged (EFS_DOT0) data has approximately 3 second time resolution. Fast-survey (EFF_DOT0) data has 1/8 second time resolution.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_efs_dot0_epoch, @1 => thc_eff_dot0_epoch, @2 => thc_eff_q_mag_epoch, @3 => thc_eff_q_pha_epoch, @4 => thc_eff_e12_efs_epoch, @5 => thc_eff_e34_efs_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_efs_dot0_epoch, @1 => thc_eff_dot0_epoch, @2 => thc_eff_q_mag_epoch, @3 => thc_eff_q_pha_epoch, @4 => thc_eff_e12_efs_epoch, @5 => thc_eff_e34_efs_epoch.)

thc_efs_dot0_epoch: Electric field Instrument Spin-fit (EFS_DOT0, approx. 3 sec time resolution) epoch variable

thc_eff_dot0_epoch: Electric field Instrument Fast-survey (EFF_DOT0, 1/8 sec time resolution) epoch variable

thc_eff_q_mag_epoch: Electric field Instrument Spin-averaged (EFF_Q_MAG, approx. 3 sec time resolution) epoch variable

thc_eff_q_pha_epoch: Electric field Instrument Spin-averaged (EFF_Q_PHA, approx. 3 sec time resolution) epoch variable

thc_eff_e12_efs_epoch: Electric field Instrument Spin-averaged (EFF_E12_EFS, approx. 3 sec time resolution) epoch variable

thc_eff_e34_efs_epoch: Electric field Instrument Spin-averaged (EFF_E34_EFS, approx. 3 sec time resolution) epoch variable

THEMIS-C: Electric Field Instrument Particle Burst Mode (EFP) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/128 to 1/512 second time resolution.

thc_efp_epoch: Electric field Instrument Fast-survey (EFP, 1/8 sec time resolution) epoch variable

THEMIS-C: Electric Field Instrument Wave Burst Mode (EFW) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/16384 second time resolution.

thc_efw_epoch: Electric field Instrument Fast-survey (EFW, 1/8 sec time resolution) epoch variable

THEMIS-C (P2/ARTEMIS-P2): Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution.

THEMIS-C: Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 2: Counter saturation, 4: Solar Wind not in Solar Wind Mode, or Solar Wind Mode, not in Solar Wind, 8: (Reduced Mode only) slow survey mode+flows, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_peif_epoch, @1 => thc_peef_epoch, @2 => thc_peir_epoch, @3 => thc_peer_epoch, @4 => thc_peib_epoch, @5 => thc_peeb_epoch, @6 => thc_eesa_solarwind_flag_epoch, @7 => thc_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_peif_epoch, @1 => thc_peef_epoch, @2 => thc_peir_epoch, @3 => thc_peer_epoch, @4 => thc_peib_epoch, @5 => thc_peeb_epoch, @6 => thc_eesa_solarwind_flag_epoch, @7 => thc_iesa_solarwind_flag_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fb_hff_epoch, @1 => thc_fb_v1_epoch, @2 => thc_fb_v2_epoch, @3 => thc_fb_v3_epoch, @4 => thc_fb_v4_epoch, @5 => thc_fb_v5_epoch, @6 => thc_fb_v6_epoch, @7 => thc_fb_edc12_epoch, @8 => thc_fb_edc34_epoch, @9 => thc_fb_edc56_epoch, @10 => thc_fb_scm1_epoch, @11 => thc_fb_scm2_epoch, @12 => thc_fb_scm3_epoch, @13 => thc_fb_eac12_epoch, @14 => thc_fb_eac34_epoch, @15 => thc_fb_eac56_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fb_hff_epoch, @1 => thc_fb_v1_epoch, @2 => thc_fb_v2_epoch, @3 => thc_fb_v3_epoch, @4 => thc_fb_v4_epoch, @5 => thc_fb_v5_epoch, @6 => thc_fb_v6_epoch, @7 => thc_fb_edc12_epoch, @8 => thc_fb_edc34_epoch, @9 => thc_fb_edc56_epoch, @10 => thc_fb_scm1_epoch, @11 => thc_fb_scm2_epoch, @12 => thc_fb_scm3_epoch, @13 => thc_fb_eac12_epoch, @14 => thc_fb_eac34_epoch, @15 => thc_fb_eac56_epoch.)

THEMIS-C:  On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field, for particle and wave burst survey modes.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fff_16_epoch, @1 => thc_fff_32_epoch, @2 => thc_fff_64_epoch, @3 => thc_ffp_16_epoch, @4 => thc_ffp_32_epoch, @5 => thc_ffp_64_epoch, @6 => thc_ffw_16_epoch, @7 => thc_ffw_32_epoch, @8 => thc_ffw_64_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fff_16_epoch, @1 => thc_fff_32_epoch, @2 => thc_fff_64_epoch, @3 => thc_ffp_16_epoch, @4 => thc_ffp_32_epoch, @5 => thc_ffp_64_epoch, @6 => thc_ffw_16_epoch, @7 => thc_ffw_32_epoch, @8 => thc_ffw_64_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fgs_epoch, @1 => thc_fgl_epoch16, @2 => thc_fgh_epoch16, @3 => thc_fge_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fgs_epoch, @1 => thc_fgl_epoch16, @2 => thc_fgh_epoch16, @3 => thc_fge_epoch16.)

THEMIS-C (P2/ARTEMIS-P2):  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

THEMIS-C:  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fgs_epoch, @1 => thc_efs_epoch, @2 => thc_fit_bfit_epoch, @3 => thc_fit_efit_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_fgs_epoch, @1 => thc_efs_epoch, @2 => thc_fit_bfit_epoch, @3 => thc_fit_efit_epoch.)

THEMIS-C:  Solid State Telescope (ESA+SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (ions: 5 eV - 4 MeV,electrons: 6 eV - 700 keV)

THEMIS-C:  Solid State Telescope (SST) & Electrostatic Analyzer (ESA): ground calculatedenergy fluxes & moments.(density, velocity, pressure, and temperature) Generated from ESA+SST combined distributions

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_ptiff_epoch, @1 => thc_pteff_epoch, @2 => thc_ptirf_epoch, @3 => thc_pterf_epoch, @4 => thc_ptibb_epoch, @5 => thc_ptebb_epoch, @6 => thc_eesa_solarwind_flag_epoch, @7 => thc_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_ptiff_epoch, @1 => thc_pteff_epoch, @2 => thc_ptirf_epoch, @3 => thc_pterf_epoch, @4 => thc_ptibb_epoch, @5 => thc_ptebb_epoch, @6 => thc_eesa_solarwind_flag_epoch, @7 => thc_iesa_solarwind_flag_epoch.)

This data set contains ARTEMIS P2(THEMIS C) plasma parameters from the Electrostatic Analyzer (ESA), magnetic field data from the FGM instrument, and geocentric and selenocentric spacecraft position data. The data are at 96s or 384s resolution. For more details see 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thc/l2/merged/cdf/2010/thc_l2_merged_20100101_v01.cdf. The most common cadence, 420174 [ms] = PT7M0.174S, occurred for 15.2732% of the 1012 timesteps. 

THEMIS-C (P2/ARTEMIS-P2):  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.

THEMIS-C:  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_peim_epoch, @1 => thc_peem_epoch, @2 => thc_pxxm_epoch, @3 => thc_eesa_solarwind_flag_epoch, @4 => thc_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_peim_epoch, @1 => thc_peem_epoch, @2 => thc_pxxm_epoch, @3 => thc_eesa_solarwind_flag_epoch, @4 => thc_iesa_solarwind_flag_epoch.)

(Good data only) ESA On Board Moment (MOM) Ion Density, THEMIS-C

(All qualities data) ESA On Board Moment (MOM) Ion Density, THEMIS-C

(Good data only) ESA On Board Moment (MOM) Electron Density, THEMIS-C

(All Qualities data) ESA On Board Moment (MOM) Electron Density, THEMIS-C

THEMIS-C: Search Coil Magnetometer (SCM) Magnetic Field Measurements. Includes FAST SURVEY, PARTICLE BURST and WAVE BURST data. FAST SURVEY (SCF): 1/8 second time resolution. PARTICLE BURST (SCP): 1/128 second time resolution; only short bursts of data. WAVE BURST (SCW): 1/8192 second time resolution; only short bursts of data. Sensor and electronics design provided by LPP, Roux and Le Contel

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_scf_epoch, @1 => thc_scp_epoch16, @2 => thc_scw_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_scf_epoch, @1 => thc_scp_epoch16, @2 => thc_scw_epoch16.)

thc_scf_epoch: Search Coil Fast-survey (SCF, 1/8 sec time resolution) epoch variable

thc_scp_epoch16: Search Coil Particle-burst (SCP, 1/128 sec time resolution) epoch variable

thc_scw_epoch16: Search Coil Wave-burst (SCW, 1/8192 sec time resolution) epoch variable

THEMIS-C:  Solid State Telescope (SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (30 keV - 300 keV).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_psif_epoch, @1 => thc_psef_epoch, @2 => thc_psib_epoch, @3 => thc_pseb_epoch, @4 => thc_eesa_solarwind_flag_epoch, @5 => thc_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thc_psif_epoch, @1 => thc_psef_epoch, @2 => thc_psib_epoch, @3 => thc_pseb_epoch, @4 => thc_eesa_solarwind_flag_epoch, @5 => thc_iesa_solarwind_flag_epoch.)

Spacecraft potential used in generation of thc_psif moments(Good data only)

Spacecraft potential used in generation of thc_psif moments(All qualities)

Spacecraft potential used in generation of thc_psef moments(Good data only)

Spacecraft potential used in generation of thc_psef moments(All qualities)

Spacecraft potential used in generation of thc_psib moments(Good data only)

Spacecraft potential used in generation of thc_psib moments(All qualities)

Spacecraft potential used in generation of thc_pseb moments(Good data only)

Spacecraft potential used in generation of thc_pseb moments(All qualities)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thc/ssc/2007/thc_or_ssc_20070217_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 15826 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thd/ssc_pre/2008/thdpred_or_ssc_20080101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 240450 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_state_epoch, @1 => thd_spin_epoch, @2 => thd_spin_ecl_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_state_epoch, @1 => thd_spin_epoch, @2 => thd_spin_ecl_epoch.)

THEMIS-D: Electric Field Instrument (EFI) Electric field measurements. The L2 product is a 3D estimate of Eperp derived from the spin plane E-field measurements assuming E dot B = 0, using relevant FGM (Flux-Gate Magnetometer) data.Includes spin-averaged, and Fast-survey field data.Spin-averaged (EFS_DOT0) data has approximately 3 second time resolution. Fast-survey (EFF_DOT0) data has 1/8 second time resolution.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_efs_dot0_epoch, @1 => thd_eff_dot0_epoch, @2 => thd_eff_q_mag_epoch, @3 => thd_eff_q_pha_epoch, @4 => thd_eff_e12_efs_epoch, @5 => thd_eff_e34_efs_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_efs_dot0_epoch, @1 => thd_eff_dot0_epoch, @2 => thd_eff_q_mag_epoch, @3 => thd_eff_q_pha_epoch, @4 => thd_eff_e12_efs_epoch, @5 => thd_eff_e34_efs_epoch.)

thd_efs_dot0_epoch: Electric field Instrument Spin-fit (EFS_DOT0, approx. 3 sec time resolution) epoch variable

thd_eff_dot0_epoch: Electric field Instrument Fast-survey (EFF_DOT0, 1/8 sec time resolution) epoch variable

thd_eff_q_mag_epoch: Electric field Instrument Spin-averaged (EFF_Q_MAG, approx. 3 sec time resolution) epoch variable

thd_eff_q_pha_epoch: Electric field Instrument Spin-averaged (EFF_Q_PHA, approx. 3 sec time resolution) epoch variable

thd_eff_e12_efs_epoch: Electric field Instrument Spin-averaged (EFF_E12_EFS, approx. 3 sec time resolution) epoch variable

thd_eff_e34_efs_epoch: Electric field Instrument Spin-averaged (EFF_E34_EFS, approx. 3 sec time resolution) epoch variable

THEMIS-D: Electric Field Instrument Particle Burst Mode (EFP) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/128 to 1/512 second time resolution.

thd_efp_epoch: Electric field Instrument Fast-survey (EFP, 1/8 sec time resolution) epoch variable

THEMIS-D: Electric Field Instrument Wave Burst Mode (EFW) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/16384 second time resolution.

thd_efw_epoch: Electric field Instrument Fast-survey (EFW, 1/8 sec time resolution) epoch variable

THEMIS-D (P3): Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution.

THEMIS-D: Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 2: Counter saturation, 4: Solar Wind not in Solar Wind Mode, or Solar Wind Mode, not in Solar Wind, 8: (Reduced Mode only) slow survey mode+flows, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_peif_epoch, @1 => thd_peef_epoch, @2 => thd_peir_epoch, @3 => thd_peer_epoch, @4 => thd_peib_epoch, @5 => thd_peeb_epoch, @6 => thd_eesa_solarwind_flag_epoch, @7 => thd_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_peif_epoch, @1 => thd_peef_epoch, @2 => thd_peir_epoch, @3 => thd_peer_epoch, @4 => thd_peib_epoch, @5 => thd_peeb_epoch, @6 => thd_eesa_solarwind_flag_epoch, @7 => thd_iesa_solarwind_flag_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fb_hff_epoch, @1 => thd_fb_v1_epoch, @2 => thd_fb_v2_epoch, @3 => thd_fb_v3_epoch, @4 => thd_fb_v4_epoch, @5 => thd_fb_v5_epoch, @6 => thd_fb_v6_epoch, @7 => thd_fb_edc12_epoch, @8 => thd_fb_edc34_epoch, @9 => thd_fb_edc56_epoch, @10 => thd_fb_scm1_epoch, @11 => thd_fb_scm2_epoch, @12 => thd_fb_scm3_epoch, @13 => thd_fb_eac12_epoch, @14 => thd_fb_eac34_epoch, @15 => thd_fb_eac56_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fb_hff_epoch, @1 => thd_fb_v1_epoch, @2 => thd_fb_v2_epoch, @3 => thd_fb_v3_epoch, @4 => thd_fb_v4_epoch, @5 => thd_fb_v5_epoch, @6 => thd_fb_v6_epoch, @7 => thd_fb_edc12_epoch, @8 => thd_fb_edc34_epoch, @9 => thd_fb_edc56_epoch, @10 => thd_fb_scm1_epoch, @11 => thd_fb_scm2_epoch, @12 => thd_fb_scm3_epoch, @13 => thd_fb_eac12_epoch, @14 => thd_fb_eac34_epoch, @15 => thd_fb_eac56_epoch.)

THEMIS-D:  On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field, for particle and wave burst survey modes.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fff_16_epoch, @1 => thd_fff_32_epoch, @2 => thd_fff_64_epoch, @3 => thd_ffp_16_epoch, @4 => thd_ffp_32_epoch, @5 => thd_ffp_64_epoch, @6 => thd_ffw_16_epoch, @7 => thd_ffw_32_epoch, @8 => thd_ffw_64_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fff_16_epoch, @1 => thd_fff_32_epoch, @2 => thd_fff_64_epoch, @3 => thd_ffp_16_epoch, @4 => thd_ffp_32_epoch, @5 => thd_ffp_64_epoch, @6 => thd_ffw_16_epoch, @7 => thd_ffw_32_epoch, @8 => thd_ffw_64_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fgs_epoch, @1 => thd_fgl_epoch16, @2 => thd_fgh_epoch16, @3 => thd_fge_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fgs_epoch, @1 => thd_fgl_epoch16, @2 => thd_fgh_epoch16, @3 => thd_fge_epoch16.)

THEMIS-D:  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fgs_epoch, @1 => thd_efs_epoch, @2 => thd_fit_bfit_epoch, @3 => thd_fit_efit_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_fgs_epoch, @1 => thd_efs_epoch, @2 => thd_fit_bfit_epoch, @3 => thd_fit_efit_epoch.)

THEMIS-D:  Solid State Telescope (ESA+SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (ions: 5 eV - 4 MeV,electrons: 6 eV - 700 keV)

THEMIS-D:  Solid State Telescope (SST) & Electrostatic Analyzer (ESA): ground calculatedenergy fluxes & moments.(density, velocity, pressure, and temperature) Generated from ESA+SST combined distributions

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_ptiff_epoch, @1 => thd_pteff_epoch, @2 => thd_ptirf_epoch, @3 => thd_pterf_epoch, @4 => thd_ptibb_epoch, @5 => thd_ptebb_epoch, @6 => thd_eesa_solarwind_flag_epoch, @7 => thd_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_ptiff_epoch, @1 => thd_pteff_epoch, @2 => thd_ptirf_epoch, @3 => thd_pterf_epoch, @4 => thd_ptibb_epoch, @5 => thd_ptebb_epoch, @6 => thd_eesa_solarwind_flag_epoch, @7 => thd_iesa_solarwind_flag_epoch.)

THEMIS-D (P3):  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.

THEMIS-D:  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_peim_epoch, @1 => thd_peem_epoch, @2 => thd_pxxm_epoch, @3 => thd_eesa_solarwind_flag_epoch, @4 => thd_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_peim_epoch, @1 => thd_peem_epoch, @2 => thd_pxxm_epoch, @3 => thd_eesa_solarwind_flag_epoch, @4 => thd_iesa_solarwind_flag_epoch.)

(Good data only) ESA On Board Moment (MOM) Ion Density, THEMIS-D

(All qualities data) ESA On Board Moment (MOM) Ion Density, THEMIS-D

(Good data only) ESA On Board Moment (MOM) Electron Density, THEMIS-D

(All Qualities data) ESA On Board Moment (MOM) Electron Density, THEMIS-D

THEMIS-D: Search Coil Magnetometer (SCM) Magnetic Field Measurements. Includes FAST SURVEY, PARTICLE BURST and WAVE BURST data. FAST SURVEY (SCF): 1/8 second time resolution. PARTICLE BURST (SCP): 1/128 second time resolution; only short bursts of data. WAVE BURST (SCW): 1/8192 second time resolution; only short bursts of data. Sensor and electronics design provided by LPP, Roux and Le Contel

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_scf_epoch, @1 => thd_scp_epoch16, @2 => thd_scw_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_scf_epoch, @1 => thd_scp_epoch16, @2 => thd_scw_epoch16.)

thd_scf_epoch: Search Coil Fast-survey (SCF, 1/8 sec time resolution) epoch variable

thd_scp_epoch16: Search Coil Particle-burst (SCP, 1/128 sec time resolution) epoch variable

thd_scw_epoch16: Search Coil Wave-burst (SCW, 1/8192 sec time resolution) epoch variable

THEMIS-D:  Solid State Telescope (SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (30 keV - 300 keV).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_psif_epoch, @1 => thd_psef_epoch, @2 => thd_psib_epoch, @3 => thd_pseb_epoch, @4 => thd_eesa_solarwind_flag_epoch, @5 => thd_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thd_psif_epoch, @1 => thd_psef_epoch, @2 => thd_psib_epoch, @3 => thd_pseb_epoch, @4 => thd_eesa_solarwind_flag_epoch, @5 => thd_iesa_solarwind_flag_epoch.)

Spacecraft potential used in generation of thd_psif moments(Good data only)

Spacecraft potential used in generation of thd_psif moments(All qualities)

Spacecraft potential used in generation of thd_psef moments(Good data only)

Spacecraft potential used in generation of thd_psef moments(All qualities)

Spacecraft potential used in generation of thd_psib moments(Good data only)

Spacecraft potential used in generation of thd_psib moments(All qualities)

Spacecraft potential used in generation of thd_pseb moments(Good data only)

Spacecraft potential used in generation of thd_pseb moments(All qualities)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thd/ssc/2007/thd_or_ssc_20070217_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 15826 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/the/ssc_pre/2008/thepred_or_ssc_20080101_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 240450 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_state_epoch, @1 => the_spin_epoch, @2 => the_spin_ecl_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_state_epoch, @1 => the_spin_epoch, @2 => the_spin_ecl_epoch.)

THEMIS-E: Electric Field Instrument (EFI) Electric field measurements. The L2 product is a 3D estimate of Eperp derived from the spin plane E-field measurements assuming E dot B = 0, using relevant FGM (Flux-Gate Magnetometer) data.Includes spin-averaged, and Fast-survey field data.Spin-averaged (EFS_DOT0) data has approximately 3 second time resolution. Fast-survey (EFF_DOT0) data has 1/8 second time resolution.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_efs_dot0_epoch, @1 => the_eff_dot0_epoch, @2 => the_eff_q_mag_epoch, @3 => the_eff_q_pha_epoch, @4 => the_eff_e12_efs_epoch, @5 => the_eff_e34_efs_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_efs_dot0_epoch, @1 => the_eff_dot0_epoch, @2 => the_eff_q_mag_epoch, @3 => the_eff_q_pha_epoch, @4 => the_eff_e12_efs_epoch, @5 => the_eff_e34_efs_epoch.)

the_efs_dot0_epoch: Electric field Instrument Spin-fit (EFS_DOT0, approx. 3 sec time resolution) epoch variable

the_eff_dot0_epoch: Electric field Instrument Fast-survey (EFF_DOT0, 1/8 sec time resolution) epoch variable

the_eff_q_mag_epoch: Electric field Instrument Spin-averaged (EFF_Q_MAG, approx. 3 sec time resolution) epoch variable

the_eff_q_pha_epoch: Electric field Instrument Spin-averaged (EFF_Q_PHA, approx. 3 sec time resolution) epoch variable

the_eff_e12_efs_epoch: Electric field Instrument Spin-averaged (EFF_E12_EFS, approx. 3 sec time resolution) epoch variable

the_eff_e34_efs_epoch: Electric field Instrument Spin-averaged (EFF_E34_EFS, approx. 3 sec time resolution) epoch variable

THEMIS-E: Electric Field Instrument Particle Burst Mode (EFP) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/128 to 1/512 second time resolution.

the_efp_epoch: Electric field Instrument Fast-survey (EFP, 1/8 sec time resolution) epoch variable

THEMIS-E: Electric Field Instrument Wave Burst Mode (EFW) Electric field measurements. The L2 product is the cleaned 3D E-field with 1/16384 second time resolution.

the_efw_epoch: Electric field Instrument Fast-survey (EFW, 1/8 sec time resolution) epoch variable

THEMIS-E (P4): Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution.

THEMIS-E: Electrostatic Analyzer (ESA): Electron/Ion Ground-Calculated Energy Fluxes (ions: 5 eV to 25 keV) electrons: 6 eV to 30 keV) and Moments (density, velocity, pressure, and temperature). Includes FULL, REDUCED and BURST modes. FULL: high angular resolution, low (few min) time resolution. REDUCED: degraded angular resolution, high (approx. 3 sec) time resolution. BURST: high angular resolution, high time resolution; only short bursts of data. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 2: Counter saturation, 4: Solar Wind not in Solar Wind Mode, or Solar Wind Mode, not in Solar Wind, 8: (Reduced Mode only) slow survey mode+flows, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_peif_epoch, @1 => the_peef_epoch, @2 => the_peir_epoch, @3 => the_peer_epoch, @4 => the_peib_epoch, @5 => the_peeb_epoch, @6 => the_eesa_solarwind_flag_epoch, @7 => the_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_peif_epoch, @1 => the_peef_epoch, @2 => the_peir_epoch, @3 => the_peer_epoch, @4 => the_peib_epoch, @5 => the_peeb_epoch, @6 => the_eesa_solarwind_flag_epoch, @7 => the_iesa_solarwind_flag_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fb_hff_epoch, @1 => the_fb_v1_epoch, @2 => the_fb_v2_epoch, @3 => the_fb_v3_epoch, @4 => the_fb_v4_epoch, @5 => the_fb_v5_epoch, @6 => the_fb_v6_epoch, @7 => the_fb_edc12_epoch, @8 => the_fb_edc34_epoch, @9 => the_fb_edc56_epoch, @10 => the_fb_scm1_epoch, @11 => the_fb_scm2_epoch, @12 => the_fb_scm3_epoch, @13 => the_fb_eac12_epoch, @14 => the_fb_eac34_epoch, @15 => the_fb_eac56_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fb_hff_epoch, @1 => the_fb_v1_epoch, @2 => the_fb_v2_epoch, @3 => the_fb_v3_epoch, @4 => the_fb_v4_epoch, @5 => the_fb_v5_epoch, @6 => the_fb_v6_epoch, @7 => the_fb_edc12_epoch, @8 => the_fb_edc34_epoch, @9 => the_fb_edc56_epoch, @10 => the_fb_scm1_epoch, @11 => the_fb_scm2_epoch, @12 => the_fb_scm3_epoch, @13 => the_fb_eac12_epoch, @14 => the_fb_eac34_epoch, @15 => the_fb_eac56_epoch.)

THEMIS-E:  On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field, for particle and wave burst survey modes.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fff_16_epoch, @1 => the_fff_32_epoch, @2 => the_fff_64_epoch, @3 => the_ffp_16_epoch, @4 => the_ffp_32_epoch, @5 => the_ffp_64_epoch, @6 => the_ffw_16_epoch, @7 => the_ffw_32_epoch, @8 => the_ffw_64_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 9 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fff_16_epoch, @1 => the_fff_32_epoch, @2 => the_fff_64_epoch, @3 => the_ffp_16_epoch, @4 => the_ffp_32_epoch, @5 => the_ffp_64_epoch, @6 => the_ffw_16_epoch, @7 => the_ffw_32_epoch, @8 => the_ffw_64_epoch.)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fgs_epoch, @1 => the_fgl_epoch16, @2 => the_fgh_epoch16, @3 => the_fge_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fgs_epoch, @1 => the_fgl_epoch16, @2 => the_fgh_epoch16, @3 => the_fge_epoch16.)

THEMIS-E:  On Board spin fits of Electric (EFI) and Magnetic (FGM) field. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fgs_epoch, @1 => the_efs_epoch, @2 => the_fit_bfit_epoch, @3 => the_fit_efit_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_fgs_epoch, @1 => the_efs_epoch, @2 => the_fit_bfit_epoch, @3 => the_fit_efit_epoch.)

THEMIS-E:  Solid State Telescope (ESA+SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (ions: 5 eV - 4 MeV,electrons: 6 eV - 700 keV)

THEMIS-E:  Solid State Telescope (SST) & Electrostatic Analyzer (ESA): ground calculatedenergy fluxes & moments.(density, velocity, pressure, and temperature) Generated from ESA+SST combined distributions

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_ptiff_epoch, @1 => the_pteff_epoch, @2 => the_ptirf_epoch, @3 => the_pterf_epoch, @4 => the_ptibb_epoch, @5 => the_ptebb_epoch, @6 => the_eesa_solarwind_flag_epoch, @7 => the_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 8 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_ptiff_epoch, @1 => the_pteff_epoch, @2 => the_ptirf_epoch, @3 => the_pterf_epoch, @4 => the_ptibb_epoch, @5 => the_ptebb_epoch, @6 => the_eesa_solarwind_flag_epoch, @7 => the_iesa_solarwind_flag_epoch.)

THEMIS-E (P4):  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.

THEMIS-E:  On Board moments:  Electron/Ion moments density, flux, velocity, pressure and temperature.Moment Data Quality flags (0: good data; non-zero flags are totals of values; 1: missing S/C potential, 16: electron density Gt 2*ion density, 32: ion density Gt 2*electron density, 64: Spacecraft Maneuver).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_peim_epoch, @1 => the_peem_epoch, @2 => the_pxxm_epoch, @3 => the_eesa_solarwind_flag_epoch, @4 => the_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_peim_epoch, @1 => the_peem_epoch, @2 => the_pxxm_epoch, @3 => the_eesa_solarwind_flag_epoch, @4 => the_iesa_solarwind_flag_epoch.)

(Good data only) ESA On Board Moment (MOM) Ion Density, THEMIS-E

(All qualities data) ESA On Board Moment (MOM) Ion Density, THEMIS-E

(Good data only) ESA On Board Moment (MOM) Electron Density, THEMIS-E

(All Qualities data) ESA On Board Moment (MOM) Electron Density, THEMIS-E

THEMIS-E: Search Coil Magnetometer (SCM) Magnetic Field Measurements. Includes FAST SURVEY, PARTICLE BURST and WAVE BURST data. FAST SURVEY (SCF): 1/8 second time resolution. PARTICLE BURST (SCP): 1/128 second time resolution; only short bursts of data. WAVE BURST (SCW): 1/8192 second time resolution; only short bursts of data. Sensor and electronics design provided by LPP, Roux and Le Contel

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_scf_epoch, @1 => the_scp_epoch16, @2 => the_scw_epoch16.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_scf_epoch, @1 => the_scp_epoch16, @2 => the_scw_epoch16.)

the_scf_epoch: Search Coil Fast-survey (SCF, 1/8 sec time resolution) epoch variable

the_scp_epoch16: Search Coil Particle-burst (SCP, 1/128 sec time resolution) epoch variable

the_scw_epoch16: Search Coil Wave-burst (SCW, 1/8192 sec time resolution) epoch variable

THEMIS-E:  Solid State Telescope (SST): Energy Flux spectrogram:  Data includes: Electron/Ion Ground-Calculated Fluxes (30 keV - 300 keV).

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_psif_epoch, @1 => the_psef_epoch, @2 => the_psib_epoch, @3 => the_pseb_epoch, @4 => the_eesa_solarwind_flag_epoch, @5 => the_iesa_solarwind_flag_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => the_psif_epoch, @1 => the_psef_epoch, @2 => the_psib_epoch, @3 => the_pseb_epoch, @4 => the_eesa_solarwind_flag_epoch, @5 => the_iesa_solarwind_flag_epoch.)

Spacecraft potential used in generation of the_psif moments(Good data only)

Spacecraft potential used in generation of the_psif moments(All qualities)

Spacecraft potential used in generation of the_psef moments(Good data only)

Spacecraft potential used in generation of the_psef moments(All qualities)

Spacecraft potential used in generation of the_psib moments(Good data only)

Spacecraft potential used in generation of the_psib moments(All qualities)

Spacecraft potential used in generation of the_pseb moments(Good data only)

Spacecraft potential used in generation of the_pseb moments(All qualities)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/the/ssc/2007/the_or_ssc_20070217_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 15826 timesteps. 

Ground-based All Sky Imager (ASI), 3-sec N-S Keograms ordered by longitude, THEMIS GBO network

THEMIS Ground Based Observatory part of the THEMIS GBO effort. The All-Sky-Imagers (ASI) take white lght images of the overhead sky. N-S Keograms are generated by combining the North-Southcross section of the image from each UT time into a single image with UT time as x-axis.

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos, S. Mende & E. Donovan at UCB & Univ of Calgary respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos, S. Mende & E. Donovan at UCB & Univ of Calgary respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos, S. Mende & E. Donovan at UCB & Univ of Calgary respectively, NASA NAS5-02099

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 20 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thg_ask_gbay_epoch, @1 => thg_ask_kuuj_epoch, @2 => thg_ask_chbg_epoch, @3 => thg_ask_snkq_epoch, @4 => thg_ask_kapu_epoch, @5 => thg_ask_rank_epoch, @6 => thg_ask_gill_epoch, @7 => thg_ask_pina_epoch, @8 => thg_ask_tpas_epoch, @9 => thg_ask_ekat_epoch, @10 => thg_ask_fsmi_epoch, @11 => thg_ask_atha_epoch, @12 => thg_ask_fsim_epoch, @13 => thg_ask_pgeo_epoch, @14 => thg_ask_inuv_epoch, @15 => thg_ask_whit_epoch, @16 => thg_ask_gako_epoch, @17 => thg_ask_fykn_epoch, @18 => thg_ask_mcgr_epoch, @19 => thg_ask_kian_epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 20 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => thg_ask_gbay_epoch, @1 => thg_ask_kuuj_epoch, @2 => thg_ask_chbg_epoch, @3 => thg_ask_snkq_epoch, @4 => thg_ask_kapu_epoch, @5 => thg_ask_rank_epoch, @6 => thg_ask_gill_epoch, @7 => thg_ask_pina_epoch, @8 => thg_ask_tpas_epoch, @9 => thg_ask_ekat_epoch, @10 => thg_ask_fsmi_epoch, @11 => thg_ask_atha_epoch, @12 => thg_ask_fsim_epoch, @13 => thg_ask_pgeo_epoch, @14 => thg_ask_inuv_epoch, @15 => thg_ask_whit_epoch, @16 => thg_ask_gako_epoch, @17 => thg_ask_fykn_epoch, @18 => thg_ask_mcgr_epoch, @19 => thg_ask_kian_epoch.)

THEMIS Ground Based Observatory (from all.xml/observatory/description/@short)

THEMIS Ground Based Observatory (from Master/CDFglobalAttributes/Source_name)

All Sky Imager, Keogram images, High resolution (from Master/CDFglobalAttributes/Data_type)

----------> EKAT Ekati, Canada  (Geog Lat 64.7, Long 249.3) [Data start 2005 through April 2006]

----------> PGEO Prince George (Geog Lat 53.8, Long 237.2) [Data only prior to Nov. 27, 2008]

Higher latitude chain (Lat 68.4, Long 18.8), Ground-based Vector Magnetic Field at Abisko, Sweden, 60 sec time resolution. 

Ground based observatory, part of the Geological Survey of Sweden (SGU). 

Geological Survey of Sweden, and INTERMAGNET for providing the data and promoting high standards of magnetic observatory practice.

Further information about the Time History of Events and Macroscale Interactions During Substorms (THEMIS) mission can be found at the

Information about the Fluxgate Magnetometers (GMAGS) can be found at the

The data made available through INTERMAGNET are provided for your use and are not for commercial use or sale or distribution to third parties without the written permission of the institute operating the observatory. Publications making use of the data should include an acknowledgment statement (see intermagnet.org). A citation reference should be sent to the INTERMAGNET Secretary (secretary@intermagnet.org) for inclusion in a publications list on the INTERMAGNET website.

SPDF/CDAWeb. Please also acknowledge the data producer: Gerhard Schwarz at Geological Survey of Sweden, Box 670 SE-751  28, Uppsala, Sweden

SPDF/SSCWeb. Please also acknowledge the data producer: Gerhard Schwarz at Geological Survey of Sweden, Box 670 SE-751  28, Uppsala, Sweden

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Gerhard Schwarz at Geological Survey of Sweden, Box 670 SE-751  28, Uppsala, Sweden

Higher latitude chain (Lat 60.8, Long 281.9), Ground-based Vector Magnetic Field at Akulivik, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

THEMIS Ground-based Observatory (GBO) Magnetic Field Data Portal

Calibration files at http://autumn.athabascau.ca/themis.gbo.mag.calibration

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos,  C. T. Russell, and M. Connors at UCB, UCLA, and U Athabasca respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos,  C. T. Russell, and M. Connors at UCB, UCLA, and U Athabasca respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos,  C. T. Russell, and M. Connors at UCB, UCLA, and U Athabasca respectively, NASA NAS5-02099

Higher latitude chain (Lat 69.6, Long 60.2), Ground-based Vector Magnetic Field at Amderma, Russia, 1 min, AARI network

Ground based observatory, Arctic and Antarctic Research Institute (AARI), Russia. 

Arctic and Antarctic Research Institute (AARI), Department of Geophysics

SPDF/CDAWeb. Please also acknowledge the data producer: Oleg Troshichev at Department of Geophysics, Arctic and Antarctic Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: Oleg Troshichev at Department of Geophysics, Arctic and Antarctic Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Oleg Troshichev at Department of Geophysics, Arctic and Antarctic Research Institute

Lower latitude chain (Lat 38.5, Long 263.7), Ground-based Vector Magnetic Field at Americus, KS, 0.5 sec, McMaC network, supported under NSF grant ATM-0245139

NASA Contract NAS5-02099, CSA Carisma, supported under NSF grant ATM-0245139

SPDF/CDAWeb. Please also acknowledge the data producer: Peter Chi at MCMAC data and NSF for support through grant ATM-0245139

SPDF/SSCWeb. Please also acknowledge the data producer: Peter Chi at MCMAC data and NSF for support through grant ATM-0245139

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Peter Chi at MCMAC data and NSF for support through grant ATM-0245139

Higher latitude chain (Lat 65.6, Long 322.4), Ground-based Vector Magnetic Field at Tasiilaq, Greenland, 60 sec, DTU network

DTU Space - National Space Institute, Denmark; Tromso Geophysical Observatory - University of Tromso, Norway

Information about the Technical University of Denmark (DTU) Department of Space Research and Space Technology can be found at the

Acknowledgement: Magnetometer data provided by: Hans Gleisner, Danish Meteorological Institute

SPDF/CDAWeb. Please also acknowledge the data producer: Hans Gleisner at Geomagnetism & Remote Sensing, Danish Meteorological Institute, Lyngbyvej 100, DK-2100 Copenhagen. email: hgl@dmi.dk

SPDF/SSCWeb. Please also acknowledge the data producer: Hans Gleisner at Geomagnetism & Remote Sensing, Danish Meteorological Institute, Lyngbyvej 100, DK-2100 Copenhagen. email: hgl@dmi.dk

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Hans Gleisner at Geomagnetism & Remote Sensing, Danish Meteorological Institute, Lyngbyvej 100, DK-2100 Copenhagen. email: hgl@dmi.dk

Tasiilaq, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 69.3, Long 16.0), Ground-based Vector Magnetic Field at Andenes, Norway, 1 min, Norwegian auroral zone magnetometer network

Part of the Tromso Geophysical Observatory ground magnetometer network 

Information about the The Arctic University of Norway (UiT) Department of Physics and Technology can be found at the

The geomagnetic information available at our web-pages is primarily intended for the non-commercial scientific community, educational purposes, and the general public. Commercial users of our services are urged to contact us to establish an agreement of use. As part of an agreement we normally offer to construct exclusive web-pages specifically for the application in question. We accept no liability for loss or damages of any kind resulting from this or from errors or inaccuracies in the data.

SPDF/CDAWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso N-9037 Tromso, Norway

SPDF/SSCWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso N-9037 Tromso, Norway

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso N-9037 Tromso, Norway

Higher latitude chain (Lat 68.1, Long 214.4), Ground-based Vector Magnetic Field at Arctic Village, AK, 1.0 sec, GIMA network

GIMA observatories - Data served as part of the THEMIS GBO effort

THEMIS Ground-based Observatory (GBO) Network Information Web Site

SPDF/CDAWeb. Please also acknowledge the data producer: D.Hampton at U Alaska, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: D.Hampton at U Alaska, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D.Hampton at U Alaska, NASA NAS5-02099

GIMA Ground Based Observatory (from all.xml/observatory/description/@short)

GIMA Ground Based Observatory (from Master/CDFglobalAttributes/Source_name)

Higher latitude chain (Lat 54.7, Long 246.7), Ground-based Vector Magnetic Field at Athabasca, Canada, 0.5 sec, CARISMA network

SPDF/CDAWeb. Please also acknowledge the data producer: I. Mann at U Alberta

SPDF/SSCWeb. Please also acknowledge the data producer: I. Mann at U Alberta

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: I. Mann at U Alberta

Higher latitude chain (Lat 67.9, Long 306.4), Ground-based Vector Magnetic Field at Attu, Greenland, 20 >sec, DMI network

DTU Space - National Space Institute, Denmark; Danish Meteorological Institute, Lyngbyvej 100, DK-2100 Copenhagen

Higher latitude chain (Lat 78.1, Long 14.2), Ground-based Vector Magnetic Field at Barentsburg, Russia. 1 min, AARI network

Barentsburg, Russia (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 41.4, Long 263.8), Ground-based Vector Magnetic Field at Bennington, NE, 0.5 sec, McMaC network, supported under NSF grant ATM-0245139

Higher latitude chain (Lat 66.9, Long 208.5), Ground-based Vector Magnetic Field at Bettles, AK, 1.0 sec, GIMA network

SPDF/CDAWeb. Please also acknowledge the data producer: D. Hampton at UAlaska, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: D. Hampton at UAlaska, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Hampton at UAlaska, NASA NAS5-02099

Higher latitude chain (Lat 55.6, Long 11.7), Ground-based Vector Magnetic Field at Brofelde, Denmark, 1 min, DTU network

Part of the Technical University of Denmark ground magnetometer network. 

Higher latitude chain (Lat 74.5, Long 19.0), Ground-based Vector Magnetic Field at Bjornoya, Norway, 1 min, Norwegian auroral zone magnetometer network

SPDF/CDAWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso N-9037, Tromso, Norway

SPDF/SSCWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso N-9037, Tromso, Norway

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso N-9037, Tromso, Norway

Higher latitude chain (Lat 64.3, Long 264.0), Ground-based Vector Magnetic Field at Baker Lake, Canada, 1.0 sec, NRCan Network

Part of the Geological Survey of Canada (Natural Resources Canada) ground magnetometer network.

The Canadian Magnetic Observatory Network (CANMON), maintained and operated by the Geological Survey of Canada, provided the data used in this study - http://www.geomag.nrcan.gc.ca.

Geomagnetic data are provided for your use and are not for sale or distribution by you to third parties, without the express written permission of the Geological Survey of Canada (GSC). Any report or publication that makes use of these data should acknowledge the Geological Survey of Canada as the source. One copy of each report or publication should be sent to the GSC.  We ask that the data not be used for commercial purposes, nor in any project in which you, your organization, or your collaborators are in a commercial agreement with any third party.  Commercial users may contact the Geological Survey of Canada.

SPDF/CDAWeb. Please also acknowledge the data producer: David Calp at Geological Survey of Canada

SPDF/SSCWeb. Please also acknowledge the data producer: David Calp at Geological Survey of Canada

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David Calp at Geological Survey of Canada

Lower latitude chain (Lat 46.2, Long 275.7), Ground-based Vector Magnetic Field at Bay Mills, MI, 0.5 sec, THEMIS GEONS network

Geomagnetic Event Observation Network by Students (GEONS),  part of the THEMIS EPO Effort.

Geomagnetic Event Observation Network by Students (GEONS) Magnetic Field Data Portal

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos & C. T. Russell at UCB & UCLA respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos & C. T. Russell at UCB & UCLA respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos & C. T. Russell at UCB & UCLA respectively, NASA NAS5-02099

Lower latitude chain (Lat 40.1, Long 254.8), Ground-based Vector Magnetic Field at Boulder, Colorado, 1 sec, USGS Network 

United States Geological Survey (USGS) Geomagnetism Program information can be found at

Access to preliminary data is provided as-is. We request that you acknowledge the USGS Geomagnetism Program in all published documents which make use of USGS data.

SPDF/CDAWeb. Please also acknowledge the data producer: Carol A. Finn at United States Geological Survey, 1711 Illinois St, Golden, CO 80401-1865, USA

SPDF/SSCWeb. Please also acknowledge the data producer: Carol A. Finn at United States Geological Survey, 1711 Illinois St, Golden, CO 80401-1865, USA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Carol A. Finn at United States Geological Survey, 1711 Illinois St, Golden, CO 80401-1865, USA

Lower latitude chain (Lat 47.8, Long 132.4), Ground-based Vector Magnetic Field at Baranov, Russia, 1 min, AARI network

Higher latitude chain (Lat 71.3, Long 203.4), Ground-based Vector Magnetic Field at Barrow, Alaska, 1.0 sec, USGS network

Access to the data is provided as-is, without any additional promises to respond quickly to outages, data quality, etc. We request that you acknowledge the USGS Geomagnetism Program in all published documents which make use of our data.

Lower latitude chain (Lat 30.4, Long 270.4), Ground-based Vector Magnetic Field at NASA , Stennis Space Center,  1 sec, USGS Network

NASA Stennis Space Center, MS (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 69.1, Long 255.0), Ground-based Vector Magnetic Field at Cambridge Bay, Canada, 1.0 sec, NRCan Network

Cambridge Bay, Canada (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 39.2, Long 240.2), Ground-based Vector Magnetic Field at Carson City, NV, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 64.2, Long 283.4), Ground-based Vector Magnetic Field at Dorset, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Augsburg College, Magnetometer for Cusp and Cleft Studies (MACCS) Magnetic Field Data Portal

Augsburg University Space Physics Magnetometer Array for Cusp and Cleft Studies (MACCS) program home page

Acknowledgement: Magnetometer data provided by: Dr. Erik Steinmetz, Augsburg College

SPDF/CDAWeb. Please also acknowledge the data producer: Erik S. Steinmetz at Magnetometer Array for Cusp and Cleft Studies (MACCS), Augsburg College, Dr. Erik Steinmetz. email: steinmee@augsburg.edu

SPDF/SSCWeb. Please also acknowledge the data producer: Erik S. Steinmetz at Magnetometer Array for Cusp and Cleft Studies (MACCS), Augsburg College, Dr. Erik Steinmetz. email: steinmee@augsburg.edu

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Erik S. Steinmetz at Magnetometer Array for Cusp and Cleft Studies (MACCS), Augsburg College, Dr. Erik Steinmetz. email: steinmee@augsburg.edu

Cape Dorset, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 49.8, Long 285.6), Ground-based Vector Magnetic Field at Chibougamau, Canada, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 64.2, Long 276.7), Ground-based Vector Magnetic Field at Coral Harbour, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS); NOTE: no data from 2013 to 2018

Coral Harbour, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 64.9, Long 212.1), Ground-based Vector Magnetic Field at College, AK, 0.5 sec, GIMA network

Higher latitude chain (Lat 64.9, Long 212.1),  Ground-based Vector Magnetic Field at Fairbanks, College, Alaska, 1.0 sec, USGS network

Fairbanks, AlaskaCollege (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 36.3, Long 263.2), Ground-based Vector Magnetic Field at Pawnee, Colorado, 1 sec time Resolution.

Computational Physics, Inc, University of Colorado, Boulder, GIC Magnetics

Acknowledgement: Magnetometer data provided by: Computational Physics, Inc, University of Colorado, Boulder, GIC Magnetics

SPDF/CDAWeb. Please also acknowledge the data producer: Jennifer Gannon, Delores Knipp, Mike Henderson at Computational Physics, Inc, University of Colorado, Boulder, GIC Magnetics.

SPDF/SSCWeb. Please also acknowledge the data producer: Jennifer Gannon, Delores Knipp, Mike Henderson at Computational Physics, Inc, University of Colorado, Boulder, GIC Magnetics.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Jennifer Gannon, Delores Knipp, Mike Henderson at Computational Physics, Inc, University of Colorado, Boulder, GIC Magnetics.

Counts based on variable 'thg_mag_col_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/col/2021/thg_l2_mag_col_20210727_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 20993 timesteps. 

MagStar Ground Based Observatory (from all.xml/observatory/description/@short)

MagStar Ground Based Observatory (from Master/CDFglobalAttributes/Source_name)

Higher latitude chain (Lat 70.5, Long 291.4), Ground-based Vector Magnetic Field at Clyde River, Nunavut, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Clyde River, Nunavut, Canada (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 44.3, Long 286.4), Ground-based Vector Magnetic Field at Lewis, NY, 1 sec time Resolution.

Counts based on variable 'thg_mag_dat_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dat/2021/thg_l2_mag_dat_20210201_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9921% of the 25158 timesteps. 

Lower latitude chain (Lat 40.0, Long 209.7), Ground-based Vector Magnetic Field at University of Colorado, 1 sec time Resolution.

Counts based on variable 'thg_mag_dbo_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dbo/2019/thg_l2_mag_dbo_20191105_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9506% of the 14177 timesteps. 

University of Colorado, Boulder (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 41.7, Long 287.2), Ground-based Vector Magnetic Field at New Britain, CT, 1 sec time Resolution.

Counts based on variable 'thg_mag_dct_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dct/2021/thg_l2_mag_dct_20210309_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 1048 timesteps. 

Higher latitude chain (Lat 70.4, Long 211.2), Ground-based Vector Magnetic Field at Dead Horse, Alaska, 1.0 sec, USGS network

Lower latitude chain (Lat 40.2, Long 256.3), Ground-based Vector Magnetic Field at Hennepin, MN, 1 sec time Resolution.

Counts based on variable 'thg_mag_dhe_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dhe/2020/thg_l2_mag_dhe_20200803_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 41 timesteps. 

Higher latitude chain (Lat 73.5, Long 80.7), Ground-based Vector Magnetic Field at Dikson, Russia, 1 min, AARI network

Lower latitude chain (Lat 42.6, Long 288.5), Ground-based Vector Magnetic Field at Haystack Observatory, MIT, 1 sec time Resolution.

Counts based on variable 'thg_mag_dma_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dma/2021/thg_l2_mag_dma_20210312_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9933% of the 29667 timesteps. 

Haystack Observatory MIT (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 44.3, Long 290.2), Ground-based Vector Magnetic Field at Augusta, ME, 1 sec time Resolution.

Counts based on variable 'thg_mag_dme_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dme/2021/thg_l2_mag_dme_20210615_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9284% of the 1395 timesteps. 

Higher latitude chain (Lat 76.8, Long 341.4), Ground-based Vector Magnetic Field at Danmarkshavn, Greenland, 20 sec, DMI network

Danmarkshavn, Greenland (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 39.9, Long 267.7), Ground-based Vector Magnetic Field at University of Missouri, 1 sec time Resolution.

Counts based on variable 'thg_mag_dmo_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dmo/2022/thg_l2_mag_dmo_20220217_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for all 86399 timesteps. 

University of Missouri, Missouri (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 74.3, Long 339.8), Ground-based Vector Magnetic Field at Daneborg, Greenland, 20 sec, DMI network

Danish Meteorological Institute, Lyngbyvej 100, DK-2100 Copenhagen

Daneborg, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 62.1, Long 9.1), Ground-based Vector Magnetic Field at Dombas, Norway, 1 min, Norwegian auroral zone magnetometer network

Part of the Tromso Geophysical Observatory ground magnetometer network. 

SPDF/CDAWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso, N-9037 Tromso, Norway

SPDF/SSCWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso, N-9037 Tromso, Norway

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso, N-9037 Tromso, Norway

Lower latitude chain (Lat 41.6, Long 275.9), Ground-based Vector Magnetic Field at Wauseon, OH, 1 sec time Resolution.

Counts based on variable 'thg_mag_doh_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/doh/2020/thg_l2_mag_doh_20200803_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 93.8776% of the 46 timesteps. 

Blue Skies, Wauseon, OH (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 66.1, Long 12.5), Ground-based Vector Magnetic Field at Donna, Norway, 1 min, Norwegian auroral zone magnetometer network

SPDF/CDAWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso,  N-9037 Tromso, Norway

SPDF/SSCWeb. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso,  N-9037 Tromso, Norway

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Truls Lynne Hansen at Tromso Geophysical Observatory Faculty of Science University of Tromso,  N-9037 Tromso, Norway

Lower latitude chain (Lat 45.0, Long 287.9), Ground-based Vector Magnetic Field at Derby, VT, 0.5 sec, THEMIS GEONS network

Lower latitude chain (Lat 47.1, Long 266.3), Ground-based Vector Magnetic Field at Sugar Hills, MN, 1 sec time Resolution.

Counts based on variable 'thg_mag_dsh_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dsh/2020/thg_l2_mag_dsh_20200703_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.6471% of the 378 timesteps. 

Lower latitude chain (Lat 31.8, Long 257.6), Ground-based Vector Magnetic Field at Odessa, TX, 1 sec time Resolution.

Counts based on variable 'thg_mag_dtx_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dtx/2020/thg_l2_mag_dtx_20200825_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.0984% of the 711 timesteps. 

Higher latitude chain (Lat 38.7, Long 287.2), Ground-based Vector Magnetic Field at Warrenton, VA, 1 sec time Resolution.

Counts based on variable 'thg_mag_dva_time' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/themis/thg/l2/mag/dva/2020/thg_l2_mag_dva_20200628_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.9802% of the 20169 timesteps. 

Warrenton, Virginia (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 64.8, Long 218.8), Ground-based Vector Magnetic Field at Eagle, AK, 0.5 sec, GIMA network

GIMA Ground Based Observatories. Data served as part of the THEMIS GBO effort

Higher latitude chain (Lat 64.7, Long 249.3), Ground-based Vector Magnetic Field at Ekati, Canada, 0.5 sec, THEMIS GBO network

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos & I. Mann at UCB & U Calgary respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos & I. Mann at UCB & U Calgary respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos & I. Mann at UCB & U Calgary respectively, NASA NAS5-02099

Higher latitude chain (Lat 58.8, Long 265.9), Ground-based Vector Magnetic Field at Fort Churchill, Canada, 1.0 sec, NRCan Network 

Data provided via the Canadian Magnetic Observatory System (CANMOS), maintained and operated by Natural Resources Canada (NRCAN)

SPDF/CDAWeb. Please also acknowledge the data producer: David Calp at Geological Survey of Canada Geomagnetic Laboratory 7 Observatory Crescent Ottawa, Ontario, Canada K1A 0Y3

SPDF/SSCWeb. Please also acknowledge the data producer: David Calp at Geological Survey of Canada Geomagnetic Laboratory 7 Observatory Crescent Ottawa, Ontario, Canada K1A 0Y3

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David Calp at Geological Survey of Canada Geomagnetic Laboratory 7 Observatory Crescent Ottawa, Ontario, Canada K1A 0Y3

Fort Churchill, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 62.0, Long 310.3), Ground-based Vector Magnetic Field at Paamiut(Frederikshap), Greenland, 1 min, DTU network

Part of the Technical University of Denmark ground magnetometer network.   

Lower latitude chain (Lat 38.2, Long 282.6), Ground-based Vector Magnetic Field at Corbin, VA, 1 sec, USGS Network

Lower latitude chain (Lat 37.1, Long 240.3), Ground-based Vector Magnetic Field at Fresno, Californaia, 1 sec, USGS Network

Higher latitude chain (Lat 61.8, Long 238.8), Ground-based Vector Magnetic Field at Fort Simpson, Canada, 0.5 sec, CARISMA network

Fort Simpson, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 56.3, Long 239.2), Ground-based Vector Magnetic Field at Fort St., John, BC, Canada, 1.0 sec STEP Polar Network, available through AUTUMN network

Original data provided by the STEP Polar Network and Dr. Kanji Hayashi

Access to the data is provided as-is. We request you acknowledge STEP Polar Network and Dr. Hayashi in all published documents which make use of this data.

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Kanji Hayashi at Step Polar Network, available through AUTUMN, network Univ Athabasca

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Kanji Hayashi at Step Polar Network, available through AUTUMN, network Univ Athabasca

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Kanji Hayashi at Step Polar Network, available through AUTUMN, network Univ Athabasca

Fort St.John, BC, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 60.0, Long 248.2), Ground-based Vector Magnetic Field at Fort Smith, Canada, 0.5 sec, CARISMA network

Higher latitude chain (Lat 58.9, Long 237.2), Ground-based Vector Magnetic Field at Fort Nelson, BC, Canada, 1.0 sec, STEP Polar Network

Original data provided by the STEP Polar Network and Dr. Kanji Hayashi, IAGA2002 format data provided AUTUMN network at University Athabasca.

Access to the data is provided as-is. We request you acknowledge STEP Polar Network and Dr. Hayashi as well as the AUTUMN network at the Univ Athabasca in all published documents which make use of this data.

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Kanji Hayashi at Step Polar Network

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Kanji Hayashi at Step Polar Network

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Kanji Hayashi at Step Polar Network

Fort Nelson, BC, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 66.6, Long 214.8), Ground-based Vector Magnetic Field at Fort Yukon, AK, 0.5 sec,  GIMA network

Lower latitude chain (Lat 46.1, Long 259.4), Ground-based Vector Magnetic Field at Fort Yates, ND, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 62.4, Long 214.8), Ground-based Vector Magnetic Field at Gakona, AK, 1.0 sec, GIMA network

Higher latitude chain (Lat 53.3, Long 299.5), Ground-based Vector Magnetic Field at Goose Bay, Canada, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 69.3, Long 306.5), Ground-based Vector Magnetic Field at Qeqertarsuaq, Greenland, 1 min, DTU network

SPDF/CDAWeb. Please also acknowledge the data producer: R. Behlke and A.N. Willer at DTU Space - National Sapce Institute, Denmark

SPDF/SSCWeb. Please also acknowledge the data producer: R. Behlke and A.N. Willer at DTU Space - National Sapce Institute, Denmark

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Behlke and A.N. Willer at DTU Space - National Sapce Institute, Denmark

Qeqertarsuaq, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 64.2, Long 308.3), Ground-based Vector Magnetic Field at Nuuk(Godthap), Greenland 1 min, DTU network

Part of the Technical University of Denmark ground magnetometer network.  

Higher latitude chain (Lat 56.4, Long 265.3), Ground-based Vector Magnetic Field at Gillam, Canada, 0.5 sec Level-2, CARISMA network

Higher latitude chain (Lat 68.6, Long 264.1), Ground-based Vector Magnetic Field at Gjoa Haven, Nunavut, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Gjoa Haven, Nunavut, Canada (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 46.9, Long 263.5), Ground-based Vector Magnetic Field at Glyndon, MN, 0.5 sec, McMaC network, supported under NSF grant ATM-0245139

Lower latitude chain (Lat 13.6, Long 144.9), Ground-based Vector Magnetic Field at Dededo, Guam, 1 sec, USGS Network

Higher latitude chain (Lat 62.3, Long 26.6), Ground-based Vector Magnetic Field at Hankasalmi, Finland, 10 sec, IMAGE network

Original data provided by the Finnish Meteorological Institute (FMI).

SPDF/CDAWeb. Please also acknowledge the data producer: Liisa Juusola at Finnish Meteorological Institute P.O. Box 503, FI-00101 Helsinki, Finland

SPDF/SSCWeb. Please also acknowledge the data producer: Liisa Juusola at Finnish Meteorological Institute P.O. Box 503, FI-00101 Helsinki, Finland

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Liisa Juusola at Finnish Meteorological Institute P.O. Box 503, FI-00101 Helsinki, Finland

Hankasalmi, Finland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 61.2, Long 210.1), Ground-based Vector Magnetic Field at Anchorage, AK, 0.5 sec, GIMA network

Higher latitude chain (Lat 59.7, Long 209.5), Ground-based Vector Magnetic Field at Homer, AK, 0.5 sec, GIMA network

Lower latitude chain (Lat 21.3, Long 202.0), Ground-based Vector Magnetic Field at Ewa Beach, HI, 1 sec, USGS Network

Higher latitude chain (Lat 76.5, Long 25.0), Ground-based Vector Magnetic Field at Hopen, Norway 1 min, Norwegian auroral zone magnetometer network

Lower latitude chain (Lat 47.6, Long 245.3), Ground-based Vector Magnetic Field at Hot Springs, MT, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 61.5, Long 353.2), Ground-based Vector Magnetic Field at Hov, Faroe Islands, Denmark, 1 min 

Hov Faroe Islands, Denmark (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 45.6, Long 267.0), Ground-based Vector Magnetic Field at Hrisis, Minnesota, 0.5 sec, Falcon network

SPDF/CDAWeb. Please also acknowledge the data producer: P. Chi at USAF Academy, UCLA

SPDF/SSCWeb. Please also acknowledge the data producer: P. Chi at USAF Academy, UCLA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: P. Chi at USAF Academy, UCLA

FALCON - Ground Based Observatory (from all.xml/observatory/description/@short)

FALCON - Ground Based Observatory (from Master/CDFglobalAttributes/Source_name)

Higher latitude chain (Lat 49.2, Long 275.3), Ground-based Vector Magnetic Field at Hornepayne, Ont, Canada, 1.0 sec, STEP Polar Network

Hornepayne, Ont, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 69.3, Long 278.2), Ground-based Vector Magnetic Field at Igloolik, Nunavut, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Igloolik, Nunavut, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 58.5, Long 281.9), Ground-based Vector Magnetic Field at Inukjuak, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Calibration files at https://autumn.athabascau.ca/themis.gbo.mag.calibration

Higher latitude chain (Lat 68.4, Long 226.2), Ground-based Vector Magnetic Field at Inuvik, Canada, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 63.8, Long 291.5), Ground-based Vector Magnetic Field at Iqaluit, Canada, 1.0 sec, NRCan Network

Higher latitude chain (Lat 68.6, Long 27.3), Ground-based Vector Magnetic Field at Ivalo, Finland, 10 sec, IMAGE network

Higher latitude chain (Lat 70.9, Long 351.3), Ground-based Vector Magnetic Field at Jan Mayen, Norway,1 min, Norwegian auroral zone magnetometer network

The geomagnetic information available at our web-pages is primarily intended for the non-commercial scientific community, educational purposes, and the general public. Commercial users of our services are urged to contact us to esjanlish an agreement of use. As part of an agreement we normally offer to construct exclusive web-pages specifically for the application in question. We accept no liability for loss or damages of any kind resulting from this or from errors or inaccuracies in the data.

Higher latitude chain (Lat 66.4, Long 17.0), Ground-based Vector Magnetic Field at Jackvik, Sweden, 1 min, Norwegian auroral zone magnetometer network

Part of the Tromso Geophysical Observatory ground magnetometer network

Higher latitude chain (Lat 70.1, Long 217.4), Ground-based Vector Magnetic Field at Kaktovik, AK, 0.5 sec, GIMA network

Higher latitude chain (lat 49.4, long 277.7), ground-based vector Magnetic field at Kapuskasing, Canada, 0.5 sec, THEMIS GBO network

Kapuskasing, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 59.2, Long 5.2), Ground-based Vector Magnetic Field at Karmoy, Norway 1 min, Norwegian auroral zone magnetometer network

Part of the Tromso Geophysical Observatory ground magnetometer network.

Higher latitude chain (Lat 60.6, Long 208.7), Ground-based Vector Magnetic Field at Kaktovik, AK, 1.0 sec, GIMA network 

Higher latitude chain (Lat 69.8, Long 27.0), Ground-based Vector Magnetic Field at Kevo, Finland, 10 sec, IMAGE network 

Higher latitude chain (Lat 67.0, Long 199.6), Ground-based Vector Magnetic Field at Kiana, AK, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 69.1, Long 20.8), Ground-based Vector Magnetic Field at Kilpisjarvi, Finland, 10 sec, IMAGE network

Kilpisjarvi, Finland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 55.3, Long 282.2), Ground-based Vector Magnetic Field at Kuujjuarapik, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Kuujjuarapik, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 57.8, Long 207.6), Ground-based Vector Magnetic Field at Kodkak, Alaska, 0.5 sec, Falcon network

Higher latitude chain (Lat 58.3, Long 291.8), Ground-based Vector Magnetic Field at Kuujjuaq, Canada, 0.5 sec, THEMIS GBO network

SPDF/CDAWeb. Please also acknowledge the data producer: V. Angelopoulos & C.T. Russell at UCB & UCLA Respectively, NASA NAS5-02099

SPDF/SSCWeb. Please also acknowledge the data producer: V. Angelopoulos & C.T. Russell at UCB & UCLA Respectively, NASA NAS5-02099

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: V. Angelopoulos & C.T. Russell at UCB & UCLA Respectively, NASA NAS5-02099

Higher latitude chain (Lat 74.6, Long 302.8), Ground-based Vector Magnetic Field at Kullorsuaq, Greenland, 1 min, DTU network

Kullorsuaq, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 55.2, Long 254.7), Ground-based Vector Magnetic Field at  La Ronge, Saskatchewan, Canada, 0.5 sec, AUTUMN network

Higher latitude chain (Lat 51.0, Long 252.9), Ground-based Vector Magnetic Field at Lucky Lake, Sask, Canada, 1.0 sec, STEP Polar Network

Lucky Lake, Sask, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 49.6, Long 247.1), Ground-based Vector Magnetic Field at Lethbridge, Alberta, Canada, 0.5 sec, AUTUMN network

Lower latitude chain (Lat 40.2, Long 281.6), Ground-based Vector Magnetic Field at Loysburg  PA, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 68.0, Long 35.0), Ground-based Vector Magnetic Field at Lovozero, Russia, 1 min, AARI network

Lower latitude chain (Lat 39.1, Long 283.2), Ground-based Vector Magnetic Field at Lrelel, Maryland, 0.5 sec, Falcon network

Lower latitude chain (Lat 24.8, Long 260.4), Ground-based Vector Magnetic Field at Linares, Mexico, 0.5 sec, McMac network, supported under NSF grant ATM-0245139

Higher latitude chain (Lat 55.2, Long 254.7), Ground-based Vector Magnetic Field at LaRonge Sask, Canada, 1.0 sec, STEP Polar Network

LaRonge, Sask, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 64.2, Long 338.3), Ground-based Vector Magnetic Field at Leirvogur, Iceland, 10 second resolution data.

Ground based observatory, affiliated with Science Institute, University of Iceland. Data is preliminary 10 second resolution data. 

Leirvogur Magnetic Observatory, Science Institute, University of Iceland

SPDF/CDAWeb. Please also acknowledge the data producer: Gunnlaugur Bjornsson at Science Institute, University of Iceland, Reykjavik, Iceland

SPDF/SSCWeb. Please also acknowledge the data producer: Gunnlaugur Bjornsson at Science Institute, University of Iceland, Reykjavik, Iceland

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Gunnlaugur Bjornsson at Science Institute, University of Iceland, Reykjavik, Iceland

Lower latitude chain (Lat 26.4, Long 262.2), Ground-based Vector Magnetic Field at Lyford, TX, 0.5 sec, McMaC network, supported under NSF grant ATM-024513

Higher latitude chain (Lat 78.2, Long 15.8), Ground-based Vector Magnetic Field at Longyearbyen, Norway, 1 min, Norwegian auroral zone magnetometer network 

Longyearbyen, Norway (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 69.5, Long 23.7), Ground-based Vector Magnetic Field at Masi, Finland, 10 sec, IMAGE network

Higher latitude chain (Lat 63.0, Long 204.4), Ground-based Vector Magnetic Field at McGrath, AK, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 54.6, Long 246.7), Ground-based Vector Magnetic Field at Meanook, Canada, 1.0 sec, NRCan Network

Higher latitude chain (Lat 62.8, Long 31.0), Ground-based Vector Magnetic Field at Mekrijarvi, Finland, 10 sec, IMAGE network

Mekrijarvi, Finland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 68.0, Long 23.5), Ground-based Vector Magnetic Field at Muono, Finland, 10 sec, IMAGE network 

Higher latitude chain (Lat 56.4, Long 298.3 ), Ground-based Vector Magnetic Field at Nain, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Higher latitude chain (Lat 79.0, Long 11.9), Ground-based Vector Magnetic Field at Ny Alesund, Norway, 1 min, Norwegian auroral zone magnetometer network

Higher latitude chain (Lat 61.2, Long 314.6), Ground-based Vector Magnetic Field at Narsarsuaq, Greenland, 1 min, DTU network

Narsarsuaq, Greenland (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 48.3, Long 242.9),  Ground-based Vector Magnetic Field at Colville, National Forest, WA, 1 sec, USGS Network

Colville National Forest, Washington (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 71.1, Long 25.8), Ground-based Vector Magnetic Field at Nordkapp, Norway, 1 min, Norwegian auroral zone magnetometer network

Higher latitude chain (Lat 81.6, Long 343.3), Ground-based Vector Magnetic Field at Nord, Greenland, 20 sec, DMI network

Higher latitude chain (Lat 61.2, Long 314.6), Ground-based Vector Magnetic Field at Narsarsuaq, Greenland, 20 sec, THEMIS GBO network

SPDF/CDAWeb. Please also acknowledge the data producer: Hans Gleisner at DMI, Denmark

SPDF/SSCWeb. Please also acknowledge the data producer: Hans Gleisner at DMI, Denmark

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Hans Gleisner at DMI, Denmark

Higher latitude chain (Lat 60.5, Long 24.7), Ground-based Vector Magnetic Field at Nurmijarvi, Finland, 10 sec, IMAGE network

Nurmijarvi, Finland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 45.4, Long 284.4), Ground-based Vector Magnetic Field at Ottawa, Canada, 1.0 sec, NRCan Network

Higher latitude chain (Lat 64.5, Long 27.2), Ground-based Vector Magnetic Field at Oulujarvi, Finland, 10 sec, IMAGE network

Higher latitude chain (Lat 66.1, Long 294.2), Ground-based Vector Magnetic Field at Pangnirtung, Nunavut, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Pangnirtung, Nunavut, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 70.1, Long 170.9), Ground-based Vector Magnetic Field at Pevek, Russia, 1 min, AARI network

Lower latitude chain (Lat 38.3, Long 255.4), Ground-based Vector Magnetic Field at Pblolo, Colorado, 0.5 sec, Falcon network

Lower latitude chain (Lat 35.0, Long 262.8), Ground-based Vector Magnetic Field at Purcell, OK, 0.5 sec McMaC network, supported under NSF grant ATM-0245139

Higher latitude chain (Lat 66.9, Long 24.1), Ground-based Vector Magnetic Field at Pello, Finland, 10 sec, IMAGE network

Higher latitude chain (Lat -83.7, Long 88.7), Ground-based Vector Magnetic Field in Antarctica, 1-sec, raw data. Instrument deployed in Dec 2014 under NSF awards ANT0839858, ATM922979

Polar Experimental Network for Geospace Upper atmosphere Investigations (PENGUIn) Ground Based Observatory.

This effort is supported by the National Science Foundation throught the following awards: ANT0839858, ATM922979 (Virginia Tech), and ANT0838861 (University of Michigan).

SPDF/CDAWeb. Please also acknowledge the data producer: C. R. Clauer at Virginia Tech.

SPDF/SSCWeb. Please also acknowledge the data producer: C. R. Clauer at Virginia Tech.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: C. R. Clauer at Virginia Tech.

PENGUIn 40 degree magnetic meridian chain ground based observatory (from all.xml/observatory/description/@short)

PEUNGUIn-0, Antarctia, at -83.670, 88.681 (from all.xml/instrument/description/@short)

PENGUIn 40 degree magnetic meridian chain ground based observatory (from Master/CDFglobalAttributes/Source_name)

Higher latitude chain (Lat -84.5, Long 77.2), Ground-based Vector Magnetic Field in Antarctica, 1-sec raw data. Station deployed Jan 2008 under NSF award ATM-922979

PEUNGUIn-1, Antarctia, at -85.50,77.20 (from all.xml/instrument/description/@short)

Higher latitude chain (Lat -84.4, Long 58.0), Ground-based Vector Magnetic Field in Antarctica, 1-sec raw data. Station deployed Jan 2009, redeployed Dec 2012 under NSF award PLR-1243390 and ATM-922979

PEUNGUIn-2, Antarctia, at -84.42, 57.96 (from all.xml/instrument/description/@short)

Higher latitude chain (Lat -84.8, Long 37.6), Ground-based Vector Magnetic Field in Antarctica, 1-sec raw data. Station deployed Jan 2013 under NSF awards PLR-1243390 and ATM-922979

PEUNGUIn-2, Antarctia, at -84.81, 37.63 (from all.xml/instrument/description/@short)

Higher latitude chain (Lat -83.3, Long 12.3), Ground-based Vector Magnetic Field in Antarctica, 1-sec raw data. Station deployed Jan 2014 under NSF awards PLR-1243390 and ATM-922979

PEUNGUIn-4, Antarctia, at -83.34, 12.25 (from all.xml/instrument/description/@short)

Higher latitude chain (Lat -83.7, Long 88.7), Ground-based Vector Magnetic Field at PG5 site in Antarctica, 1-sec raw data. Instrument deployed in Jan 2016 under NSF awards ANT0839858, ATM922979

PEUNGUIn-5, Antarctia, at -81.96,  5.71 (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 53.8, Long 237.2), Ground-based Vector Magnetic Field at Prince George Canada, 0.5 sec, THEMIS GBO network

Prince George Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 50.2, Long 263.9), Ground-based Vector Magnetic Field at Pinawa, Canada, 0.5 sec, CARISMA network

Lower latitude chain (Lat 43.1, Long 257.4), Ground-based Vector Magnetic Field at Pine Ridge, SD, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 52.5, Long 252.8), Ground-based Vector Magnetic Field at Parksite Sask, Canada, 1.0 sec, STEP Polar Network

ParkSite, Sask, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 65.1, Long 212.6), Ground-based Vector Magnetic Field at Poker Flat, AK, 0.5 sec, GIMA network

Higher latitude chain (Lat 56.8, Long 226.8), Ground-based Vector Magnetic Field at Petersburg, AK, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 60.1, Long 282.7), Ground-based Vector Magnetic Field at Puvirnituq, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Higher latitude chain (Lat 53.8, Long 282.4), Ground-based Vector Magnetic Field at Radisson, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Higher latitude chain (Lat 65.9, Long 26.4), Ground-based Vector Magnetic Field at Ranua, Finland, 10 sec, IMAGE network 

Higher latitude chain (Lat 62.8, Long 267.9), Ground-based Vector Magnetic Field at Rankin Inlet, Canada, 0.5 sec, CARISMA network

Rankin Inlet, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 66.5, Long 273.8), Ground-based Vector Magnetic Field at Repulse Bay, Canada, 0.5 sec, Magnetometer Array for Cusp and Cleft Studies (MACCS)

Repulse Bay, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 52.1, Long 246.2), Ground-based Vector Magnetic Field at Red Deer, Alberta, Canada, 0.5 sec, AUTUMN network

Red Deer, Alberta, Canada (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 33.0, Long 263.2), Ground-based Vector Magnetic Field at Richardson, TX, 0.5 sec, McMac network, supported under NSF grant ATM-0245139

Lower latitude chain (Lat 43.6, Long 274.8), Ground-based Vector Magnetic Field at Remus, MI, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 55.2, Long 8.6), Ground-based Vector Magnetic Field at Roemoe, Denmark, 1 min, DTU network

Higher latitude chain (Lat 50.9, Long 245.7), Ground-based Vector Magnetic Field at Priddis, Alberta, Canada, 0.5 sec, AUTUMN network

Priddis, Alberta, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 64.9, Long 11.0), Ground-based Vector Magnetic Field at Rorvik, Norway, 1 min, Norwegian auroral zone magnetometer network

Higher latitude chain (Lat 62.2, Long 284.3), Ground-based Vector Magnetic Field at Salluit, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Lower latitude chain (Lat 29.4, Long 261.4), Ground-based Vector Magnetic Field at SanAntonio, TX, 0.5 sec, McMaC network, supported under NSF grant ATM-0245139

Higher latitude chain (Lat 54.8, Long 293.2), Ground-based Vector Magnetic at Schefferville, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Schefferville, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 70.4, Long 338.0), Ground-based Vector Magnetic Field at Ittoqqortoormiit, Greenland, 60 sec, DTU network

Ittoqqortoormiit, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 50.2, Long 293.7), Ground-based Vector Magnetic Field at Sept Iles, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Higher latitude chain (Lat 55.4, Long 199.5), Ground-based Vector Magnetic Field at Sand Point, Alaska, 1.0 sec, USGS network

Higher latitude chain (Lat 57.1, Long 224.7), Ground-based Vector Magnetic Field at Sitka, Alaska, 1.0 sec, USGS network

Lower latitude chain (Lat 18.1, Long 293.8), Ground-based Vector Magnetic Field at Cayey, Puerto Rico, 1 sec, USGS Network

Higher latitude chain (Lat 65.4, Long 307.1), Ground-based Vector Magnetic Field at Maniitsoq, Greenland, 1, DTU network

Maniitsoq, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 63.6, Long 249.1), Ground-based Vector Magnetic Field at Snap Lake, Canada, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 56.5, Long 280.8), Ground-based Vector Magnetic Field at Sanikiluaq, Canada, 0.5 sec, CARISMA network

Higher latitude chain (Lat 61.1, Long 4.8), Ground-based Vector Magnetic Field at Solund, Norway 1 min, Norwegian auroral zone magnetometer network

Higher latitude chain (Lat 70.5, Long 22.2), Ground-based Vector Magnetic Field at Soroya Norway, 1 min, Norwegian auroral zone magnetometer network

Part of the Tromso Geophysical Observatory ground magnetometer network.  

Higher latitude chain (Lat 67.0, Long 309.3), Ground-based Vector Magnetic Field at Kangerlussuaq, Greenland, 1 min, DTU network

Kangerlussuaq, Greenland (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 37.4, Long 237.8), Magnetic Field at Stanford, California, 0.5 sec, Falcon network

Stfdford, California (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 48.7, Long 287.6), Ground-based Vector Magnetic Field at Saint-Felicien, Quebec, Canada, 0.5 sec, AUTUMNX network, Canadian Space Agency GO program and Athabasca University

Saint-Felicien, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 47.6, Long 307.3), Ground-based Vector Magnetic Field at St.John Newfoundland, 1.0 sec, NRCan Network

St. John, Newfoundland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 72.3, Long 321.7), Ground-based Vector Magnetic Field at Summit, Greenland, Ice Cap, 1 min, DTU network (Previously operated by Virginia Tech)

Higher latitude chain (Lat 76.0, Long 294.9), Ground-based Vector Magnetic Field at Savissivik, Greenland, 20 sec, DMI network

Savissivik, Greenland (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 44.8, Long 271.4), Ground-based Vector Magnetic Field at Shawano, WI, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 76.5, Long 291.2), Ground-based Vector Magnetic Field at Thule Air Base, Greenland, 1 min, DTU network

Thule Air Base, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 58.3, Long 26.5), Ground-based Vector Magnetic Field at Tartu, Estonia, 10 sec, IMAGE network

Lower latitude chain (Lat -37.1, Long 347.7), Ground-based Vector Magnetic Field at Tristan Da Cunha, 1 min, DTU network

Part of the Technical University of Denmark ground magnetometer network  

Higher latitude chain (Lat 77.5, Long 290.8), Ground-based Vector Magnetic Field at Qaanaaq, Greenland, 1 min, DTU network

Higher latitude chain (Lat 71.6, Long 128.9), Ground-based Vector Magnetic Field at Tiksi, Russia, 1 min, AARI network

Higher latitude chain (Lat 66.6, Long 210.4), Ground-based Vector Magnetic Field at Toolik Lake, AK, 1.0 sec, GIMA network

GIMA observatoies - Data served as part of the THEMIS GBO effort

SPDF/CDAWeb. Please also acknowledge the data producer: D. Hampton at Geophysical Institute, University of Alaska Fairbanks

SPDF/SSCWeb. Please also acknowledge the data producer: D. Hampton at Geophysical Institute, University of Alaska Fairbanks

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Hampton at Geophysical Institute, University of Alaska Fairbanks

Higher latitude chain (Lat 54.0, Long 259.1), Ground-based Vector Magnetic Field at Flin Flon/The Pas, Canada, 0.5 sec, THEMIS GBO network

Higher latitude chain (Lat 62.3, Long 209.8), Ground-based Vector Magnetic Field at Trapper Creek, AK, 0.5 sec, GIMA network

Higher latitude chain (Lat 69.7, Long 18.9), Ground-based Vector Magnetic Field at Tromso, Norway, 1 min, Norwegian auroral zone magnetometer network

Lower latitude chain (Lat 32.2, Long 249.3), Ground-based Vector Magnetic Field at Tucson, Arizona, 1 sec, USGS Network

Lower latitude chain (Lat 45.1, Long 241.1), Ground-based Vector Magnetic Field at Ukiah, OR, 0.5 sec, THEMIS GEONS network

Higher latitude chain (Lat 70.7, Long 307.9), Ground-based Vector Magnetic Field at Uummannaq, Greenland, 1 min, DTU network

Uummannaq, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 72.8, Long 303.8), Ground-based Vector Magnetic Field at Upernavik, Greenland, 1 min., DTU network

Upernavik, Greenland (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 48.5, Long 236.6), Ground-based Vector Magnetic Field at Victoria, Canada, 1.0 sec, NRCan Network

Higher latitude chain (Lat 79.3, Long 76.5), Ground-based Vector Magnetic Field at Vize Island, Russia, 1 min, AARI network

Vize Island, Russia (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 48.2, Long 282.2), Ground-based Vector Magnetic Field at Val-d'Or, Quebec, Canada, 0.5 sec, AUTUMN network.

Higher latitude chain (Lat 61.0, Long 224.8), Ground-based Vector Magnetic Field at White Horse, Canada, 0.5 sec, THEMIS GBO network

White Horse, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 60.7, Long 224.9), Ground-based Vector Magnetic Field at WhiteHorse YT, Canada, 1.0 sec time Resolution. 

WhiteHorse, YT, Canada (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 37.9, Long 284.6), Ground-based Vector Magnetic Field at Wlpsops Island, Virginia, 0.5 sec,Falcon network

Wlpsops Island, Virginia (from all.xml/instrument/description/@short)

Lower latitude chain (Lat 43.6, Long 264.4), Ground-based Vector Magnetic Field at Worthington, MN, 0.5 sec, McMaC network, supported under NSF grant ATM-0245139

Higher latitude chain (Lat 62.5, Long 245.5), Ground-based Vector Magnetic Field at  Yellowknife, Canada, 1.0 sec, NRCan Network

SPDF/CDAWeb. Please also acknowledge the data producer: David Calp at Geological Survey of Canada (GSC) Geomagnetic Laboratory 7 Observatory Crescent Ottawa, Ontario, Canada K1A 0Y3

SPDF/SSCWeb. Please also acknowledge the data producer: David Calp at Geological Survey of Canada (GSC) Geomagnetic Laboratory 7 Observatory Crescent Ottawa, Ontario, Canada K1A 0Y3

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David Calp at Geological Survey of Canada (GSC) Geomagnetic Laboratory 7 Observatory Crescent Ottawa, Ontario, Canada K1A 0Y3

Yellowknife, Canada (from all.xml/instrument/description/@short)

Higher latitude chain (Lat 62.5, Long 245.7), Ground-based Vector Magnetic Field at Yellowknife, Canada, 0.5 sec, THEMIS GBO network

SPDF/CDAWeb. Please also acknowledge the data producer: Andrew Christensen at Aerospace

SPDF/SSCWeb. Please also acknowledge the data producer: Andrew Christensen at Aerospace

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Andrew Christensen at Aerospace

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/guvi/levels_v10/level2b_e/edp/cdf/2002/01/timed_edp_guvi_20020107055328_v01.cdf. The most common cadence, 15000 [ms] = PT15S, occurred for 98.1132% of the 104 timesteps. 

Global UltraViolet Imager (from all.xml/instrument/description/@short)

Volume emission rate (no mutual neutralization correction) for 23 channels

Geomagnetic (simple dipole) Latitude of profile [registered at ~300km]

IR Radiances in 10 channels (1.27 to 17ym) from 0 to 150 km, Version 1.07, 

SPDF/CDAWeb. Please also acknowledge the data producer: James Russell III at Hampton University

SPDF/SSCWeb. Please also acknowledge the data producer: James Russell III at Hampton University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: James Russell III at Hampton University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/saber/level1b_cdf/2002/01/timed_l1bv20_saber_200201250121_v01.cdf. The most common cadence, 53947 [ms] = PT53.947S, occurred for 2.0202% of the 2 timesteps. 

Thermosphere+Ionosphere+Mesosphere+Energetics and Dynamics (from all.xml/observatory/description/@short)

Sounding of the Atmosphere using Broadband Emission Radiometry (from all.xml/instrument/description/@short)

Mesospheric Science (from Master/CDFglobalAttributes/Discipline)

Thermosphere+Ionosphere+Mesosphere+Energetics and Dynamics (from Master/CDFglobalAttributes/Source_name)

Level 1B version 2.0 (from Master/CDFglobalAttributes/Data_type)

Phase of day at Tangent Point (0=Day 1=Night 2=Twilight(85<solar zenith angle<95)), 

Calibrated RADIANCE centered at 15.2um (C02-N) vs tangent point height

NMC temperature vs geopotential height at tangent point (scan-average)

NMC geopotential height vs pressure at tangent point (scan-average)

GUVI measures FUV airglow in five spectral bands: HI(121.6nm), OI(130.4nm), OI(135.6nm), LBHS(141-152.8nm), and  LBHL(167.2-181.2nm). The cross-track scanning spectrograph images a ground swath of 3000 km width providing a nearly contiguous global coverage duringone day (15 orbits). The L1CDisk (Level 1C disk, V03) data provide the calibrated, geolocated,and rectified intensities for the 5wavelengths bands. DISPLAY OPTIONS:    (1) Mapped images of the (lin or log) intensities by orbit using a transverseMercator projection.(2) Mapped images of the (lin or log) intensities using a polar projectionof the North and South pole areas.  Generating thumbnails for (1) or (2)   for one day takes about 1 minute.(3) Movies of plot types (1),(2):There are 15 orbits/frames per day,max is 2 days, i.e. 30  frames. (4) Images of intensitiesas scannedalong the orbit.(5) Line plots of intensitiesat selected across-track positions.    CDAWeb TUTORIAL:A tutorial on how to use CDAWeb to quickly generate GUVI plots canbe found athttps://cdaweb.gsfc.nasa.gov/cdaweb/cdaweb_guvi_tutorial.pdf  DATA DESCRIPTION:Details about the data format and processing can be found at http://guvi.jhuapl.edu/data/understanding.shtml 

Note: THE L1C FILES CURRENTLY AVAILABLE ARE BEING EVALUATED; It looks like the L1C LBH1 and LBH2 colors have too much background subtracted.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch2, @1 => Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch2, @1 => Epoch.)

[Mercator Projection by Orbit, Log10 Scaling] H Ly-alpha (1216 A) Intensities [Plots/CDFs ONLY]

[Mercator Projection by Orbit, Linear Scaling] H Ly-alpha (1216 A) Intensities [Plots/CDFs ONLY]

[Movie, Mercator Projection by Orbit, Log10 Scaling] H Ly-alpha (1216 A) Intensities

[North Polar Projection by Orbit, Log10 Scaling] H Ly-alpha (1216 A) Intensities [Plot/CDFs ONLY]

[Movie, North Polar Projection by Orbit, Log10 Scaling] H Ly-alpha (1216 A) Intensities

[South Polar Projection by Orbit, Log10 Scaling] H Ly-alpha (1216 A) Intensities [Plots/CDFs ONLY]

[Movie, South Polar Projection by Orbit, Log10 Scaling] H Ly-alpha (1216 A) Intensities

[SUPPORTING DATA, Mercator Projection by Orbit, Linear Scaing] Array of pixel center geographic latitude

[Errors in Intensities, Mercator Projection by Orbit, Linear Scaling] Systematic H Ly-alpha (1216 A)

[Intensities for all Across-Track Positions, Linear Scaling] H Ly-alpha (1216 A)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/guvi/levels_v10/level1c/disk_cdf/2001/10/timed_L1Cdisk_guvi_20011018061025_v01.cdf. The most common cadence, 31448911000 [ms] = P363DT23H48M31S, occurred for 0.4762% of the 1 timesteps. 

[Intensities for 7 Across-Track Positions, Linear Scaling] H Ly-alpha (1216 A)

Nadir geographic latitude of GUVI sweep as function of time (plot)

Nadir geographic longitude of GUVI sweep as function of time (plot)

Nadir geomagnetic latitude of GUVI sweep as function of time (plot)

Nadir geomagnetic longitude of GUVI sweep as function of time (plot)

O3, CO2, H2O Mixing Ratios and O, O2, OH, NO Volume Emission Rates, also NMC Neutral Temp., Density, and Pressure, Version 2.0, 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/saber/level2a_cdf/2002/01/timed_l2a_saber_200201250121_v02-07-01.cdf. The most common cadence, 71504 [ms] = PT1M11.504S, occurred for 2.1978% of the 2 timesteps. 

Phase of day at Tangent Point (0=Day, 1=Night, 2=Twilight (85<solar zenith angle<95)), 

Tangent point solar zenith angle vs tangent point height (lower part of scan)

---------> solar zenith angle vs tangent point height (upper part of scan

Volume Emission Rates (VER): -> O2(1delta) VER vs tangent point height

--------------> filtered (actual measurement with SABER's spectral bandpass for this line)

Included the final TIMED-SEE suborbital rocket calibration (NASA 36.240, 14-Apr-2008).  This involved a departure from previous calibration methods which were derived from very similar instrumentation. The primary instrument aboard NASA 36.240  is the prototype SDO EUV Variability Experiment (EVE) with a spectral range of 6 nm to 105 nm.  The SORCE SOLSTICE is used for correcting the EGS degradation trend in the FUV (115 nm - 190 nm).  A novel approach is applied in Version 10 in which information from the EGS on-board flatfield-measured changes is mapped to all of the rocket calibrations to provide improved EGS degradation trend. -  Updated and extended EGS flatfield degradation curve fits through 2008.-  Updated EGS FOV correction to perform monthly averaging to remove day-to-day jumps in irradiance. This removes the need for the beta angle correction that was added into version 9.-  Updated degradation algorithm to keep the normal channel in better agreement with the calibration channel. This improves the spectral shape in heavily degraded regions.-  Updated EGS gain to be a function of wavelength and temperature.  The present assumption is that enough degradation has occurred to affect the electrical resistance of the microchannel plates such that low-exposure regions on the detector are increasing with time.-  Added a step correction for EGS data beyond 2004/263. Near this time period the spacecraft entered a prolonged safe mode demotion.  An operational decision was made to point SEE down toward the spacecraft deck. We now believe this allowed a small amount of contamination to enter the aperture which decreased the sensitivity by approximately 8% in the EUV.-  The responsivity of the XPS photometers was updated.-  The second order subtraction of 30.4 has been adjusted to avoid zero flux.  This is based on a curve fit to two gaussians, which has some problems, but is an improvement over previous versions.-  Wavelengths longer than 190 nm are now zeroed out. Users interested in this range are encouraged to use the higher-precision SORCE-SOLSTICE data.(See also ftp://laspftp.colorado.edu/pub/SEE_Data/SEE_v10_releasenotes.txt including description of earlier versions)The TIMED-SEE XPS Level 4 product has been updated to include an improved solar cycle minimum reference spectrum.  This reference model is a combination of the CHIANTI Quiet Sun (QS) DEM and Coronal Hole (CH) DEM.  Now that XPS has made solar cycle minimum measurements in 2007-2009, the weighting for combining the QS and CH DEMs to match XPS observations is more accurate now. The previous XPS Level 4 model used a weighting of 0.5 for each; now the weights are 0.32 and 0.68 for the QS DEM and CH DEM, respectively.  In addition to this update, a software bug in using the GOES XRS data for 'flare' temperature has been fixed.  The previous XPS Level 4 data had a constant irradiance spectrum used throughout the day whenever the GOES XRS 0.1-0.8 nm irradiance fell below a minimum level, resulting in invalid temperatures. This is fixed now by assigning a minimum temperature of 3 MK whenever the GOES XRS irradiance falls below its minimum level.

SPDF/CDAWeb. Please also acknowledge the data producer: Tom Woods at LASP/CU

SPDF/SSCWeb. Please also acknowledge the data producer: Tom Woods at LASP/CU

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Tom Woods at LASP/CU

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/see/data/level3a_cdf/2002/01/timed_l3a_see_20020122_v01.cdf. The most common cadence, 5837000 [ms] = PT1H37M17S, occurred for 27.4725% of the 25 timesteps. 

Solar EUV Experiment (from all.xml/instrument/description/@short)

[NOT FOR PLOTTING] Accuracy of solar irradiance at 38 wavelengths

TIDI data and experiment home page hosted by National Center for Atmospheric Research, NCAR

TIDI data and experiment home page hosted by University of Michigan, UM

TIMED Mission Data Center hosted by the Johns Hopkins University, Applied Physics Laboratory, JHU/APL

General information concerning the TIMED, TIMED Doppler Interferometer, TIDI, instrument

SPDF/CDAWeb. Please also acknowledge the data producer: Timothy Killeen at NCAR

SPDF/SSCWeb. Please also acknowledge the data producer: Timothy Killeen at NCAR

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Timothy Killeen at NCAR

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epochcold_ascend, @1 => Epochwarm_ascend, @2 => Epochcold_descend, @3 => Epochwarm_descend.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epochcold_ascend, @1 => Epochwarm_ascend, @2 => Epochcold_descend, @3 => Epochwarm_descend.)

Wind Vectors from NCAR (from Master/CDFglobalAttributes/Data_type)

Zonal wind at 75, 80, 85, 90, 95, and 100 km, Ascending orbit phase, Cold side

Counts based on variable 'Epochcold_ascend' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/tidi/windvectors_ncar/2002/02/timed_windvectorsncar_tidi_200202200006_v01.cdf. The most common cadence, 99050 [ms] = PT1M39.05S, occurred for 14.3236% of the 54 timesteps. 

Meridional wind at 75, 80, 85, 90, 95, and 100 km, Ascending orbit phase, Cold Side

Zonal wind profiles (velocity as function of time and altitude), Ascending orbit phase, Cold side

- -> Zonal wind variance profiles,  Ascending orbit phase, Cold side

Meridional wind profiles, (velocity as a function of time and altitude), Ascending orbit phase, Cold side

- -> Meridional wind variance profiles Ascending orbit phase, Cold side

Wind vector map, 80 km, Cylindrical projection, Ascending orbit phase, Cold side

- -> Transverse Mercator projection, Ascending orbit phase, Cold side

- -> MOVIE: Cylindrical projection, Ascending orbit phase, Cold side

- -> MOVIE: Transverse Mercator projection, Ascending orbit phase, Cold side

Wind vector map, 90 km, Cylindrical projection, Ascending orbit phase, Cold side

Wind vector map, 100 km, Cylindrical projection, Ascending orbit phase, Cold side

Counts based on variable 'Epochwarm_ascend' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/tidi/windvectors_ncar/2002/02/timed_windvectorsncar_tidi_200202200006_v01.cdf. The most common cadence, 99050 [ms] = PT1M39.05S, occurred for 13.8824% of the 59 timesteps. 

Counts based on variable 'Epochcold_descend' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/tidi/windvectors_ncar/2002/02/timed_windvectorsncar_tidi_200202200006_v01.cdf. The most common cadence, 82280 [ms] = PT1M22.28S, occurred for 76.1006% of the 363 timesteps. 

Counts based on variable 'Epochwarm_descend' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/timed/tidi/windvectors_ncar/2002/02/timed_windvectorsncar_tidi_200202200006_v01.cdf. The most common cadence, 82280 [ms] = PT1M22.28S, occurred for 55.1724% of the 240 timesteps. 

Electron density and electric field measurements during the rocket flight.

SPDF/CDAWeb. Please also acknowledge the data producer: D. Hysell at Cornell University

SPDF/SSCWeb. Please also acknowledge the data producer: D. Hysell at Cornell University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. Hysell at Cornell University

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_1.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_1.)

Waves and Instabilities from a Neutral Dynamo (from all.xml/observatory/description/@short)

Waves and Instabilities from a Neutral Dynamo (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/toowindy/toowindy_e_ne_20190616_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 0.0800% of the 445 timesteps. 

Counts based on variable 'Epoch_1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/sounding_rockets/toowindy/toowindy_e_ne_20190616_v01.cdf. The most common cadence, 1000 [ms] = PT1S, occurred for 0.0200% of the 440 timesteps. 

References:                                             1. The Instrument Data File Set. URL http://www.idfs.org

SPDF/CDAWeb. Please also acknowledge the data producer: Tony Lavoie at Marshall Space Flight Center

SPDF/SSCWeb. Please also acknowledge the data producer: Tony Lavoie at Marshall Space Flight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Tony Lavoie at Marshall Space Flight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csaa/1996/tss-1r_m1_csaa_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

Shuttle Attitude Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csab/1996/tss-1r_m1_csab_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

Orbiter and Target State Vectors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csca/1996/tss-1r_m1_csca_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

Computed OA Data Values (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/cscb/1996/tss-1r_m1_cscb_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

Special Computation Events (from all.xml/instrument/description/@short)

TSS-1R, Temperature, Voltage, and Current Measurements IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csea/1996/tss-1r_m1_csea_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

Temperature, Voltage, and Current Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/cseb/1996/tss-1r_m1_cseb_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

Supply and Waste Water Quantities (from all.xml/instrument/description/@short)

TSS-1R, KU-Band Communications/RADAR Roll and Pitch Monitors IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csma/1996/tss-1r_m1_csma_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

KU-Band Communications/RADAR Roll and Pitch Monitors (from all.xml/instrument/description/@short)

TSS-1R, KU-Band Communications/RADAR Power and Range Monitors IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csmb/1996/tss-1r_m1_csmb_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

KU-Band Communications/RADAR Power and Range Monitors (from all.xml/instrument/description/@short)

TSS-1R, FCP, Water and Waste Dump, FES, and Power Status IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/cssa/1996/tss-1r_m1_cssa_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

FCP, Water and Waste Dump, FES, and Power Status (from all.xml/instrument/description/@short)

TSS-1R, KU-BAND Communications/RADAR and Recorder Operation Status IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/cssb/1996/tss-1r_m1_cssb_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

KU-BAND Communications/RADAR and Recorder Operation Status (from all.xml/instrument/description/@short)

TSS-1R, RCS/Vernier Jets-Impulse/Exhaust Gases Status IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/cssc/1996/tss-1r_m1_cssc_19960222212629_v01.cdf. The most common cadence, 40000000 [ns] = PT0.04S, occurred for 99.9664% of the 14893 timesteps. 

RCS/Vernier Jets-Impulse/Exhaust Gases Status (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/cas/csta/1996/tss-1r_m1_csta_19960222212629_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 99.1582% of the 589 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Jean Sabbagh at ASI

SPDF/SSCWeb. Please also acknowledge the data producer: Jean Sabbagh at ASI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Jean Sabbagh at ASI

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1.)

Boom Tip Position           (DBPO) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbpo/1996/tss-1r_m1_dbpo_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbpo/1996/tss-1r_m1_dbpo_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Boom, DPY/RTR, and JTS Status Data  (DBSA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbsa/1996/tss-1r_m1_dbsa_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbsa/1996/tss-1r_m1_dbsa_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

TSS-1R, Boom Stowed Status, DPY/RTR Status, and JTR Fire Status IDFS format

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2.)

Boom Stowed Status, DPY/RTR Status, and JTR Fire Status (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbsb/1996/tss-1r_m1_dbsb_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbsb/1996/tss-1r_m1_dbsb_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbsb/1996/tss-1r_m1_dbsb_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbsc/1996/tss-1r_m1_dbsc_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

DPY/RTR and JTR Power Status (from all.xml/instrument/description/@short)

Boom Temperature Monitors   (DBTA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbta/1996/tss-1r_m1_dbta_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbta/1996/tss-1r_m1_dbta_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/drb/dbta/1996/tss-1r_m1_dbta_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Carlo Bonifazi at ASI

SPDF/SSCWeb. Please also acknowledge the data producer: Carlo Bonifazi at ASI

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Carlo Bonifazi at ASI

DV Voltage and DVG Pressure Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcdv/1996/tss-1r_m1_dcdv_19960223093334_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8784% of the 12290 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcdv/1996/tss-1r_m1_dcdv_19960223093334_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8784% of the 12290 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcga/1996/tss-1r_m1_dcga_19960223093334_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8784% of the 12290 timesteps. 

Electron Gun Current Monitors  (DCGA) (from all.xml/instrument/description/@short)

TSS-1R, Electron Gun Tether Current Offset Measurements IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcgb/1996/tss-1r_m1_dcgb_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Electron Gun Tether Current Offset Measurements (from all.xml/instrument/description/@short)

TSS-1R, Electron Filament Voltage And Acceleration Potentials IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcgc/1996/tss-1r_m1_dcgc_19960223093334_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8784% of the 12290 timesteps. 

Electron Filament Voltage And Acceleration Potentials (from all.xml/instrument/description/@short)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4.)

General Monitor Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcma/1996/tss-1r_m1_dcma_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcma/1996/tss-1r_m1_dcma_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcma/1996/tss-1r_m1_dcma_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcma/1996/tss-1r_m1_dcma_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcma/1996/tss-1r_m1_dcma_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 6 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5.)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmb/1996/tss-1r_m1_dcmb_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmb/1996/tss-1r_m1_dcmb_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmb/1996/tss-1r_m1_dcmb_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmb/1996/tss-1r_m1_dcmb_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmb/1996/tss-1r_m1_dcmb_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmb/1996/tss-1r_m1_dcmb_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

EGA Filament and Tether Current Cycle Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmc/1996/tss-1r_m1_dcmc_19960223093334_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 49.9368% of the 395 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmc/1996/tss-1r_m1_dcmc_19960223093334_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 49.9368% of the 395 timesteps. 

DCORE Format Counter and Dump Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmd/1996/tss-1r_m1_dcmd_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcmd/1996/tss-1r_m1_dcmd_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Applicative Programs Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcme/1996/tss-1r_m1_dcme_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcme/1996/tss-1r_m1_dcme_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcsa/1996/tss-1r_m1_dcsa_19960223093334_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8784% of the 12290 timesteps. 

General High Rate Status Measurements (from all.xml/instrument/description/@short)

General Status Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcsb/1996/tss-1r_m1_dcsb_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcsb/1996/tss-1r_m1_dcsb_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcsb/1996/tss-1r_m1_dcsb_19960223093335_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Temperature Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcta/1996/tss-1r_m1_dcta_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcta/1996/tss-1r_m1_dcta_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcta/1996/tss-1r_m1_dcta_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcta/1996/tss-1r_m1_dcta_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dcore/dcta/1996/tss-1r_m1_dcta_19960223093334_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 75.0000% of the 1188 timesteps. 

TSS-1R, 16/major Frame Miscellaneous Housekeeping Data IDFS format

SPDF/CDAWeb. Please also acknowledge the data producer: Ron Geiger at Martin Marietta Astronautics

SPDF/SSCWeb. Please also acknowledge the data producer: Ron Geiger at Martin Marietta Astronautics

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Ron Geiger at Martin Marietta Astronautics

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpha/1996/tss-1r_m1_dpha_19960222235119_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8855% of the 4044 timesteps. 

16/major Frame Miscellaneous Housekeeping Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dphb/1996/tss-1r_m1_dphb_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

SFMSD Command Word Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dphc/1996/tss-1r_m1_dphc_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Rotating Memeory Dump Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dphd/1996/tss-1r_m1_dphd_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Segment Information (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dphe/1996/tss-1r_m1_dphe_19960222235119_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8855% of the 4044 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpma/1996/tss-1r_m1_dpma_19960222235119_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8855% of the 4044 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmb/1996/tss-1r_m1_dpmb_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Low Rate Tether Information (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmc/1996/tss-1r_m1_dpmc_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

16 bit Measured Tether Lengths and Rates (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmd/1996/tss-1r_m1_dpmd_19960222235119_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8855% of the 4044 timesteps. 

Tether Rate Raw Timer Counts (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpme/1996/tss-1r_m1_dpme_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Miscellaneous Tether Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmf/1996/tss-1r_m1_dpmf_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Voltage, Current, and Tether Tension Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmg/1996/tss-1r_m1_dpmg_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmh/1996/tss-1r_m1_dpmh_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmi/1996/tss-1r_m1_dpmi_19960222235119_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8855% of the 4044 timesteps. 

Tether Length Raw Encoder Counts (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmj/1996/tss-1r_m1_dpmj_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpmk/1996/tss-1r_m1_dpmk_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.0000% of the 130 timesteps. 

Reel Motor Command Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsa/1996/tss-1r_m1_dpsa_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsc/1996/tss-1r_m1_dpsc_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Power and ADC Voltage Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsd/1996/tss-1r_m1_dpsd_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpse/1996/tss-1r_m1_dpse_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

U1 and U2 Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsf/1996/tss-1r_m1_dpsf_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

L-DOT, DEL-L, and Talkback Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsg/1996/tss-1r_m1_dpsg_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

1/major Frame Miscellaneous Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsh/1996/tss-1r_m1_dpsh_19960222235119_v01.cdf. The most common cadence, 124800000 [ns] = PT0.1248S, occurred for 96.8855% of the 4044 timesteps. 

16/major Frame Miscellaneous Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsi/1996/tss-1r_m1_dpsi_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Maneuver Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpsj/1996/tss-1r_m1_dpsj_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Miscellaneous Relay Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dpta/1996/tss-1r_m1_dpta_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

Reel And Boom Temperature Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/dply/dptb/1996/tss-1r_m1_dptb_19960222235119_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 50.1931% of the 130 timesteps. 

TSS-1R, Temperature, Voltage, Current, and Freon Data IDFS format

Temperature, Voltage, Current, and Freon Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epma/1996/tss-1r_m1_epma_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epma/1996/tss-1r_m1_epma_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

TSS-1R, Output Command Block and Variable Data Block IDFS format

Output Command Block and Variable Data Block (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmb/1996/tss-1r_m1_epmb_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmb/1996/tss-1r_m1_epmb_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmb/1996/tss-1r_m1_epmb_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmb/1996/tss-1r_m1_epmb_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmb/1996/tss-1r_m1_epmb_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmc/1996/tss-1r_m1_epmc_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

SFMDM Last Command Accepted Buffer (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmf/1996/tss-1r_m1_epmf_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmf/1996/tss-1r_m1_epmf_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmf/1996/tss-1r_m1_epmf_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

DDCS and SFMDM Miscellaneous Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmg/1996/tss-1r_m1_epmg_19960222230504_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmg/1996/tss-1r_m1_epmg_19960222230504_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epmh/1996/tss-1r_m1_epmh_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

SFMDM RS-422 And IO Transfer Data (from all.xml/instrument/description/@short)

EMP Satellite and Deployer Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epsa/1996/tss-1r_m1_epsa_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epsa/1996/tss-1r_m1_epsa_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

EMP SFMDM General Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epsb/1996/tss-1r_m1_epsb_19960222230504_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epsb/1996/tss-1r_m1_epsb_19960222230504_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

TSS-1R, EMP SFMDM D05 and D28 LEV and PUL Status Data IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epsc/1996/tss-1r_m1_epsc_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

EMP SFMDM D05 and D28 LEV and PUL Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/emp/epsd/1996/tss-1r_m1_epsd_19960222230505_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9848% of the 2473 timesteps. 

SDIO Channel Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpbb/1996/tss-1r_m1_rpbb_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

Boom Biasing Current and Voltage (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Nobie Stone at Marshall Space Flight Center

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Nobie Stone at Marshall Space Flight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Nobie Stone at Marshall Space Flight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpdm/1996/tss-1r_m1_rpdm_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

DIFP Peak Monitor Data  (RPDM) (from all.xml/instrument/description/@short)

DIFP Deflection and Retard Data  (RPDP) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpdp/1996/tss-1r_m1_rpdp_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 49.9383% of the 810 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpdp/1996/tss-1r_m1_rpdp_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 49.9383% of the 810 timesteps. 

Satellite Mounted Electron Sensors  (RPEA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpea/1996/tss-1r_m1_rpea_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpea/1996/tss-1r_m1_rpea_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Boom Mounted Electron Sensors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpeb/1996/tss-1r_m1_rpeb_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpeb/1996/tss-1r_m1_rpeb_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpem/1996/tss-1r_m1_rpem_19960223183300_v01.cdf. The most common cadence, 1000000 [ns] = PT0.001S, occurred for 99.5605% of the 14271 timesteps. 

DIFP Electrometer Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpha/1996/tss-1r_m1_rpha_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

DIFP Miscellaneous Housekeeping  (RPHA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rphb/1996/tss-1r_m1_rphb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

DIFP A/D Voltage And Current Monitors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rphc/1996/tss-1r_m1_rphc_19960223180030_v01.cdf. The most common cadence, 4096000000 [ns] = PT4.096S, occurred for 78.6207% of the 684 timesteps. 

SPES Voltage And Current Monitors (RPHC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rphd/1996/tss-1r_m1_rphd_19960223180030_v01.cdf. The most common cadence, 8192000000 [ns] = PT8.192S, occurred for 57.6037% of the 250 timesteps. 

SPES Grid Voltages  (RPHD) (from all.xml/instrument/description/@short)

TSS-1R, ROPE CEP and FS Voltage And Temperature Monitors (RPHE) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rphe/1996/tss-1r_m1_rphe_19960223180030_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

ROPE CEP and FS Voltage And Temperature Monitors (RPHE) (from all.xml/instrument/description/@short)

TSS-1R, Satellite Programmable Power Supply Monitors (RPHF) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rphf/1996/tss-1r_m1_rphf_19960224202718_v01.cdf. The most common cadence, 1984000000 [ns] = PT1.984S, occurred for 75.1046% of the 359 timesteps. 

Satellite Programmable Power Supply Monitors (RPHF) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rphg/1996/tss-1r_m1_rphg_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Floating Power Supply Current (RPHG) (from all.xml/instrument/description/@short)

Satellite Mounted Ion Sensor (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpia/1996/tss-1r_m1_rpia_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpia/1996/tss-1r_m1_rpia_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Boom Mounted Ion Sensors (RPIB) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpib/1996/tss-1r_m1_rpib_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpib/1996/tss-1r_m1_rpib_19960224202718_v01.cdf. The most common cadence, 2048000000 [ns] = PT2.048S, occurred for 88.8309% of the 851 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpsa/1996/tss-1r_m1_rpsa_19960223180030_v01.cdf. The most common cadence, 8192000000 [ns] = PT8.192S, occurred for 57.6037% of the 250 timesteps. 

SPES Grid Bias And HVU 1/2 Status (RPSA) (from all.xml/instrument/description/@short)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 4 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3.)

ROPE Command Status Words (RPSB) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpsb/1996/tss-1r_m1_rpsb_19960223180030_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, Floating Supply Discrete Status Values (RPSC) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpsc/1996/tss-1r_m1_rpsc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Floating Supply Discrete Status Values (RPSC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rope/rpsd/1996/tss-1r_m1_rpsd_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

DIFP RAM Test Data (RPSD) (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Marino Dobrowolny at Instituto Di Fisica Dello Spazio Interplanetario

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Marino Dobrowolny at Instituto Di Fisica Dello Spazio Interplanetario

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Marino Dobrowolny at Instituto Di Fisica Dello Spazio Interplanetario

Langmuir Probe DC Electric Field Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtef/1996/tss-1r_m1_rtef_19960223182715_v01.cdf. The most common cadence, 200000000 [ns] = PT0.2S, occurred for 91.6103% of the 8932 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtef/1996/tss-1r_m1_rtef_19960223182715_v01.cdf. The most common cadence, 3200000000 [ns] = PT3.2S, occurred for 5.1692% of the 504 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rthf/1996/tss-1r_m1_rthf_19960223182748_v01.cdf. The most common cadence, 10944000000 [ns] = PT10.944S, occurred for 53.3742% of the 87 timesteps. 

High Frequency Electromagnetic Wave Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtip/1996/tss-1r_m1_rtip_19960223182748_v01.cdf. The most common cadence, 100000000 [ns] = PT0.1S, occurred for 95.6355% of the 17924 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtka/1996/tss-1r_m1_rtka_19960223182715_v01.cdf. The most common cadence, 16384000000 [ns] = PT16.384S, occurred for 81.8966% of the 95 timesteps. 

AC Housekeeping measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtkc/1996/tss-1r_m1_rtkc_19960223182715_v01.cdf. The most common cadence, 32768000000 [ns] = PT32.768S, occurred for 63.1579% of the 36 timesteps. 

Error table measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtkd/1996/tss-1r_m1_rtkd_19960223182715_v01.cdf. The most common cadence, 32768000000 [ns] = PT32.768S, occurred for 63.1579% of the 36 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtke/1996/tss-1r_m1_rtke_19960223182715_v01.cdf. The most common cadence, 512000000 [ns] = PT0.512S, occurred for 99.4436% of the 3753 timesteps. 

Pentode Current And DCBP Voltage (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtkf/1996/tss-1r_m1_rtkf_19960223180057_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

LF RETE Format Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtkh/1996/tss-1r_m1_rtkh_19960223182715_v01.cdf. The most common cadence, 32768000000 [ns] = PT32.768S, occurred for 61.1111% of the 33 timesteps. 

MF RETE Format Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtki/1996/tss-1r_m1_rtki_19960223182715_v01.cdf. The most common cadence, 32768000000 [ns] = PT32.768S, occurred for 61.1111% of the 33 timesteps. 

HF RETE Format Data (from all.xml/instrument/description/@short)

TSS-1R, Low Frequency Electromagnetic Wave Data (Band A) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtla/1996/tss-1r_m1_rtla_19960223180057_v01.cdf. The most common cadence, 11059000000 [ns] = PT11.059S, occurred for all 1 timesteps. 

Low Frequency Electromagnetic Wave Data (Band A) (from all.xml/instrument/description/@short)

TSS-1R, Low Frequency Electromagnetic Wave Data (Band B) IDFS format

Low Frequency Electromagnetic Wave Data (Band B) (from all.xml/instrument/description/@short)

TSS-1R, Medium Frequency Electromagnetic Wave Data (Band C) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtmc/1996/tss-1r_m1_rtmc_19960223182748_v01.cdf. The most common cadence, 3200000000 [ns] = PT3.2S, occurred for 80.1095% of the 439 timesteps. 

Medium Frequency Electromagnetic Wave Data (Band C) (from all.xml/instrument/description/@short)

TSS-1R, Medium Frequency Electromagnetic Wave Data (Band D) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtmd/1996/tss-1r_m1_rtmd_19960223182750_v01.cdf. The most common cadence, 3200000000 [ns] = PT3.2S, occurred for 80.1095% of the 439 timesteps. 

Medium Frequency Electromagnetic Wave Data (Band D) (from all.xml/instrument/description/@short)

TSS-1R, Medium Frequency Electromagnetic Wave Data (Band E) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtme/1996/tss-1r_m1_rtme_19960223182750_v01.cdf. The most common cadence, 92200000 [ns] = PT0.0922S, occurred for 75.0227% of the 1649 timesteps. 

Medium Frequency Electromagnetic Wave Data (Band E) (from all.xml/instrument/description/@short)

TSS-1R, Medium Frequency Electromagnetic Wave Data (Band F) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtmf/1996/tss-1r_m1_rtmf_19960223182751_v01.cdf. The most common cadence, 18400000 [ns] = PT0.0184S, occurred for 90.0146% of the 4949 timesteps. 

Medium Frequency Electromagnetic Wave Data (Band F) (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: J-P. Lebreton at ESA/ESTEC, Solar System Division

SPDF/SSCWeb. Please also acknowledge the data producer: J-P. Lebreton at ESA/ESTEC, Solar System Division

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J-P. Lebreton at ESA/ESTEC, Solar System Division

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/rete/rtrlp/1996/tss-1r_m1_rtrlp_19960225202808_v01.cdf. The most common cadence, 3200000000 [ns] = PT3.2S, occurred for 89.7233% of the 454 timesteps. 

Reduced Langmuir Probe Data (from all.xml/instrument/description/@short)

SLA vector coarse acceleration (SCAC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scac/1996/tss-1r_m1_scac_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scac/1996/tss-1r_m1_scac_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scac/1996/tss-1r_m1_scac_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

TSS-1R, SLA High Res Vector Acceleration Measurements (SCAF) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scaf/1996/tss-1r_m1_scaf_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

SLA High Res Vector Acceleration Measurements (SCAF) (from all.xml/instrument/description/@short)

SLA Temperature and Voltage Monitors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scma/1996/tss-1r_m1_scma_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scma/1996/tss-1r_m1_scma_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scma/1996/tss-1r_m1_scma_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scma/1996/tss-1r_m1_scma_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

TSS-1R, SA Temperature and Overtemperature Monitors  (SCMB) IDFS format

SA Temperature and Overtemperature Monitors  (SCMB) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scmb/1996/tss-1r_m1_scmb_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scmb/1996/tss-1r_m1_scmb_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

Satellite Ampmeter Current Monitors  (SCMC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scmc/1996/tss-1r_m1_scmc_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scmc/1996/tss-1r_m1_scmc_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

TSS-1R, Low time resolution experiment status flags  (SCSA) IDFS format

Low time resolution experiment status flags  (SCSA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scsa/1996/tss-1r_m1_scsa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scsa/1996/tss-1r_m1_scsa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scsa/1996/tss-1r_m1_scsa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

TSS-1R, High time resolution experiment status flags  (SCSB) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/score/scsb/1996/tss-1r_m1_scsb_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

High time resolution experiment status flags  (SCSB) (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: G. Oelker at Alenia Spazio  S.p.A.

SPDF/SSCWeb. Please also acknowledge the data producer: G. Oelker at Alenia Spazio  S.p.A.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Oelker at Alenia Spazio  S.p.A.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shaa/1996/tss-1r_m1_shaa_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Yaw, Roll and Pitch Data (from all.xml/instrument/description/@short)

Scaled Roll, Yaw and Pitch Data    (SHAB) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shab/1996/tss-1r_m1_shab_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shab/1996/tss-1r_m1_shab_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Mode_Epoch.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Mode_Epoch.)

Gyro Rate and Sun Presence (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shac/1996/tss-1r_m1_shac_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shac/1996/tss-1r_m1_shac_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shac/1996/tss-1r_m1_shac_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Gyro Angular Data           (SHAD) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shad/1996/tss-1r_m1_shad_19960223180030_v01.cdf. The most common cadence, 128000000 [ns] = PT0.128S, occurred for 99.3334% of the 27716 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shad/1996/tss-1r_m1_shad_19960223180030_v01.cdf. The most common cadence, 128000000 [ns] = PT0.128S, occurred for 99.3334% of the 27716 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 11 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO2, @2 => Epoch_TO4, @3 => Epoch_TO6, @4 => Epoch_TO1, @5 => Epoch_TO3, @6 => Epoch_TO5, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 11 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO2, @2 => Epoch_TO4, @3 => Epoch_TO6, @4 => Epoch_TO1, @5 => Epoch_TO3, @6 => Epoch_TO5, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10.)

Gyro and Attitude Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO7' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO8' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO9' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO10' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shae/1996/tss-1r_m1_shae_19960223180044_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Satellite Spin Rate        (SAHF) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shaf/1996/tss-1r_m1_shaf_19960223180046_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shaf/1996/tss-1r_m1_shaf_19960223180046_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shag/1996/tss-1r_m1_shag_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Gyro and Attitude Angular Data (from all.xml/instrument/description/@short)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 13 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10, @11 => Epoch_TO11, @12 => Epoch_TO12.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 13 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10, @11 => Epoch_TO11, @12 => Epoch_TO12.)

Miscellaneous Housekeeping Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO7' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO8' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO9' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO10' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO11' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO12' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shha/1996/tss-1r_m1_shha_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, 24 Bit Battery Current  and Power Moniters   (SHHB) IDFS format

24 Bit Battery Current  and Power Moniters   (SHHB) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhb/1996/tss-1r_m1_shhb_19960223180034_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhb/1996/tss-1r_m1_shhb_19960223180034_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhb/1996/tss-1r_m1_shhb_19960223180034_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhb/1996/tss-1r_m1_shhb_19960223180034_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhb/1996/tss-1r_m1_shhb_19960223180034_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Miscellaneous Timing Data    (SHHC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhc/1996/tss-1r_m1_shhc_19960223180038_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhc/1996/tss-1r_m1_shhc_19960223180038_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhc/1996/tss-1r_m1_shhc_19960223180038_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhc/1996/tss-1r_m1_shhc_19960223180038_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhc/1996/tss-1r_m1_shhc_19960223180038_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhc/1996/tss-1r_m1_shhc_19960223180038_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, Various 64/major frame 8 bit Housekeeping Data (SHHD) IDFS format

Various 64/major frame 8 bit Housekeeping Data (SHHD) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhd/1996/tss-1r_m1_shhd_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhd/1996/tss-1r_m1_shhd_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

TSS-1R, Low time resolution 3 bit satellite monitors  (SHHE) IDFS format

Low time resolution 3 bit satellite monitors  (SHHE) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhe/1996/tss-1r_m1_shhe_19960223180036_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhe/1996/tss-1r_m1_shhe_19960223180036_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, Satellite RX Coherent AGC and Loop Stress Data IDFS format

Satellite RX Coherent AGC and Loop Stress Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhf/1996/tss-1r_m1_shhf_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shhf/1996/tss-1r_m1_shhf_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shma/1996/tss-1r_m1_shma_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Onboard Data Handling RSMN Data    (SHMA) (from all.xml/instrument/description/@short)

Onboard Data Handling ASMN Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmb/1996/tss-1r_m1_shmb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmb/1996/tss-1r_m1_shmb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Memory Dump And TLC Data   (SHMC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO7' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO8' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO9' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO10' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO11' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO12' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmc/1996/tss-1r_m1_shmc_19960223180039_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

OBDH And AMCS Status Flags (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmd/1996/tss-1r_m1_shmd_19960223180040_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmd/1996/tss-1r_m1_shmd_19960223180040_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmd/1996/tss-1r_m1_shmd_19960223180040_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmd/1996/tss-1r_m1_shmd_19960223180040_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shmd/1996/tss-1r_m1_shmd_19960223180040_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shme/1996/tss-1r_m1_shme_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shme/1996/tss-1r_m1_shme_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shme/1996/tss-1r_m1_shme_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shme/1996/tss-1r_m1_shme_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 7 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 7 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6.)

Satellite miscellaneous power monitors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shpa/1996/tss-1r_m1_shpa_19960223180031_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_TO1, @1 => Epoch, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 5 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch_TO1, @1 => Epoch, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4.)

Low resolution gyro status flags  (SHSA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsa/1996/tss-1r_m1_shsa_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsa/1996/tss-1r_m1_shsa_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsa/1996/tss-1r_m1_shsa_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsa/1996/tss-1r_m1_shsa_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsa/1996/tss-1r_m1_shsa_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, Gyro converter, heating and wheel status data   (SHSB) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsb/1996/tss-1r_m1_shsb_19960223180030_v01.cdf. The most common cadence, 128000000 [ns] = PT0.128S, occurred for 99.3334% of the 27716 timesteps. 

Gyro converter, heating and wheel status data   (SHSB) (from all.xml/instrument/description/@short)

TSS-1R, Low resolution FDS3/FDS4 status flags   (SHSC) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsc/1996/tss-1r_m1_shsc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Low resolution FDS3/FDS4 status flags   (SHSC) (from all.xml/instrument/description/@short)

Satellite Program Status Flags (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsd/1996/tss-1r_m1_shsd_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsd/1996/tss-1r_m1_shsd_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsd/1996/tss-1r_m1_shsd_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsd/1996/tss-1r_m1_shsd_19960223180035_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, Medium resolution miscellaneous status flags  (SHSE) IDFS format

Medium resolution miscellaneous status flags  (SHSE) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shse/1996/tss-1r_m1_shse_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shse/1996/tss-1r_m1_shse_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shse/1996/tss-1r_m1_shse_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shse/1996/tss-1r_m1_shse_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

TSS-1R, Satellite medium resolution status data  (SHSF) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsf/1996/tss-1r_m1_shsf_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Satellite medium resolution status data  (SHSF) (from all.xml/instrument/description/@short)

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 10 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 10 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9.)

Satellite slow status data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO7' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO8' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

Counts based on variable 'Epoch_TO9' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsg/1996/tss-1r_m1_shsg_19960223180043_v01.cdf. The most common cadence, 16385000000 [ns] = PT16.385S, occurred for 41.2037% of the 89 timesteps. 

TSS-1R, Satellite high time resolution status data  (SHSH) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsh/1996/tss-1r_m1_shsh_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

Satellite high time resolution status data  (SHSH) (from all.xml/instrument/description/@short)

Satellite miscellaneous power status data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsi/1996/tss-1r_m1_shsi_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsi/1996/tss-1r_m1_shsi_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsi/1996/tss-1r_m1_shsi_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

TSS-1R, Alpha, Beta, and FDS1/FDS2 status data  (SHSJ) IDFS format

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsj/1996/tss-1r_m1_shsj_19960223180030_v01.cdf. The most common cadence, 256000000 [ns] = PT0.256S, occurred for 98.6667% of the 13764 timesteps. 

Alpha, Beta, and FDS1/FDS2 status data  (SHSJ) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shsk/1996/tss-1r_m1_shsk_19960223180030_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6667% of the 55620 timesteps. 

Satellite Thruster Status Data (from all.xml/instrument/description/@short)

Gyro and Earth Sensor Temperatures (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shta/1996/tss-1r_m1_shta_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shta/1996/tss-1r_m1_shta_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10, @11 => Epoch_TO11, @12 => Epoch_TO12, @13 => Epoch_TO13, @14 => Epoch_TO14, @15 => Epoch_TO15.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 16 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10, @11 => Epoch_TO11, @12 => Epoch_TO12, @13 => Epoch_TO13, @14 => Epoch_TO14, @15 => Epoch_TO15.)

Satellite temperatures (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO7' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO8' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO9' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO10' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO11' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO12' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO13' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO14' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO15' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtb/1996/tss-1r_m1_shtb_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

TSS-1R, Satellite temperatures and pressures   (SHTC) IDFS format

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 11 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 11 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_TO1, @2 => Epoch_TO2, @3 => Epoch_TO3, @4 => Epoch_TO4, @5 => Epoch_TO5, @6 => Epoch_TO6, @7 => Epoch_TO7, @8 => Epoch_TO8, @9 => Epoch_TO9, @10 => Epoch_TO10.)

Satellite temperatures and pressures   (SHTC) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO4' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO5' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO6' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO7' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO8' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO9' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

Counts based on variable 'Epoch_TO10' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sahk/shtc/1996/tss-1r_m1_shtc_19960223180030_v01.cdf. The most common cadence, 1024000000 [ns] = PT1.024S, occurred for 94.6644% of the 3300 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Dr Dave Hardy at GL/PHE

SPDF/SSCWeb. Please also acknowledge the data producer: Dr Dave Hardy at GL/PHE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr Dave Hardy at GL/PHE

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spba/1996/tss-1r_m1_spba_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

TSS-1R, Selected Electron Spectra From Spectrometer A IDFS format

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Dave Hardy at GL/PHE

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Dave Hardy at GL/PHE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Dave Hardy at GL/PHE

Selected Electron Spectra From Spectrometer A (from all.xml/instrument/description/@short)

Selected_Electron_Spectra_Head_A_1_Telemetry_Dimensionless Science Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spea/1996/tss-1r_m1_spea_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Selected_Electron_Spectra_Head_A_2_counts_acc_c_per_acc Science Data

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spea/1996/tss-1r_m1_spea_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

TSS-1R, Selected Electron Spectra From Spectrometer B IDFS format

Selected Electron Spectra From Spectrometer B (from all.xml/instrument/description/@short)

Selected_Electron_Spectra_Head_B_1_Telemetry_Dimensionless Science Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/speb/1996/tss-1r_m1_speb_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Selected_Electron_Spectra_Head_B_2_counts_acc_c_per_acc Science Data

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/speb/1996/tss-1r_m1_speb_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Electron Spectra From Spectrometer A (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spec/1996/tss-1r_m1_spec_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 45.2055% of the 33 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spec/1996/tss-1r_m1_spec_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 45.2055% of the 33 timesteps. 

Electron Spectra From Spectrometer B (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/sped/1996/tss-1r_m1_sped_19960223131955_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 48.5714% of the 34 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/sped/1996/tss-1r_m1_sped_19960223131955_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 48.5714% of the 34 timesteps. 

TSS-1R, ESA A, High Frequency Electron Auto-Corellation Spectra IDFS format

ESA A, High Frequency Electron Auto-Corellation Spectra (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spfa/1996/tss-1r_m1_spfa_19960223131959_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 48.8372% of the 21 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spfa/1996/tss-1r_m1_spfa_19960223131959_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 48.8372% of the 21 timesteps. 

TSS-1R, ESA B, High Frequency Electron Auto-Corellation Spectra IDFS format

ESA B, High Frequency Electron Auto-Corellation Spectra (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spfb/1996/tss-1r_m1_spfb_19960223132003_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 50.0000% of the 21 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spfb/1996/tss-1r_m1_spfb_19960223132003_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 50.0000% of the 21 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spha/1996/tss-1r_m1_spha_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 87.3418% of the 138 timesteps. 

Subcommutated Housekeeping Measureents (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/sphb/1996/tss-1r_m1_sphb_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

FDR Housekeeping Measurements (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/sphc/1996/tss-1r_m1_sphc_19960223131953_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 48.7179% of the 38 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/sphd/1996/tss-1r_m1_sphd_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/sphe/1996/tss-1r_m1_sphe_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

Uplink Command Echo (from all.xml/instrument/description/@short)

Zone Summed Ion Spectra From Spectrometer A (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spia/1996/tss-1r_m1_spia_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spia/1996/tss-1r_m1_spia_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Zone Summed Ion Spectra From Spectrometer B (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spib/1996/tss-1r_m1_spib_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spib/1996/tss-1r_m1_spib_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Selected Ion Spectra From Spectrometer A (from all.xml/instrument/description/@short)

Selected_Ion_Spectra_Head_A_1_Telemetry_Dimensionless Science Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spic/1996/tss-1r_m1_spic_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spic/1996/tss-1r_m1_spic_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

SPDF/CDAWeb. Please also acknowledge the data producer: Capt. Marilyn R. Oberhardt at GL/PHE

SPDF/SSCWeb. Please also acknowledge the data producer: Capt. Marilyn R. Oberhardt at GL/PHE

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Capt. Marilyn R. Oberhardt at GL/PHE

Selected Ion Spectra From Spectrometer B (from all.xml/instrument/description/@short)

Selected_Ion_Spectra_Head_B_1_Telemetry_Dimensionless Science Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spid/1996/tss-1r_m1_spid_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spid/1996/tss-1r_m1_spid_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Ion Spectra From Spectrometer A (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spie/1996/tss-1r_m1_spie_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spie/1996/tss-1r_m1_spie_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Ion Spectra From Spectrometer B (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spif/1996/tss-1r_m1_spif_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spif/1996/tss-1r_m1_spif_19960223131953_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 92.4138% of the 134 timesteps. 

TSS-1R, Spectrometer A, Low Frequency Ion Auto-Corellation Spectra IDFS format

Spectrometer A, Low Frequency Ion Auto-Corellation Spectra (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spla/1996/tss-1r_m1_spla_19960223131957_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 41.5094% of the 22 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spla/1996/tss-1r_m1_spla_19960223131957_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 41.5094% of the 22 timesteps. 

TSS-1R, ESA A, Low Frequency Electron Auto-Corellation Spectra IDFS format

ESA A, Low Frequency Electron Auto-Corellation Spectra (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/splb/1996/tss-1r_m1_splb_19960223131957_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 24.7525% of the 25 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/splb/1996/tss-1r_m1_splb_19960223131957_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 24.7525% of the 25 timesteps. 

TSS-1R, Spectrometer B, Low Frequency Ion Auto-Corellation Spectra IDFS format

Spectrometer B, Low Frequency Ion Auto-Corellation Spectra (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/splc/1996/tss-1r_m1_splc_19960223131959_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 26.6667% of the 24 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/splc/1996/tss-1r_m1_splc_19960223131959_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 26.6667% of the 24 timesteps. 

TSS-1R, ESA B, Low Frequency Electron Auto-Corellation Spectra IDFS format

ESA B, Low Frequency Electron Auto-Corellation Spectra (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spld/1996/tss-1r_m1_spld_19960223132001_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 50.0000% of the 21 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spld/1996/tss-1r_m1_spld_19960223132001_v01.cdf. The most common cadence, 1000000000 [ns] = PT1S, occurred for 50.0000% of the 21 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spmf/1996/tss-1r_m1_spmf_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

Orbiter Potential Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spop/1996/tss-1r_m1_spop_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spop/1996/tss-1r_m1_spop_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spsa/1996/tss-1r_m1_spsa_19960223131953_v01.cdf. The most common cadence, 1996800000 [ns] = PT1.9968S, occurred for 48.7179% of the 38 timesteps. 

SPACE Status And Flow Monitor Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spsb/1996/tss-1r_m1_spsb_19960223131958_v01.cdf. The most common cadence, 8000000000 [ns] = PT8S, occurred for 82.3529% of the 14 timesteps. 

DPU and FDR Sense Key Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spsc/1996/tss-1r_m1_spsc_19960223131953_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.6667% of the 112 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/spree/spsd/1996/tss-1r_m1_spsd_19960223131953_v01.cdf. The most common cadence, 499200000 [ns] = PT0.4992S, occurred for 87.3333% of the 262 timesteps. 

DCORE and SETS Gun Status (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: Ivan Linscott at Stanford University

SPDF/SSCWeb. Please also acknowledge the data producer: Ivan Linscott at Stanford University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Ivan Linscott at Stanford University

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/staa/1996/tss-1r_m1_staa_19960222230942_v01.cdf. The most common cadence, 499200000 [ns] = PT0.4992S, occurred for 87.4626% of the 5267 timesteps. 

Current and Charge Probe, Peak Monitors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stca/1996/tss-1r_m1_stca_19960222230942_v01.cdf. The most common cadence, 41600000 [ns] = PT0.0416S, occurred for 98.9555% of the 71531 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stca/1996/tss-1r_m1_stca_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 3.1209% of the 2256 timesteps. 

Direct Current and Charge Probe Monitors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stcb/1996/tss-1r_m1_stcb_19960222230942_v01.cdf. The most common cadence, 41600000 [ns] = PT0.0416S, occurred for 98.9555% of the 71531 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stcb/1996/tss-1r_m1_stcb_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 3.1209% of the 2256 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stcc/1996/tss-1r_m1_stcc_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stcd/1996/tss-1r_m1_stcd_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

SETS CCP Monitor Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stda/1996/tss-1r_m1_stda_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

DEP and Timing Information (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stdb/1996/tss-1r_m1_stdb_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

DEP Operation Timing Information (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stdc/1996/tss-1r_m1_stdc_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

DEP: CPU, GMT and Multibus Time (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stfa/1996/tss-1r_m1_stfa_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stfb/1996/tss-1r_m1_stfb_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stma/1996/tss-1r_m1_stma_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

SRPA, SPIB and AMAG Power Status Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stmb/1996/tss-1r_m1_stmb_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

SETS AMAG And SPIB Monitors (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stsa/1996/tss-1r_m1_stsa_19960222230942_v01.cdf. The most common cadence, 249600000 [ns] = PT0.2496S, occurred for 93.7324% of the 11291 timesteps. 

Spherical Retarding Potential Analyzer (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stsb/1996/tss-1r_m1_stsb_19960222230942_v01.cdf. The most common cadence, 249600000 [ns] = PT0.2496S, occurred for 93.7324% of the 11291 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stsb/1996/tss-1r_m1_stsb_19960222230942_v01.cdf. The most common cadence, 249600000 [ns] = PT0.2496S, occurred for 93.7324% of the 11291 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stsc/1996/tss-1r_m1_stsc_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/stta/1996/tss-1r_m1_stta_19960222230942_v01.cdf. The most common cadence, 41600000 [ns] = PT0.0416S, occurred for 98.9555% of the 71531 timesteps. 

TCVM Tether Current Monitor (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: Brian Gilchrist at Unversity of Michigan

SPDF/SSCWeb. Please also acknowledge the data producer: Brian Gilchrist at Unversity of Michigan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Brian Gilchrist at Unversity of Michigan

Tether Voltage Monitor (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/sttb/1996/tss-1r_m1_sttb_19960222230942_v01.cdf. The most common cadence, 2773000 [ns] = PT0.002773S, occurred for 87.7190% of the 860522 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/sttb/1996/tss-1r_m1_sttb_19960222230942_v01.cdf. The most common cadence, 41595000 [ns] = PT0.041595S, occurred for 5.6199% of the 55131 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/sttc/1996/tss-1r_m1_sttc_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

SETS TCVM Monitor Data (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/sets/sttd/1996/tss-1r_m1_sttd_19960222230942_v01.cdf. The most common cadence, 998400000 [ns] = PT0.9984S, occurred for 74.9169% of the 2255 timesteps. 

TCVM Relay Status Data (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. Franco Mariani at University of Vergata, Departmento Fisica

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. Franco Mariani at University of Vergata, Departmento Fisica

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. Franco Mariani at University of Vergata, Departmento Fisica

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmha/1996/tss-1r_m1_tmha_19960223180013_v01.cdf. The most common cadence, 512000000 [ns] = PT0.512S, occurred for 97.2899% of the 6785 timesteps. 

Housekeeping Data   (TMHA) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmhb/1996/tss-1r_m1_tmhb_19960223180013_v01.cdf. The most common cadence, 512000000 [ns] = PT0.512S, occurred for 97.3330% of the 6788 timesteps. 

Telecommand Echo And Checksum  (TMHB) (from all.xml/instrument/description/@short)

Satellite Inboard Magnetometer Data  (TMMI) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmmi/1996/tss-1r_m1_tmmi_19960223180013_v01.cdf. The most common cadence, 512000000 [ns] = PT0.512S, occurred for 56.5691% of the 6226 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmmi/1996/tss-1r_m1_tmmi_19960223180013_v01.cdf. The most common cadence, 512000000 [ns] = PT0.512S, occurred for 60.6124% of the 6671 timesteps. 

TSS-1R, Satellite Outboard Magnetometer Data  (TMMO) IDFS format

Satellite Outboard Magnetometer Data  (TMMO) (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmmo/1996/tss-1r_m1_tmmo_19960223180013_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 96.1081% of the 49759 timesteps. 

Counts based on variable 'Mode_Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmmo/1996/tss-1r_m1_tmmo_19960223180013_v01.cdf. The most common cadence, 512000000 [ns] = PT0.512S, occurred for 10.6617% of the 5520 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/tss/tss-1r/cdf/temag/tmta/1996/tss-1r_m1_tmta_19960223180013_v01.cdf. The most common cadence, 64000000 [ns] = PT0.064S, occurred for 99.6649% of the 55619 timesteps. 

Tether Current   (TMTA) (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: D. McComas at Southwest Research Institute

SPDF/SSCWeb. Please also acknowledge the data producer: D. McComas at Southwest Research Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. McComas at Southwest Research Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins1/ephemeris/att/2007/twins1_at_def_20070401_v01.cdf. The most common cadence, 1024 [ms] = PT1.024S, occurred for 90.2406% of the 61073 timesteps. 

TWINS (Two Wide-angle Imaging Neutral-atom Spectrometers) is a Mission of Opportunity under NASA's Small Explorer (SMEX) program. TWINS-1 and TWINS-2 are the designations for NASA-sponsored instruments flying on unspecified non-NASA U.S. government spacecraft.The TWINS-1 instrument high voltages were turned on in April 2007 and the TWINS-2 high voltages in May 2008; the exact launchdates are not available. The data (including both science data and spacecraft ephemeris/attitude information) from the two NASA-funded science instruments are publicly available to the scientific research community.  See http://twins.swri.edu/TWINS is a stereo mission whose overall scientific objective is to establish the global connectivities and causal relationships between processes in different regions of the Earth.s magnetosphere. To meet this goal, TWINS-1 and TWINS-2 provide stereoscopic neutral atom imaging of the magnetosphere from two widely spaced, high-altitude, high-inclination spacecraft. TWINS instrumentation includes an energetic neutral atom (ENA) imager to capture charge-exchange-produced neutral atoms over a broad energy range (approximately 1-100 keV) and a Lyman-alpha detector to measure the density of the neutral hydrogen geocorona needed for extraction of magnetospheric ion fluxes from neutral atom data.The TWINS-1 and TWINS-2 instruments are identical. Each spacecraft carrying TWINS instruments is in a Molniya orbit (63.4 deg, 7.2 Re apogee, 1000 km perigee; period 12 h), and is three-axis stabilized and approximately nadir-pointing. Each acquires image data with time resolution of 60 s. The time required to change actuator direction between scans (no data collection) was 25 seconds from June 2008 to July 2009, and 12 seconds at all other times.  This gives an effective cadence of 72 or 85 seconds.  The nominal design lifetime for each instrument is four years. TWINS operates  only during the apogee portion of each orbit, when the spacecraft is above the radiation belts.More detailed information is available at the TWINS home page http://twins.swri.edu/

SPDF/CDAWeb. Please also acknowledge the data producer: D. McComas & H. Fahr at SwRI & U. Bonn, respectively.

SPDF/SSCWeb. Please also acknowledge the data producer: D. McComas & H. Fahr at SwRI & U. Bonn, respectively.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. McComas & H. Fahr at SwRI & U. Bonn, respectively.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins1/housekeeping_cdf/2007/twins1_hk_1sec_20070130_v01.cdf. The most common cadence, 1333 [ms] = PT1.333S, occurred for 97.9478% of the 12982 timesteps. 

Two Wide-angle Imaging Neutral-atom Spectrometers (from all.xml/observatory/description/@short)

Two Wide-angle Imaging Neutral-atom Spectrometers (from Master/CDFglobalAttributes/Source_name)

TWINS Spacecraft 1 - Neutral-atom Spectrometer Level-1 Magnetospheric Images and Image Movies at Full (9 Energy Steps and 15 minute) Resolution

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins1/imager/2007/twins1_l1_imager_2007041800_v01.cdf. The most common cadence, 901000 [ms] = PT15M1S, occurred for 22.8070% of the 13 timesteps. 

Attitude Variation (degrees) during the time interval of each image. 

Average spacecraft position vector in ECI coordinates (time series)

TWINS Spacecraft 1 - Lyman Alpha Detector Level-1 Geocorona Data

TWINS (Two Wide-angle Imaging Neutral-atom Spectrometers) is a Mission of Opportunity under NASA's Small Explorer (SMEX) program. TWINS-1 and TWINS-2 are the designations for NASA-sponsored instruments flying on unspecified non-NASA U.S. government spacecraft.The TWINS-1 instrument high voltages were turned on in April 2007 and the TWINS-2 high voltages in May 2008; the exact launchdates are not available. The data (including both science data and spacecraft ephemeris/attitude information) from the two NASA-funded science instruments are publicly available to the scientific research community.  See http://twins.swri.edu/TWINS is a stereo mission whose overall scientific objective is to establish the global connectivities and causal relationships between processes in different regions of the Earth.s magnetosphere. To meet this goal, TWINS-1 and TWINS-2 provide stereoscopic neutral atom imaging of the magnetosphere from two widely spaced, high-altitude, high-inclination spacecraft. TWINS instrumentation includes an energetic neutral atom (ENA) imager to capture charge-exchange-produced neutral atoms over a broad energy range (approximately 1-100 keV) and a Lyman-alpha detector to measure the density of the neutral hydrogen geocorona needed for extraction of magnetospheric ion fluxes from neutral atom data.The TWINS-1 and TWINS-2 instruments are identical. Each spacecraft carrying TWINS instruments is in a Molniya orbit (63.4 deg, 7.2 Re apogee, 1000 km perigee; period 12 h), and is three-axis stabilized and approximately nadir-pointing. Each acquires image data with time resolution of 60 s. The time required to change actuator direction between scans (no data collection) was 25 seconds from June 2008 to July 2009, and 12 seconds at all other times.  This gives an effective cadence of 72 or 85 seconds.  The nominal design lifetime for each instrument is four years. TWINS operates  only during the apogee portion of each orbit, when the spacecraft is above the radiation belts.The TWINS Lyman-a Detector  consists of two independent  sensors to measure     Lyman alpha radiation being  emitted by neutral hydrogen atoms.  The sensors oriented at angles of  ..40 deg. with respect to the actuator  spin axis. Each sensor has a FWHM field  of view of 4 deg., defined by collimation hole baffles, uses Lyman-a interference filters as  narrow band transmissions filters,  and applies a KBr or CsI photodiode for  photon detection. The Lyman-a detector is   located on the rotating actuator platform  to provide full 360 deg. azimuthal angle coverage Time resolution is 60 sec.More detailed information is available at the TWINS home page http://twins.swri.edu/

Initial Inventory CDAWeb Two Wide-angle Imaging Neutral-atom Spectrometers, TWINS, List of Events and Sample Plots

Two Wide-angle Imaging Neutral-atom Spectrometers, TWINS, Release Notes and other Information, Southwest Research Institute, SwRI, Web Site

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins1/lad/2007/twins1_l1_lad_20070706_v01.cdf. The most common cadence, 1333 [ms] = PT1.333S, occurred for 2.9938% of the 808 timesteps. 

[Diagnostic Use Only] LAD photon intensities from the Toward LAD sensor with 0 degree offset 

[Diagnostic Use Only] LAD photon intensities from the Away LAD sensor with 0 degree offset 

[Diagnostic Use Only] LAD photon intensities from the Toward LAD sensor with 2 degree offset 

[Diagnostic Use Only] LAD photon intensities from the Away LAD sensor with 2 degree offset 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins1/ephemeris/or/2007/twins1_or_def_20070401_v01.cdf. The most common cadence, 105000 [ms] = PT1M45S, occurred for 20.0617% of the 65 timesteps. 

Images of plasma sheet ion temperature during storms calculated from ENA measurements

SPDF/CDAWeb. Please also acknowledge the data producer: Amy Keesee at West Virginia University

SPDF/SSCWeb. Please also acknowledge the data producer: Amy Keesee at West Virginia University

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Amy Keesee at West Virginia University

Two Wide-angle Imaging Neutral-atom Spectrometers 1 (from all.xml/observatory/description/@short)

Two Wide-angle Imaging Neutral-atom Spectrometers 1 (from Master/CDFglobalAttributes/Source_name)

[NO PLOT] Average ENA flux images for different energies projected along the LOS to the bins in the GSM xy plane

[NO PLOT] countarrays: Number of flux values in each energy-spatial bin

Ion temperature images calculated from ENA fluxes in each GSM spatial bin

[NO PLOT] Error in each energy-space bin based on the error given by the algorithm that calculates the flux from the raw TWINS data.

[NO PLOT] Another error value determined as 1/sqrt(countarrays).

Uncertainty in the angle that gives the direction in which the TWINS instrument is pointing.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins2/ephemeris/att/2008/twins2_at_def_20080414_v01.cdf. The most common cadence, 1024 [ms] = PT1.024S, occurred for 84.1730% of the 50609 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins2/housekeeping_cdf/2008/twins2_hk_1sec_20080411_v01.cdf. The most common cadence, 1333 [ms] = PT1.333S, occurred for 97.2118% of the 35877 timesteps. 

TWINS Spacecraft 2 - Neutral-atom Spectrometer Level-1 Magnetospheric Images and Image Movies at Full (9 Energy Steps and 15 minute) Resolution

TWINS (Two Wide-angle Imaging Neutral-atom Spectrometers) is a Mission of Opportunity under NASA's Small Explorer (SMEX) program. TWINS-1 and TWINS-2 are the designations for NASA-sponsored instruments flying on unspecified non-NASA U.S. government spacecraft.The TWINS-1 instrument high voltages were turned on in April 2007 and the TWINS-2 high voltages in May 2008; the exact launchdates are not available. The data (including both science data and spacecraft ephemeris/attitude information) from the two NASA-funded science instruments are publicly available to the scientific research community. See http://twins.swri.edu/TWINS is a stereo mission whose overall scientific objective is to establish the global connectivities and causal relationships between processes in different regions of the Earth.s magnetosphere. To meet this goal, TWINS-1 and TWINS-2 provide stereoscopic neutral atom imaging of the magnetosphere from two widely spaced, high-altitude, high-inclination spacecraft. TWINS instrumentation includes an energetic neutral atom (ENA) imager to capture charge-exchange-produced neutral atoms over a broad energy range (approximately 1-100 keV) and a Lyman-alpha detector to measure the density of the neutral hydrogen geocorona needed for extraction of magnetospheric ion fluxes from neutral atom data.The TWINS-1 and TWINS-2 instruments are identical. Each spacecraft carrying TWINS instruments is in a Molniya orbit (63.4 deg, 7.2 Re apogee, 1000 km perigee; period 12 h), and is three-axis stabilized and approximately nadir-pointing. Each acquires image data with time resolution of 60 s. The time required to change actuator direction between scans (no data collection) was 25 seconds from June 2008 to July 2009, and 12 seconds at all other times.  This gives an effective cadence of 72 or 85 seconds.  The nominal design lifetime for each instrument is four years. TWINS operates  only during the apogee portion of each orbit, when the spacecraft is above the radiation belts.More detailed information is available at the TWINS home page http://twins.swri.edu/ 

TWINS Spacecraft 2 - Lyman Alpha Detector Level-1 Geocorona Data

TWINS (Two Wide-angle Imaging Neutral-atom Spectrometers) is a Mission of Opportunity under NASA's Small Explorer (SMEX) program. TWINS-1 and TWINS-2 are the designations for NASA-sponsored instruments flying on unspecified non-NASA U.S. government spacecraft.The TWINS-1 instrument high voltages were turned on in April 2007 and the TWINS-2 high voltages in May 2008; the exact launchdates are not available. The data (including both science data and spacecraft ephemeris/attitude information) from the two NASA-funded science instruments are publicly available to the scientific research community.  See http://twins.swri.edu/TWINS is a stereo mission whose overall scientific objective is to establish the global connectivities and causal relationships between processes in different regions of the Earth.s magnetosphere. To meet this goal, TWINS-1 and TWINS-2 provide stereoscopic neutral atom imaging of the magnetosphere from two widely spaced, high-altitude, high-inclination spacecraft. TWINS instrumentation includes an energetic neutral atom (ENA) imager to capture charge-exchange-produced neutral atoms over a broad energy range (approximately 1-100 keV) and a Lyman-alpha detector to measure the density of the neutral hydrogen geocorona needed for extraction of magnetospheric ion fluxes from neutral atom data.The TWINS-1 and TWINS-2 instruments are identical. Each spacecraft carrying TWINS instruments is in a Molniya orbit (63.4 deg, 7.2 Re apogee, 1000 km perigee; period 12 h), and is three-axis stabilized and approximately nadir-pointing. Each acquires image data with time resolution of 60 s. The time required to change actuator direction between scans (no data collection) was 25 seconds from June 2008 to July 2009, and 12 seconds at all other times.  This gives an effective cadence of 72 or 85 seconds.  The nominal design lifetime for each instrument is four years. TWINS operates  only during the apogee portion of each orbit, when the spacecraft is above the radiation belts.More detailed information is available at the TWINS home page http://twins.swri.edu/The TWINS Lyman-a Detector consists of two independent sensors to measure Lyman alpha  radiation being emitted by neutral hydrogen atoms. The sensors oriented at angles of ..40 deg. with respect to the actuator spin axis. Each sensor has a FWHM field of view of 4 deg., defined by collimation hole baffles, uses Lyman-a interference filters as narrow band transmissions filters, and applies a KBr or CsI photodiode for photon detection. The Lyman-a detector is located on the rotating actuator platform to provide full 360 deg. azimuthal angle coverage Time resolution is 60 sec.

SPDF/CDAWeb. Please also acknowledge the data producer: D. McComas & H. Fahr at SwRI & U. Bonn, respectively

SPDF/SSCWeb. Please also acknowledge the data producer: D. McComas & H. Fahr at SwRI & U. Bonn, respectively

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D. McComas & H. Fahr at SwRI & U. Bonn, respectively

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins2/lad/2008/twins2_l1_lad_20080502_v01.cdf. The most common cadence, 1335 [ms] = PT1.335S, occurred for 99.8443% of the 41040 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/twins2/ephemeris/or/2008/twins2_or_def_20080411_v01.cdf. The most common cadence, 420000 [ms] = PT7M, occurred for 29.4118% of the 70 timesteps. 

Katus, R. M., A. M. Keesee, E. Scime, and M. W. Liemohn (2017), Storm time equatorial magnetospheric ion temperature derived from TWINS ENA flux,J. Geophys. Res. Space Physics, 122, 3996, doi:10.1002/2016JA023824.

TWINS Energetic Neutral Atom, Mission of Opportunity, Space Science Reviews publication

McComas, D.J., F. Allegrini, J. Baldonado, B. Blake, P.C. Brandt, J. Burch, J. Clemmons, W. Crain, D. Delapp, R. DeMajistre, D. Everett, H. Fahr, L. Friesen, H. Funsten, J. Goldstein, M. Gruntman, R. Harbaugh, R. Harper, H. Henkel, C. Holmlund, G. Lay, D. Mabry, D. Mitchell, U. Nass, C. Pollock, S. Pope, M. Reno, S. Ritzau, E. Roelof, E. Scime, M. Sivjee, R. Skoug, Sotirelis, T.S., Thomsen, M., Urdiales, C., Valek, P., Viherkanto, K., Weidner, S., Ylikorpi, T., Young, M., and J. Zoennchen. The Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) NASA Mission-of-Opportunity, Space Sci. Rev., 142, 157-231, 2009, DOI: 10.1007/s11214-008-9467-4

Katus et al. (2017) TWINS EUV storm time equatorial magnetospheric ion temperature images, Journal of Geophysical Research: Space Physics publication

Katus, R.M., D.L. Gallagher, M.W. Liemohn, A.M. Keesee, and L.K. Sarno-Smith, Statistical Storm Time Examination of MLT dependent Plasmapause Location derived from IMAGE EUV, J. Geophys. Res. Space Phys., 120, 5545-5559, 2015, DOI: 10.1002/2015JA021225.

General information concerning the Two Wide-angle Imaging Neutral-atom Spectrometer 1, TWINS 1, Energetic Neutral Atom, ENA, imager

General information concerning the Two Wide-angle Imaging Neutral-atom Spectrometer 2, TWINS 2, Energetic Neutral Atom, ENA, imager

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/twins/combined/ena/m2/2009/twins_m2_ena_20090409_v05.cdf. The most common cadence, 1439999994635 [ns] = PT23M59.999995S, occurred for all 1 timesteps. 

energetic neutral atom imager (from all.xml/instrument/description/@short)

The 5-level quality flag for data coverage. 5-level quality flag for data coverage. 5 > 95%, 4 > 90%, 3 > 75%, 2 > 50%, 1 > 25%

Overlap of TWINS error array and the overlapped identified active regions. Error_array comes from the estimation of the error in the flux values from the statistical smoothing algorithm. 0 = good quality, 1 = bad

The Count_Error spatial map. The Count_Error is the energy averaged from raw counts per instrument pixel

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/helio1day/ulysses_helio1day_position_19901007_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 6840 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/helio1hr/ulysses_helio1hr_position_19901007_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 519263 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/uranus_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/uranus_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

This data set contains 1 minute data of the magnetic field components (RTN) and field magnitude from the Vector Helium Magnetometer.Units are nT.Data Set Contact: Joyce Wolf,NASA JPL Principal Investigator: A Balogh, The Blackett Laboratory, Imperial College, London, UK.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 221-236 (1992).Relevant Web Sites: http://www.sp.ph.ic.ac.uk/Ulysses/

SPDF/CDAWeb. Please also acknowledge the data producer: A. Balogh at Imperial College, London, UK

SPDF/SSCWeb. Please also acknowledge the data producer: A. Balogh at Imperial College, London, UK

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: A. Balogh at Imperial College, London, UK

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/mag_cdaweb/vhm_1min/1990/uy_1min_vhm_19901025_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for 99.7689% of the 1727 timesteps. 

Vector Helium Magnetometer (from all.xml/instrument/description/@short)

This data set contains 1 second data of the magnetic field components (RTN) and field magnitude from the Vector Helium Magnetometer.Units are nT.Data Set Contact: Joyce Wolf,NASA JPL Principal Investigator: A Balogh, The Blackett Laboratory, Imperial College, London, UK.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 221-236 (1992).Relevant Web Sites: http://www.sp.ph.ic.ac.uk/Ulysses/

Site hosting instrument information, data and plots for Ulysses magnetometer

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/mag_cdaweb/vhm_1sec/1990/uy_1sec_vhm_19901025_v01.cdf. The most common cadence, 500 [ms] = PT0.5S, occurred for 72.0856% of the 19089 timesteps. 

This file contains the distribution function of alpha particles. DATA REDUCTION: The SWOOPS (Solar Wind Observations Over the Poles of the Sun) ion instrument is a spherical-section curved-plate electrostatic analyzer. Particle arrival directions are measured in spacecraft coordinates of azimuth (scanned by spacecraft rotation) and elevation (determined by the detector number) angles. The spacecraft spin axis was oriented toward the Earth. The energy/charge (E/q) resolution was ~2.5% while the azimuth (phi) and elevation (theta) resolutions were both ~5.6o. A description of the SWOOPS is given in a paper by S. J. Bame, D. J. McComas, B. L. Barraclough, J. L. Phillips, K. J. Sofaly, J. C. Chavez, B. E. Goldstein, and R. K. Sakurai, Astronomy and Astrophysics Supplement Series, Ulysses Instruments Special Issue, Vol. 92, No. 2, p.237-265, 1992. The number of counts in each E/q-phi-theta bin were examined to determine the peak of the proton and alpha particle distribution, respectively, and the vector magnetic field (in spacecraft coordinates) was obtained for the time at which the peak was measured. A "coarse" 2-dimensional matrix was then formed by rotating the data into a coordinate system with axes parallel and perpendicular to the field direction. Note that gyrotropy is assumed in making that transformation. The resolution of the matrix is "coarse" because the vector velocity assigned to each bin was taken to be at the center of the bin. In reality, the counts in each bin were probably not smoothly distributed in velocity space over the bin, but were weighted toward the part of the bin nearest the center of the peak of the velocity distribution. The "coarse" distribution would thus yield values for the density and temperature that were higher than the true values. A correction for that effect was accomplished by fitting contours to the coarse distribution, breaking each bin or pixel into subpixels, and then using the contours and the calibrated angular responses to distribute the counts among the subpixels. New contours were then computed and the process was continued until it converged. More details about this deconvolution of the angular data are given in the appendix of a paper by Neugebauer, M., et al., "Ion distributions in large magnetic holes in the fast solar wind", J. Geophys. Res.,106, 5635, 2001. This procedure generated the matrix of velocity distribution functions of protons and alpha-particles parallel and perpendicular to the simultaneously measured magnetic field.

The Ulysses Solar Wind Observations Over the Poles of the Sun, SWOOPS, Instrument Web Page hosted at the Los Alamos National Laboratory, LANL

SPDF/CDAWeb. Please also acknowledge the data producer: David. J. McComas at Princeton/PPPL

SPDF/SSCWeb. Please also acknowledge the data producer: David. J. McComas at Princeton/PPPL

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: David. J. McComas at Princeton/PPPL

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/alpha-distributions_swoops/1990/uy_alpha-distributions_swoops_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 39.6467% of the 1526 timesteps. 

Solar Wind Plasma Distribution Function (from Master/CDFglobalAttributes/Data_type)

This file contains  the parameters obtained by fitting data to a bi-maxwellian core-beam distribution. Under normal circumstances, the first (slow) population is the core and the second (fast) population is the beam. When the interplanetary magnetic field is folded back on itself due to turbulence or other processes the relation of the first and second populations to the core and beam, respectively, is reversed (see, e.g, M. Neugebauer and B. E. Goldstein, AIP Conf. Proc. 1539, 46, 2013). The vector magnetic field is given in  RTN coordinates and it was obtained for the time at which the peak of the alpha distribution function was measured. Only good fits are retained.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/alpha-fit-parameters_swoops/1990/uy_alpha-fit-parameters_swoops_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 39.6467% of the 1526 timesteps. 

Magnetic field component BN in inertial RTN coordinates                  

This file contains the moments obtained from the distribution function of alpha particles after deconvolution using the same magnetic field values used to construct the matrices. The vector magnetic field and the particle velocity are given in inertial RTN coordinates. The magnetic field was obtained for the time at which the peak of the alpha distribution function was measured. The particle velocity was obtained after rotating the fluid velocity from spacecraft to RTN coordinates and taking into account the spacecraft velocity. During periods of spacecraft nutation only the bulk speed and density are reliable, individual velocity components and temperatures are invalid. The beginning of scientifically useful SWOOPS data is at Day 322, 00:59 of 1990; at that time the spacecraft was already nutating; nutation ceased as of Day 351, 22:00, 1990. There are small systematic uncertainties in the velocity components. These are due to such effects as uncertainty in the accuracy of alignment on the spacecraft, relatively wide angular bins, variation in gains between channeltrons, etc. The velocity component data should not be used for studies of large scale, long term, solar wind deflection. The data are generally suitable for all other studies.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/alpha-moments_swoops/1990/uy_alpha-moments_swoops_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 39.6467% of the 1526 timesteps. 

Alpha particle velocity component VR in inertial RTN coordinates

Alpha particle velocity component VT in inertial RTN coordinates

Alpha particle velocity component VN in inertial RTN coordinates

Ulysses merged hourly magnetic field, plasma, proton fluxes, and ephermis data

ULYSSES data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions:- All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.- calculation of RTN Spherical components of the solar wind velocity from RTN cartesian components:- data are a merging of trajectory coordinates, magnetic field data, proton fluxes, and plasma data files. - Data gaps were filled with -1.e31. Note that an COHOWeb interface to this dataset, providing data subsetting and and graphical browsing, is available at https://omniweb.gsfc.nasa.gov/coho/The difference between T (Large) and T (Small) is discussed at https://spdf.gsfc.nasa.gov/pub/data/ulysses/plasma/swoops/ion/swoops_ion_users_guide_update_20030214.txtThe Heliographic Inertial (HGI) coordinates are Sun-centered and inertially fixed with respect to an X-axis directed along the intersection line of the ecliptic and solar equatorial  planes. The solar equator plane is inclined at 7.25 degrees from the ecliptic. This direction was towards ecliptic longitude of 74.36 degrees  on  1  January  1900  at  1200  UT; because of precession of the celestial equator, this longitude increases by 1.4 degrees/century. The Z axis is directed perpendicular and northward from the solar equator, and the Y-axis completes the right-handed set. This system differs from the usual heliographic coordinates (e.g. Carrington longitudes) which are fixed in the frame of the rotating Sun.The RTN system is fixed at a spacecraft (or the planet). The R axis is directed radially away from the Sun, the T axis is the cross product of the solar rotation axis and the R axis, and the N axis is the cross product of R and T.  At zero Heliographic Latitude when the spacecraft is in the solar equatorial plane the N and solar rotation axes are parallel.

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. A. Balogh (magnetic field), Dr. John L. Phillips (plasma) at Imperial College, London, UK,

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. A. Balogh (magnetic field), Dr. John L. Phillips (plasma) at Imperial College, London, UK,

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. A. Balogh (magnetic field), Dr. John L. Phillips (plasma) at Imperial College, London, UK,

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/merged/coho1hr_magplasma/1990/uy_coho1hr_merged_mag_plasma_19900101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Merged Trajectory, Magnetic Field, Proton Fluxes, and Plasma (from all.xml/instrument/description/@short)

The Ulysses/SWICS instrument is a mass spectrometer combining an electrostatic analyzer with post acceleration, followed by a time-of-flight and energy measurement. The instrument covers an energy per charge range from 0.16 to 59.6 keV/e with a time resolution of about 13 minutes.SWICS is designed to determine uniquely the elemental and ionic-charge composition, the temperatures and mean speeds of all major solar wind ions, from H through Fe. For more information see G. Gloeckler, J. Geiss et al., Astron. Astrophys. Suppl. Ser. 92, 267-289, 1992.This archive consists of all 18 Matrix Rates (MR) as a function of energy per charge (E/q) and of time. Each MR represents a specific element in one or several ionization states, but it may also contain significant contributions from neighbouring elements due to spillover. The MRs are given in units of count rates only. The accompanying SAPRO (SWICS Archive Processor) software can be used both to convert the MR count rates to physical units (differential flux, phase space density), to correct for spillover between different MRs, and to obtain kinetic parameters (density, speed, thermal speed) of selected ions (to be used with caution).

Ulysses Solar Wind Ion Composition Spectrometer, SWICS GLG Operations Web Page

Ulysses , SWICS, GLG Operations Web Page. The SWICS GLG Experiment determines the Elemental and Ionic-Charge Composition, Temperatures and Mean Speeds of all major Solar Wind Ions from Hydrogen, H, through Iron, Fe, at Solar Wind Speeds ranging from 175 km/s to 1280 km/s.

These data can reasonably be used only in collaboration with a member of the 

SPDF/CDAWeb. Please also acknowledge the data producer: G. Gloeckler, J. Geiss at Department of Physics, University of Maryland, College Park, Maryland, USA;

SPDF/SSCWeb. Please also acknowledge the data producer: G. Gloeckler, J. Geiss at Department of Physics, University of Maryland, College Park, Maryland, USA;

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Gloeckler, J. Geiss at Department of Physics, University of Maryland, College Park, Maryland, USA;

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swics_cdaweb/glg_h0/1990/uy_h0_glg_19901108_v01.cdf. The most common cadence, 779000 [ms] = PT12M59S, occurred for 93.3333% of the 14 timesteps. 

Solar Wind Ion Composition Spectrometer (SWICS) (from all.xml/instrument/description/@short)

H+, protons, measured in triple coincidence. Note: CDF_UINT4 data was converted to HAPI double.

4He++, alpha particles, measured in triple coincidence. Note: CDF_UINT4 data was converted to HAPI double.

H+, protons, measured in double coincidence. Note: CDF_UINT4 data was converted to HAPI double.

4He+, singly charged helium, measured in double coincidence. Note: CDF_UINT4 data was converted to HAPI double.

Heavy ions with m/q>10, measured in double coincidence. Note: CDF_UINT4 data was converted to HAPI double.

C4+ and C5+ nominal, with spillover from N and O. Note: CDF_UINT4 data was converted to HAPI double.

C6+ nominal, with spillover from N and O. Note: CDF_UINT4 data was converted to HAPI double.

N5+ to N7+ nominal, with strong spillover from C and O. Note: CDF_UINT4 data was converted to HAPI double.

O6+ nominal, with spillover from C, N, and Ne. Note: CDF_UINT4 data was converted to HAPI double.

O7+ and O8+ nominal, with spillover from C, N, and Ne. Note: CDF_UINT4 data was converted to HAPI double.

Ne8+ nominal, with spillover from O and Mg. Note: CDF_UINT4 data was converted to HAPI double.

Mg6+ to Mg8+ nominal, with spillover from Si. Note: CDF_UINT4 data was converted to HAPI double.

Mg9+ to Mg11+ nominal, with spillover from O, Ne, and Si. Note: CDF_UINT4 data was converted to HAPI double.

Si5+ to Si8+ nominal, with spillover from Mg and S. Note: CDF_UINT4 data was converted to HAPI double.

Si9+ to Si12+ nominal, with spillover from Mg and S. Note: CDF_UINT4 data was converted to HAPI double.

S6+ to S14+ nominal, with spillover from Mg, Si, and Fe. Note: CDF_UINT4 data was converted to HAPI double.

Fe7+ to Fe9+ nominal, with spillover from Si and S. Note: CDF_UINT4 data was converted to HAPI double.

Fe10+ to Fe14+ nominal, with spillover from Si and S. Note: CDF_UINT4 data was converted to HAPI double.

This data set contains 10 minute averages of the proton and Z>=1 flux data from the Ulysses Cosmic Ray and Solar Particle Investigation Anisotropy Telescope 1. Flux units are /cm2/s/sr/Mev. Data Set Contact: S Dalla, Space & Atmospheric Physics Group, Imperial College, London, UK.Principal Investigator: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 365-399 (1992). Relevant web sites: ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.htmlhttp://www.sp.ph.ic.ac.uk/Ulysses/

The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN dual Anisotropy Telescopes, AT1 and AT2, 10 min Average Proton and Helium Spin-Averaged and Sectored Fluxes

SPDF/CDAWeb. Please also acknowledge the data producer: R. McKibben at University of Chicago, USA

SPDF/SSCWeb. Please also acknowledge the data producer: R. McKibben at University of Chicago, USA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. McKibben at University of Chicago, USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/cospin_cdaweb/at1/1991/uy_m0_at1_19910101_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

COSPIN Anisotropy Telescope 1 (from all.xml/instrument/description/@short)

10 minute resolution (from Master/CDFglobalAttributes/Data_type)

Z>=1 flux (0.7-2.2 MeV/n) in 3 channels (A1:0.7-0.9,A2:0.9-1.3,A3:1.3-2.2 MeV/n)

Proton flux (2.2-6.6 MeV) in 2 channels (A4:2.2-3.6, A5:3.6-6.6 MeV)

Z>=2 flux (3.1-23 MeV/n) in 3 channels (A38:3.1-7.2,A39:7.2-12,A40:12-23 MeV/n)

This data set contains 10 minute averages of the proton and Z>=1 flux data from the Ulysses Cosmic Ray and Solar Particle Investigation Anisotropy Telescope 2. Flux units are /cm2/s/sr/Mev. Data Set Contact: S Dalla, Space & Atmospheric Physics Group, Imperial College, London, UK.Principal Investigator: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 365-399 (1992). Relevant web sites: ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.htmlhttp://www.sp.ph.ic.ac.uk/Ulysses/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/cospin_cdaweb/at2/1991/uy_m0_at2_19910101_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

COSPIN Anisotropy Telescope 2 (from all.xml/instrument/description/@short)

This data set contains 3 to 22 minute averages of the electron density and temperature data from the Ulysses Solar Wind Observations Over the Poles of the Sun instrument. Density units are /cm3, temperature units are K. Data Set Contact: B E Goldstein, NASA Ames Research Center, USA. Principal Investigator: D J McComas, Southwest Research Institute, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 237-265 (1992).Relevant Web Sites: http://sst.lanl.gov/nis-projects/swoops/

SPDF/CDAWeb. Please also acknowledge the data producer: D McComas at Southwest Research Institute, USA

SPDF/SSCWeb. Please also acknowledge the data producer: D McComas at Southwest Research Institute, USA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D McComas at Southwest Research Institute, USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/bae_m0/1990/uy_m0_bae_19901118_v02.cdf. The most common cadence, 428000 [ms] = PT7M8S, occurred for 24.7788% of the 28 timesteps. 

SWOOPS Electron Measurements (from all.xml/instrument/description/@short)

3 to 22 minute resolution (from Master/CDFglobalAttributes/Data_type)

This data set contains 4 to 8 minute averages of the ion density, temperature and velocity data from the Ulysses Solar Wind Observations Over the Poles of the Sun instrument. Density units are /cm3, temperature units are K, velocity units are km/s. Data Set Contact: B E Goldstein, NASA Ames Research Center, USA. Principal Investigator: D J McComas, Southwest Research Institute, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 237-265 (1992).Relevant Web Sites: http://sst.lanl.gov/nis-projects/swoops/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/bai_m0/1990/uy_m0_bai_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 70.2381% of the 236 timesteps. 

SWOOPS Ion Measurements (from all.xml/instrument/description/@short)

4 to 8 minute resolution (from Master/CDFglobalAttributes/Data_type)

This data set contains 5 minute resolution filtered averages of cosmic gamma ray and solar X-Ray count rates.Count rate units are c/s. Data Set Contact: R Williams, Space Science Laboratory, University of California, Berkeley, USA.Principal Investigator: K Hurley, Space Science Laboratory,University of California, Berkeley, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 401-410 (1992).Relevant Web Sites: http://www.ssl.berkeley.edu/ipn3/grb.htm

SPDF/CDAWeb. Please also acknowledge the data producer: K Hurley at University of California, Berkeley, USA

SPDF/SSCWeb. Please also acknowledge the data producer: K Hurley at University of California, Berkeley, USA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K Hurley at University of California, Berkeley, USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/gamma/grb_cdaweb/grb_m0/1990/uy_m0_grb_19901110_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for all 287 timesteps. 

Cosmic Gamma Rays and Solar X-Rays (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the proton, electron, and Z>=3 count rate data from the Ulysses Cosmic Ray and Solar Particle Investigation High Energy Telescope. Count rate units are /s. Data Set Contact: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Principal Investigator: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 365-399 (1992).Relevant Web Sites: ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.htmlftp://odysseus.uchicago.edu/WWW/Simpson/UlyDocs/HET.html

The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN High Energy Telescope, HET, 10 min Average Ion and Electron Spin-Averaged Coincidence Counting Rates

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/cospin_cdaweb/het/1990/uy_m0_het_19901023_v02.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 43 timesteps. 

COSPIN High Energy Telescope (from all.xml/instrument/description/@short)

Proton count rate (5-92MeV), 5 channels (H1:5-14,H2:14-19,H3:24-31,H4:34-48,H5:68-92 MeV)

Electron count rate (1-10 MeV) in 3 channels (H6:1-3, H7:5-10, H8:3-5 MeV)

Z>=3 count rate (26-173+ MeV/n), 4 channels (H10:26-36,H11:44-127,H12:127-173,H13:>173 MeV/n)

This data set contains 10 minute averages of the ion flux data from the Ulysses Cosmic Ray and Solar Particle Investigation High Flux Telescope. Flux units are /cm2/s/sr. Data Set Contact: J D Anglin, Herzberg Institute for Astrophysics, National Research Council of Canada, Ottawa, Canada.Principal Investigator: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 365-399 (1992).Relevant Web Sites: ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.htmlFor a fuller description of the data channels and their energy levels see the format file at file://helio.estec.esa.nl/ulysses/cospin/hft/doc/ and Anglin et al., J. Geophys. Res.,  102, 1 (1997). 

The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN High Flux Telescope, HFT, 10 min Average Proton and Heavy Ion Nominal Fluxes

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/cospin_cdaweb/hft/1991/uy_m0_hft_19910101_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

COSPIN High Flux Telescope (from all.xml/instrument/description/@short)

Z>=1 flux (mainly protons), 0.28-2.27 MeV, 3 channels: F1J(0) - F1J(2)

Z>=2 flux (mainly helium), 0.31-5.4 MeV/n, in 11 channels: F1J(3) to F1J(13)

Z>=2 flux (mainly oxygen), >= 0.34 MeV/n, in 2 channels: F1J(14) to F1J(15)

Z>=1 flux (mainly protons), 0.29-6.7 MeV,channels F2L: 0.29-6.7, F2H: 0.55-1.95 MeV

Z>=3 flux (mainly carbon 0.8-4.9 MeV/n, oxygen 0.64-10.7 MeV/n), channel F4

Z>=12 flux (mainly sulphur 1.28-8.5, iron 0.8-34 MeV/n), channel F5

This data set contains 10 minute averages of the proton, helium, and electron count rate data from theUlysses Cosmic Ray and Solar Particle Kiel Electron Telescope. Count rate units are /s. Data Set Contact: B Heber, CEA, DSM, Service d'Astrophysique, Centre d'Etudes de Saclay,91191 Gif sur Yvette, Cedex, France.Principal Investigator: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 365-399 (1992).Relevant Web Sites: ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.htmlhttp://www.ifctr.mi.cnr.it/Ulysses/

The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN Kiel Electron Telescope Telescope, KET, 10 min Average Proton, Helium and Electron Count Rates and detector Count Rates

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/cospin_cdaweb/ket/1990/uy_m0_ket_19901023_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for 94.1176% of the 32 timesteps. 

COSPIN Kiel Electron Telescope (from all.xml/instrument/description/@short)

Proton count rate (5.4-2100+ MeV), in 5 channels: P4, K3, K34, K12, K10

Helium count rate (6-2100+ MeV) in 5 channels: K2, K33, K29, K31, K30

Electron count rate (2.5-7 MeV) in 8 sectors, channels K13 - K20

Electron count rate (2.5-170+ MeV) (E4:2.5-7, K11:7-170, K32:>170 MeV)

Single detector counts in 6 channels (D10, D20, C10, C20, S20, A01)

This data set contains 10 minute averages of the ion and electron flux data from the Ulysses Cosmic Ray and Solar Particle Investigation Low Energy Telescope. Flux units are /cm2/s/sr/Mev. Data Set Contact: T R Sanderson, Solar System Division, ESA/ESTEC.Principal Investigator: R B McKibben, Laboratory for Astrophysics and Space Research, Enrico Fermi Institute, University of Chicago, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 365-399 (1992).Relevant Web Sites: ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.htmlhttp://helio.estec.esa.nl/ssd/let.html

The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN Low Energy Telescope, LET, 10 min Average Ion and Electron Fluxes and Detector Count Rates

This PDF File at the Ulysses Final Archive (UFA) COSPIN Low Energy Telescope, LET, Handbook and many other appended Documents

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/cospin_cdaweb/let/1990/uy_m0_let_19901023_v02.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

COSPIN Low Energy Telescope (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the average electric field intensities from the Unified Radio and Plasma Wave Instrument Plasma Frequency Receiver.Units are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

SPDF/CDAWeb. Please also acknowledge the data producer: R MacDowall at NASA Goddard Spaceflight Center

SPDF/SSCWeb. Please also acknowledge the data producer: R MacDowall at NASA Goddard Spaceflight Center

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R MacDowall at NASA Goddard Spaceflight Center

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/pfra_m0/1990/uy_m0_pfra_19901029_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Plasma Frequency Receiver (Average Data) (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the peak electric field intensities from the Unified Radio and Plasma Wave Instrument Plasma Frequency Receiver.Units are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/pfrp_m0/1990/uy_m0_pfrp_19901029_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Plasma Frequency Receiver (Peak Data) (from all.xml/instrument/description/@short)

This data set contains 144 second averages of the electric field intensities from the Unified Radio and Plasma Wave Instrument Radio Astronomy Receiver.Units are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Ulysses URAP Instrument page maintained by NASA GSFC with URAP data plotting tools, Data Access, Publication lists, Team member lists, documents, and related links sections

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/r144_m0/1990/uy_m0_r144_19901103_v01.cdf. The most common cadence, 144000 [ms] = PT2M24S, occurred for all 599 timesteps. 

URAP Radio Astronomy Receiver (144 second resolution) (from all.xml/instrument/description/@short)

144 second resolution (from Master/CDFglobalAttributes/Data_type)

This data set contains 10 minute averages of the average electric field intensities from the Unified Radio and Plasma Wave Instrument Radio Astronomy Receiver.Units are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/rara_m0/1990/uy_m0_rara_19901103_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Radio Astronomy Receiver (Average Data) (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the peak electric field intensities from the Unified Radio and Plasma Wave Instrument Radio Astronomy Receiver.Units are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/rarp_m0/1990/uy_m0_rarp_19901103_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Radio Astronomy Receiver (Peak Data) (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the averaged magnetic field intensities from the Unified Radio andPlasma Wave Instrument Waveform AnalyzerUnits are 1.0e-15Tesla/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/wfba_m0/1990/uy_m0_wfba_19901029_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Waveform Analyzer Magnetic Field (Average Data) (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the peak magnetic field intensities from the Unified Radio andPlasma Wave Instrument Waveform AnalyzerUnits are 1.0e-15Tesla/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/wfbp_m0/1990/uy_m0_wfbp_19901029_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Waveform Analyzer Magnetic Field (Peak Data) (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the averaged electric field intensities from the Unified Radio andPlasma Wave Instrument Waveform AnalyzerUnits are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/radio/urap_cdaweb/wfea_m0/1990/uy_m0_wfea_19901029_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

URAP Waveform Analyzer Electric Field (Average Data) (from all.xml/instrument/description/@short)

This data set contains 10 minute averages of the peak electric field intensities from the Unified Radio andPlasma Wave Instrument Waveform AnalyzerUnits are microVolt/Hz**0.5.Data Set Contact: R Hess, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Principal Investigator: R J Macdowall, NASA Goddard Spaceflight Center, Greenbelt, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 291-316 (1992).Relevant Web Sites: http://urap.gsfc.nasa.gov/www/home.html

URAP Waveform Analyzer Electric Field (Peak Data) (from all.xml/instrument/description/@short)

This data set contains 1 hour averages of the ion density, temperature and velocity data from the Ulysses Solar Wind Observations Over the Poles of the Sun instrument. Density units are /cm3, temperature units are K, velocity units are km/s. Data Set Contact: B E Goldstein, NASA Ames Research Center, USA. Principal Investigator: D J McComas, Southwest Research Institute, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 237-265 (1992).Relevant Web Sites: http://sst.lanl.gov/nis-projects/swoops/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/bai_m1/1990/uy_m1_bai_19901118_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 19 timesteps. 

This data set contains 1 hour averages of the proton and electron flux data from the Ulysses Energetic Particle CompositionExperiment. Flux units are /cm2/s/sr. Data Set Contact: M Bruns, Max Planck Institut fur Aeronomie, Lindau, Germany.Principal Investigator: E Keppler, Max Planck Institut fur Aeronomie, Lindau, Germany.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 317-331 (1992).Relevant Web Sites: http://www.mpae.gwdg.de/mpae_projects/ULYSSES/EPAC.html

SPDF/CDAWeb. Please also acknowledge the data producer: E Keppler at Max Planck Institut fur Aeronomie,

SPDF/SSCWeb. Please also acknowledge the data producer: E Keppler at Max Planck Institut fur Aeronomie,

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: E Keppler at Max Planck Institut fur Aeronomie,

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/epac_cdaweb/epac_m1/1990/uy_m1_epa_19901001_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

Energetic Particle Composition Experiment (from all.xml/instrument/description/@short)

Omnidirectional proton flux (0.5-1.5 MeV) Telescopes 1-4 (OPTL1-OPTL4)

Omnidirectional event rate, low, medium & high (channels ERL, ERM, ERH)

Proton Telescope 1 flux in 8 energy channels (0.5-1.5 MeV) and 8 sectors/channel: x>energy y>sector

Proton Telescope 2 flux in 8 energy channels (0.5-1.5 MeV) and 8 sectors/energy: x>energy y>sector

Proton Telescope 3 flux in 8 energy channels (0.5-1.5 MeV) and 8 sectors/energy: x>energy y>sector

Proton Telescope 4 flux in 8 energy channels (0.5-1.5 MeV) and 8 sectors/energy: x>energy y>sector

This data set contains 1 hour spinaveraged count rates of the electron and ion data from the Ulysses HeliosphereInstrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 150 degrees to the spacecraft spin axis.Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

SPDF/CDAWeb. Please also acknowledge the data producer: L. Lanzerotti at Bell Laboratories, USA

SPDF/SSCWeb. Please also acknowledge the data producer: L. Lanzerotti at Bell Laboratories, USA

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: L. Lanzerotti at Bell Laboratories, USA

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/lf15_m1/1990/uy_m1_lf15_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

Electron counts in channels E1:40-65,E2:60-107,E3:107-170 and E4:170-280 keV

Ion counts in channels FP5:540-765, FP6:765-1223 and FP7:1223-4942 keV

This data set contains 1 hour spinaveraged count rates of the electron and ion data from the Ulysses HeliosphereInstrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 60 degrees to the spacecraft spin axis.Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/lf60_m1/1990/uy_m1_lf60_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

Electron counts in channels E1':42-65,E2':64-112,E3':112-178 and E4':178-290 keV

Ion counts in channels FP5':546-761, FP6':761-1223 and FP7':1223-4974 keV

This data set contains 1 hour spinaveraged count rates of the ion data from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Magnetic Spectrometer at 120 degrees to the spacecraft spin axis.Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/lm12_m1/1990/uy_m1_lm12_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

This data set contains 1 hour spinaveraged count rates of the ion data from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Magnetic Spectrometer at 30 degrees to the spacecraft spin axis.Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/lm30_m1/1990/uy_m1_lm30_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

This data set contains 1 hour spinaveraged count rates of the deflected electron data from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Magnetic Spectrometer at 30 degrees to the spacecraft spin axis.Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/lmde_m1/1990/uy_m1_lmde_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

This data set contains 3.5 hour averages of the solar wind ion density ratio (to O6+), velocity and temperature from the Ulysses Solar Wind Ion Composition Spectrometer.Velocity units are km/s. Ratios and Fe Charge State have no unitsData Set Contact: R von Steiger, International Space Science Institute, Bern, Switzerland.Principal Investigators: J Geiss, International Space Science Institute,Bern, Switzerland, and G Gloeckler, University of Maryland, College Park, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 267-289 (1992).Relevant Web Sites: http://space.umd.edu/UMD_sensors/uls_swics.html

SPDF/CDAWeb. Please also acknowledge the data producer: J Geiss, G Gloeckler at International Space Science Institute,

SPDF/SSCWeb. Please also acknowledge the data producer: J Geiss, G Gloeckler at International Space Science Institute,

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: J Geiss, G Gloeckler at International Space Science Institute,

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swics_cdaweb/scs_m1/1990/uy_m1_scs_19901207_v02.cdf. The most common cadence, 4640000 [ms] = PT1H17M20S, occurred for all 1 timesteps. 

Solar Wind Ion Composition Spectrometer: Charge States (from all.xml/instrument/description/@short)

This data set contains 3.5 hour averages of the solar wind ion density ratio (to O6+), velocity and temperature from the Ulysses Solar Wind Ion Composition Spectrometer.Velocity units are km/s. Temperature units are K. Data Set Contact: R von Steiger, International Space Science Institute, Bern, Switzerland.Principal Investigators: J Geiss, International Space Science Institute,Bern, Switzerland, and G Gloeckler, University of Maryland, College Park, Maryland, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 267-289 (1992).Relevant Web Sites: http://space.umd.edu/UMD_sensors/uls_swics.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swics_cdaweb/swi_m1/1990/uy_m1_swi_19901207_v02.cdf. The most common cadence, 4640000 [ms] = PT1H17M20S, occurred for all 1 timesteps. 

Density ratio to O6+ of 8 species (Alphas,C6+,O6+,Ne8+,Mg10+,Si9+,S10+,Fe11+)

Velocity of 8 species (Alphas,C6+,O6+,Ne8+,Mg10+,Si9+,S10+,Fe11+)

Temperature of 8 species (Alphas,C6+,O6+,Ne8+,Mg10+,Si9+,S10+,Fe11+)

This data set contains 1 hour averages of the magnetic field components (RTN) and field magnitude from the Vector Helium Magnetometer.Units are nT.Data Set Contact: R J Forsyth,The Blackett Laboratory, Imperial College, London, UK.Principal Investigator: A Balogh, The Blackett Laboratory, Imperial College, London, UK.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 221-236 (1992).Relevant Web Sites: http://www.sp.ph.ic.ac.uk/Ulysses/

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/mag_cdaweb/vhm_m1/1990/uy_m1_vhm_19901025_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 7 timesteps. 

This data set contains 1 hour spinaveraged count rates of the proton and ion data from the Ulysses HeliosphereInstrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Composition ApertureTelescope at 60 degrees to the spacecraft spin axis.Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/wart_m1/1990/uy_m1_wart_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

HISCALE Composition Aperture Telescope (from all.xml/instrument/description/@short)

Alpha counts in channels W3:0.380-1.278 and W4:1.277-6.984 MeV/n

C, N, and O counts in channels W5:0.465-1.709 and W6:1.709-19.107 MeV/n

Fe group counts in channels W7:0.239-0.840 and W8:0.840-92.663 MeV/n

This data set contains 1 hour spinaveraged count rates of the ion data from the Ulysses HeliosphereInstrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Composition ApertureTelescope at 60 degrees to the spacecraft spin axis (WARTD).Count rate units are /s. Data Set Contact: T P Armstrong, Department of Physics & Astronomy, University of Kansas, USA.Principal Investigator: L J Lanzerotti, Bell Laboratories, Lucent Technologies, Murray Hill, NJ, USA.Reference: Astron. Astrophys. Suppl. Ser., 92(2), 349-363 (1992).Relevant Web Sites: http://sd-www.jhuapl.edu/Ulysses/http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/particle/hiscale_cdaweb/wrtd_m1/1990/uy_m1_wrtd_19901114_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 4 timesteps. 

HI-SCALE Composition Aperture Telescope (from all.xml/instrument/description/@short)

This file contains the distribution function of protons. DATA REDUCTION: The SWOOPS (Solar Wind Observations Over the Poles of the Sun) ion instrument is a spherical-section curved-plate electrostatic analyzer. Particle arrival directions are measured in spacecraft coordinates of azimuth (scanned by spacecraft rotation) and elevation (determined by the detector number) angles. The spacecraft spin axis was oriented toward the Earth. The energy/charge (E/q) resolution was ~2.5% while the azimuth (phi) and elevation (theta) resolutions were both ~5.6o. A description of the SWOOPS is given in a paper by S. J. Bame, D. J. McComas, B. L. Barraclough, J. L. Phillips, K. J. Sofaly, J. C. Chavez, B. E. Goldstein, and R. K. Sakurai, Astronomy and Astrophysics Supplement Series, Ulysses Instruments Special Issue, Vol. 92, No. 2, p.237-265, 1992. The number of counts in each E/q-phi-theta bin were examined to determine the peak of the proton and alpha particle distribution, respectively, and the vector magnetic field (in spacecraft coordinates) was obtained for the time at which the peak was measured. A "coarse" 2-dimensional matrix was then formed by rotating the data into a coordinate system with axes parallel and perpendicular to the field direction. Note that gyrotropy is assumed in making that transformation. The resolution of the matrix is "coarse" because the vector velocity assigned to each bin was taken to be at the center of the bin. In reality, the counts in each bin were probably not smoothly distributed in velocity space over the bin, but were weighted toward the part of the bin nearest the center of the peak of the velocity distribution. The "coarse" distribution would thus yield values for the density and temperature that were higher than the true values. A correction for that effect was accomplished by fitting contours to the coarse distribution, breaking each bin or pixel into subpixels, and then using the contours and the calibrated angular responses to distribute the counts among the subpixels. New contours were then computed and the process was continued until it converged. More details about this deconvolution of the angular data are given in the appendix of a paper by Neugebauer, M., et al., "Ion distributions in large magnetic holes in the fast solar wind", J. Geophys. Res.,106, 5635, 2001. This procedure generated the matrix of velocity distribution functions of protons and alpha-particles parallel and perpendicular to the simultaneously measured magnetic field. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/proton-distributions_swoops/1990/uy_proton-distributions_swoops_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 34.3729% of the 3075 timesteps. 

This file contains  the parameters obtained by fitting data to a bi-maxwellian core-beam distribution. Under normal circumstances, the first (slow) population is the core and the second (fast) population is the beam. When the interplanetary magnetic field is folded back on itself due to turbulence or other processes the relation of the first and second populations to the core and beam, respectively, is reversed (see, e.g, M. Neugebauer and B. E. Goldstein, AIP Conf. Proc. 1539, 46, 2013). The vector magnetic field is given in  RTN coordinates and it was obtained for the time at which the peak of the proton distribution function was measured. Only good fits are retained.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/proton-fit-parameters_swoops/1990/uy_proton-fit-parameters_swoops_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 34.3729% of the 3075 timesteps. 

This file contains the moments obtained from the distribution function of protons after deconvolution using the same magnetic field values used to construct the matrices. The vector magnetic field and the particle velocity are given in inertial RTN coordinates. The magnetic field was obtained for the time at which the peak of the proton distribution function was measured. The particle velocity was obtained after rotating the fluid velocity from spacecraft to RTN coordinates and taking into account the spacecraft velocity. During periods of spacecraft nutation only the bulk speed and density are reliable, individual velocity components and temperatures are invalid. The beginning of scientifically useful SWOOPS data is at Day 322, 00:59 of 1990; at that time the spacecraft was already nutating; nutation ceased as of Day 351, 22:00, 1990. There are small systematic uncertainties in the velocity components. These are due to such effects as uncertainty in the accuracy of alignment on the spacecraft, relatively wide angular bins, variation in gains between channeltrons, etc. The velocity component data should not be used for studies of large scale, long term, solar wind deflection. The data are generally suitable for all other studies.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/ulysses/plasma/swoops_cdaweb/proton-moments_swoops/1990/uy_proton-moments_swoops_19901118_v01.cdf. The most common cadence, 243000 [ms] = PT4M3S, occurred for 34.3729% of the 3075 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/venus_helio1day_position_19650101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 24105 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/venus_helio1hr_position_19650101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 622367 timesteps. 

Voyager 1 and Voyager 2 Plasma Wave Investigation Information and Web Site Links

SPDF/CDAWeb. Please also acknowledge the data producer: Bill Kurth at University of Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: Bill Kurth at University of Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Bill Kurth at University of Iowa

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/wave_spectra_pws/spectrum_analyzer_cdf/1977/vg1_pws_lr_19770905_v5.30.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 99.5189% of the 8481 timesteps. 

'A Plasma Wave Investigation for the Voyager Mission' F. L. Scarf and D. A. Gurnett, Space Science Reviews, Vol. 21, p. 289, 1977.

SPDF/CDAWeb. Please also acknowledge the data producer: W. Kurth at University Iowa

SPDF/SSCWeb. Please also acknowledge the data producer: W. Kurth at University Iowa

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: W. Kurth at University Iowa

Plasma Wave Science - Waveform Receiver (from all.xml/instrument/description/@short)

Electric Field Waveforms (from Master/CDFglobalAttributes/Data_type)

Calibrated Spacecraft Event Time in UTC of the first capture of the Waveform

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/wave_spectra_pws/waveform_cdf/1978/vg1_pws_wf_1978082105_v1.0.cdf. The most common cadence, 60000000 [ns] = PT0.06S, occurred for 42.7923% of the 377 timesteps. 

Raw Values, Centered/Scaled (RAW*2 - 15) - very high res. time-series

Counts based on variable 'epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/wave_spectra_pws/spectrum_analyzer_cdf/1977/vg2_pws_lr_19770820_v5.30.cdf. The most common cadence, 4000000000 [ns] = PT4S, occurred for 98.4940% of the 4578 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/wave_spectra_pws/waveform_cdf/1979/vg2_pws_wf_1979042807_v1.0.cdf. The most common cadence, 60000000 [ns] = PT0.06S, occurred for 46.6338% of the 284 timesteps. 

Voyager 1 LECP Background-corrected electron differential fluxes

This data set contains data from the LECP instrument on the Voyager 1 spacecraft. Each record in a file contains 1-day (24-hour) scan-averaged fluxes and flux uncertainties of electrons in two contiguous energy channels that cover the energy range 26-70 keV. The period 2002/001 through 2012/240 includes electrons measured upstream of the termination shock and in the heliosheath up though ~2 days after the heliopause crossing. The Voyager 1 LECP instrument steps through eight, 45 deg full-angle sectors, spending 192 sec in each sector, yielding a full scan through 360 deg every 25.6 min. The LECP scan plane is nearly parallel to RT-plane of the heliospheric RTN coordinate system. The electron data are averaged over the seven active sectors S1-S7; S8 is behind the sun-shield and not included in the average.-- Electron channels designated EB01 and EB02-- Data have been corrected to remove background due to penetrating cosmic ray ions -- Fluxes and uncertainties (one st. dev.) in units: electrons/cm^2-s-sr-MeV-- Data are 5-point running averages of daily values-- Values -9.900e+01 used for missing or nonphysical data -- Negative year indicates filled data for the associated doy

Please acknowledge the Voyager LECP Principal Investigator, Dr. Stamatios M. Krimigis of the Applied Physics Laboratory Johns Hopkins University. The LECP instrument was supported under a NASA Contract with the Johns Hopkins Applied Physics Laboratory, with subcontracts to Fundamental Technologies LLC.

1. The Principal Investigators (PIs) shall, in a timely manner, make available to the science data user community (Users) data and access methods to reach the scientifically useful data and provide analysis tools equivalent to the level that the PI uses. 2. The PI shall make available appropriate data products to the public that assist the PI?s EPO responsibilities. 3. The PI shall ensure all scientifically important data and supporting material are archived to ensure long-term accessibility of the data and their correct and independent usability. 4. The PI or the appropriate provider shall inform Users of updates to processing software and calibrations via metadata and other appropriate documentation. 5. Users shall consult with the PI to ensure that the Users are accessing the most recent available versions of the data and analysis routines, and for assistance in the proper interpretation of the data.  HDMC and the Final Archives shall facilitate this, serving as a contact point between PI and users as needed.   6. Browse products are not intended for science analysis or publication and shall not be used for those purposes without consent of the PI. 7. Users shall acknowledge the sources of data used in all publications, presentations, and reports.  In some journals, this can now be done through formal citation of the data product in the reference list.  8. Users are encouraged to provide the PI a copy of each manuscript that uses the PI?s data upon submission of that manuscript for consideration of publication. On publication the citation shall be transmitted to the PI and any other providers of data.  (The community needs to work to find ways to make this easy/automatic.) 9. Users are encouraged to make tools of general utility and/or value-added data products widely available to the community. Users are encouraged to notify the PI of such utilities or products. The User shall also clearly label the product as being different from the original PI-produced data product. 

SPDF/CDAWeb. Please also acknowledge the data producer: Rob Decker at The John Hopkins Applied Physics Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Rob Decker at The John Hopkins Applied Physics Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Rob Decker at The John Hopkins Applied Physics Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/particle/lecp/electron-background-corrected-daily-cdf/voyager-1_lecp_elec-bgnd-cor-1d_20020101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 99.3061% of the 3864 timesteps. 

Background-corrected electron differential fluxes 1day (from all.xml/instrument/description/@short)

Low Energy Charged Particle Detector (from Master/CDFglobalAttributes/Data_type)

Background-corrected electron differential fluxes 1day (from all.xml/instrument/@ID)

This data set contains count rates and uncertainties for the Voyager I spacecraft LECP detector for the year 1991.

SPDF/CDAWeb. Please also acknowledge the data producer: Stamatios M.Krimigis at The John Hopkins Applied Physics Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: Stamatios M.Krimigis at The John Hopkins Applied Physics Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Stamatios M.Krimigis at The John Hopkins Applied Physics Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/particle/lecp/final-cdf/lev-1-rates/voyager-1_lecp_lev-1-rates_19910101_v1.1.1-01.cdf. The most common cadence, 1536000000000 [ns] = PT25M36S, occurred for 62.4342% of the 8064 timesteps. 

FEDU UniDirectional Differential Electron Rates for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channels

FEDU Count rate uncertainties for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channel measurements

FEsDU UniDirectional Differential Scattered-Electron Rates for the EBD1-EBD5 energy channels

FEsDU Count rate uncertainties for the EBD1-EBD5 energy channel measurements

FHDU UniDirectional Differential Hydrogen Rates for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel.s.

FHDU Count rate uncertainties for the PL01, PL02, PL03, PL04, PL05, PL06, PL07, PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements

FHeDU UniDirectional Differential Helium Rates for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channels

FHeDU Count rate uncertainties for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channel measurements

FODU UniDirectional Differential Oxygen Rates for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channels

FODU Count rate uncertainties for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channel measurements

FFeDU UniDirectional Differential Iron Rates for the H36, H8, H9, H43, H21 energy channels

FFeDU Count rate uncertainties for the H36, H8, H9, H43, H21 energy channel measurements

Singles Sectored UniDirectional Differential Rates for the SAR, SE0-SE5, SAL, ALAR energy channels

Singles Sectored Count rate uncertainties for the SAR, SE0-SE5, SAL, ALAR energy channel measurements

Voyager I LECP Ion-Electron daily averaged fluxes and uncertainties.

This data set contains daily averaged fluxes and uncertainties for the Voyager I spacecraft LECP detector for the year 1991.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/particle/lecp/final-cdf/lev-2-daily-avg/voyager-1_lecp_lev-2-daily-avg_19910101_v1.1.1-01.cdf. The most common cadence, 86016000000000 [ns] = PT23H53M36S, occurred for 14.9502% of the 45 timesteps. 

FEDU UniDirectional Differential Electron Fluxes for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channels - by Sector

FEDU Flux uncertainties for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channel measurements - by Sector

FEsDU UniDirectional Differential Scattered-Electron Fluxes for the EBD1, EBD2, EBD3, EBD4, EBD5 energy channels - by Sector

FEsDU Flux uncertainties for the EBD1-EBD5 energy channel measurements - by Sector

FHDU UniDirectional Differential Hydrogen Fluxes for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channels - by Sector

FHDU Flux uncertainties for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements - by Sector

FHeDU UniDirectional Differential Helium Fluxes for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channels - by Sector

FHeDU Flux uncertainties for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channel measurements - by Sector

FODU UniDirectional Differential Oxygen Fluxes for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channels - by Sector

FODU Flux uncertainties for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channel measurements - by Sector

FFeDU UniDirectional Differential Iron Fluxes for the H36, H8, H9, H43, H21 energy channels - by Sector

FFeDU Flux uncertainties for the H36, H8, H9, H43, H21 energy channel measurements - by Sector

Voyager I LECP Ion-Electron hourly averaged fluxes and uncertainties.

This data set contains hourly averaged fluxes and uncertainties for the Voyager I spacecraft LECP detector for the year 1991.

SPDF/CDAWeb. Please also acknowledge the data producer: STAMATIOS M KRIMIGIS at The John Hopkins Applied Physics Laboratory

SPDF/SSCWeb. Please also acknowledge the data producer: STAMATIOS M KRIMIGIS at The John Hopkins Applied Physics Laboratory

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: STAMATIOS M KRIMIGIS at The John Hopkins Applied Physics Laboratory

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/particle/lecp/final-cdf/lev-2-hourly-avg/voyager-1_lecp_lev-2-hourly-avg_19910101_v1.1.1-01.cdf. The most common cadence, 3072000000000 [ns] = PT51M12S, occurred for 41.1118% of the 1982 timesteps. 

FEDU UniDirectional Differential Electron Fluxes for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channels

FEDU Flux uncertainties for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channel measurements

FEsDU UniDirectional Differential Scattered-Electron Fluxes for the EBD1-EBD5 energy channels

FEsDU Flux uncertainties for the EBD1-EBD5 energy channel measurements

FHDU UniDirectional Differential Hydrogen Fluxes for the PL0-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channels

FHDU Flux uncertainties for the PL0-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements

FHeDU UniDirectional Differential Helium Fluxes for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channels

FHeDU Flux uncertainties for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channel measurements

FODU UniDirectional Differential Oxygen Fluxes for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channels

FODU Flux uncertainties for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channel measurements

FFeDU UniDirectional Differential Iron Fluxes for the H36, H8, H9, H43, H21 energy channels

FFeDU Flux uncertainties for the H36, H8, H9, H43, H21 energy channel measurements

Voyager I LECP Ion-Electron scan averaged rates and fluxes with associated uncertainties.

This data set contains scan averaged rates and fluxes with associated uncertainties for the Voyager I spacecraft LECP detector for the year 1991.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/particle/lecp/final-cdf/lev-2-scan-avg/voyager-1_lecp_lev-2-scan-avg_19910101_v1.1.1-01.cdf. The most common cadence, 192000000000 [ns] = PT3M12S, occurred for 95.7114% of the 77510 timesteps. 

FEDU OmniDirectional Scan Averaged Electron Rates for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channels

FEDU OmniDirectional Scan Averaged Electron Fluxes for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channels

FEDU Count Rate Uncertainties for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channel measurements

FEDU Flux Uncertainties for the EB01-EB05, EG06-EG09, E44, E45, E37 energy channel measurements

FEsDU OmniDirectional Scan Averaged Scattered-Electron Rates for the EBD1-EBD5 energy channels

FEsDU OmniDirectional Scan Averaged Scattered-Electron Fluxes for the EBD1-EBD5 energy channels

FEsDU Count Rate Uncertainties for the EBD1-EBD5 energy channel measurements

FEsDU Flux Uncertainties for the EBD1-EBD5 energy channel measurements

FHDU OmniDirectional Scan Averaged Hydrogen Rates for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channels

FHDU OmniDirectional Scan Averaged Hydrogen Fluxes for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channels

FHDU Count Rate Uncertainties for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements.

FHDU Flux Uncertainties for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements

FHeDU OmniDirectional Scan Averaged Helium Rates for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channels

FHeDU OmniDirectional Scan Averaged Helium Fluxes for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channels

FHeDU Count Rate Uncertainties for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channel measurements

FHeDU Flux Uncertainties for the A39, A33, A46, A3, A4, A12, A13, A17, A24, A28, AL01, AL02, L5 energy channel measurements

FODU OmniDirectional Scan Averaged Oxygen Rates for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channels

FODU OmniDirectional Scan Averaged Oxygen Fluxes for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channels

FODU Count Rate Uncertainties for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channel measurements.

FODU Flux Uncertainties for the M34, L14, L18, M38, M35, M47, M6, M7, M15, M19, M20, M25 energy channel measurements

FFeDU OmniDirectional Scan Averaged Iron Rates for the H36, H8, H9, H43, H21 energy channels

FFeDU OmniDirectional Scan Averaged Iron Fluxes for the H36, H8, H9, H43, H21 energy channels

FFeDU Count Rate Uncertainties for the H36, H8, H9, H43, H21 energy channel measurements

FFeDU Flux Uncertainties for the H36, H8, H9, H43, H21 energy channel measurements

voyager 2 LECP Background-corrected electron differential fluxes

This data set contains data from the LECP instrument on the Voyager 2 spacecraft. Each record in a file contains 1-day (24-hour) scan-averaged fluxes and flux uncertainties of electrons in two contiguous energy channels that cover the energy range 22-61 keV. The period 2006/001 through 2018/304 includes electrons measured upstream of the termination shock and in the heliosheath up to heliopause crossing. The voyager 2 LECP instrument steps through eight, 45 deg full-angle sectors, spending 192 sec in each sector, yielding a full scan through 360 deg every 25.6 min. The LECP scan plane is nearly parallel to RT-plane of the heliospheric RTN coordinate system. The electron data are averaged over the seven active sectors S1-S7; S8 is behind the sun-shield and not included in the average.-- Electron channels designated EB01 and EB02-- Data have been corrected to remove background due to penetrating cosmic ray ions -- Fluxes and uncertainties (one st. dev.) in units: electrons/cm^2-s-sr-MeV-- Data are 5-point running averages of daily values-- Values -9.900e+01 used for missing or nonphysical data -- Negative year indicates filled data for the associated doy

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/particle/lecp/electron-background-corrected-daily-cdf/voyager-2_lecp_elec-bgnd-cor-1d_20060101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 98.0580% of the 4595 timesteps. 

Low_Energy_Charged_Particle_Detector (from Master/CDFglobalAttributes/Data_type)

This data set contains count rates and uncertainties for the Voyager II spacecraft LECP detector for the year 1991.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/particle/lecp/final-cdf/lev-1-rates/voyager-2_lecp_lev-1-rates_19910101_v1.1.1-01.cdf. The most common cadence, 1536000000000 [ns] = PT25M36S, occurred for 48.2314% of the 6395 timesteps. 

FEDU Count rate uncertainties for the EB01-EB05, EG01-EG09, E44, E45, E37 energy channel measurements

FHDU UniDirectional Differential Hydrogen Rates for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channels

FHDU Count rate uncertainties for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements

Singles UniDirectional Differential Rates for the SAR, SE0-SE5, SAL, ALAR energy channels

Singles Count rate uncertainties for the SAR, SE0-SE5, SAL, ALAR energy channel measurements

Voyager II LECP Ion-Electron daily averaged fluxes and uncertainties.

This data set contains daily averaged fluxes and uncertainties for the Voyager II spacecraft LECP detector for the year 1991.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/particle/lecp/final-cdf/lev-2-daily-avg/voyager-2_lecp_lev-2-daily-avg_19910101_v1.1.1-01.cdf. The most common cadence, 86015860000000 [ns] = PT23H53M35.86S, occurred for 14.9068% of the 48 timesteps. 

FEsDU Flux uncertainties for the EBD1, EBD2, EBD3, EBD4, EBD5 energy channel measurements

FHDU UniDirectional Differential Hydrogen Fluxes for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channels

FHDU Flux uncertainties for the PL01-PL08, P32, P1, P10, P11, P16, P23, P27, P31 energy channel measurements

Voyager II LECP Ion-Electron hourly averaged fluxes and uncertainties.

This data set contains hourly averaged fluxes and uncertainties for the Voyager II spacecraft LECP detector for the year 1991.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/particle/lecp/final-cdf/lev-2-hourly-avg/voyager-2_lecp_lev-2-hourly-avg_19910101_v1.1.1-01.cdf. The most common cadence, 3072000000000 [ns] = PT51M12S, occurred for 21.2182% of the 1052 timesteps. 

FEDU Flux uncertainties for the EB01, EB02, EB03, EB04, EB05, EG06, EG07, EG08, EG09, E44, E45, E37 energy channel measurements

FEsDU UniDirectional Differential Scattered-Electron Fluxes for the EBD1, EBD2, EBD3, EBD4, EBD5 energy channels

Voyager II LECP Ion-Electron scan averaged rates and fluxes with associated uncertainties.

This data set contains scan averaged rates and fluxes with associated uncertainties for the Voyager II spacecraft LECP detector for the year 1991.

1. The Principal Investigators (PIs) shall, in a timely manner, make available to the science data user community (Users) data and access methods to reach the scientifically useful data and provide analysis tools equivalent to the level that the PI uses. 2. The PI shall make available appropriate data products to the public that assist the PI's EPO responsibilities. 3. The PI shall ensure all scientifically important data and supporting material are archived to ensure long-term accessibility of the data and their correct and independent usability. 4. The PI or the appropriate provider shall inform Users of updates to processing software and calibrations via metadata and other appropriate documentation. 5. Users shall consult with the PI to ensure that the Users are accessing the most recent available versions of the data and analysis routines, and for assistance in the proper interpretation of the data.  HDMC and the Final Archives shall facilitate this, serving as a contact point between PI and users as needed.   6. Browse products are not intended for science analysis or publication and shall not be used for those purposes without consent of the PI. 7. Users shall acknowledge the sources of data used in all publications, presentations, and reports.  In some journals, this can now be done through formal citation of the data product in the reference list.  8. Users are encouraged to provide the PI a copy of each manuscript that uses the PI?s data upon submission of that manuscript for consideration of publication. On publication the citation shall be transmitted to the PI and any other providers of data.  (The community needs to work to find ways to make this easy/automatic.) 9. Users are encouraged to make tools of general utility and/or value-added data products widely available to the community. Users are encouraged to notify the PI of such utilities or products. The User shall also clearly label the product as being different from the original PI-produced data product. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/particle/lecp/final-cdf/lev-2-scan-avg/voyager-2_lecp_lev-2-scan-avg_19910101_v1.1.1-01.cdf. The most common cadence, 192000000000 [ns] = PT3M12S, occurred for 92.9130% of the 76538 timesteps. 

This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength F1 computed from high-resolution magnitudes, the elevation and azimuth angles (degrees) in heliographic (RTN) coordinates, and the magnetic field strength F2 computed from hour averages of the components. The vector components of B can be computed from F2 and the two angles. Elevation angle is the latitude angle above or below the solar equatorial plane, and azimuth angle is in the direction orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication:  Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977...At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al. 1977). ..At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. [1994] and in Appendix A of Burlaga et al. [2002]. ..References: ..Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. ..Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. ..Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. ..Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. ..Ness et al., 1973At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting  about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. [1994] and in Appendix A of Burlaga et al. [2002].COORDINATE SYSTEMS:  Interplanetary magnetic field studies make use of two important coordinate systems, the Inertial Heliographic (IHG) coordinate system and the Heliographic (HG) coordinate system.The IHG coordinate system is use to define the spacecraft's position.  The IHG system is defined with its origin at the Sun.  There are three orthogonal axes, X(IHG), Y(IHG), and Z(IHG).  The Z(IHG) axis points northward along the Sun's  spin axis.  The X(IHG) - Y(IHG) plane lays in the solar equatorial plane.  The intersection of the solar equatorial plane with the ecliptic plane defines a line, the longitude of the ascending node, which is taken to be the X(IHG) axis. The X(IHG) axis drifts slowly with time, approximately one degree per 72 years.Magnetic field orientation is defined in relation to the spacecraft.  Drawing a line from the Sun's center (IHG origin) to the spacecraft defines the X axis of the HG coordinate system.  The HG coordinate system is defined with its origin centered at the spacecraft.  Three orthogonal axes are defined, X(HG), Y(HG), and Z(HG).  The X(HG) axis points radially away from the Sun and the Y(HG) axis is parallel to the solar equatorial plane and therefore parallel to the X(IHG)-Y(IHG) plane too.  The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the IHG and HG systems may be found in Space and Science Reviews, Volume 39 (1984), pages 255-316, MHD Processes in the Outer Heliosphere,  L. F. Burlaga.

Please acknowledge the Principal Investigator, Norman F. Ness of the Bartol Research Institute, University of Delaware in publications and presentations.

SPDF/CDAWeb. Please also acknowledge the data producer: Adam Szabo at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Adam Szabo at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Adam Szabo at NASA GSFC

Triaxial Fluxgate Magnetometer (from all.xml/instrument/description/@short)

9.6 second resolution (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/mag_10s/1977/voyager1_10s_mag_19770905_v01.cdf. The most common cadence, 9600 [ms] = PT9.6S, occurred for 98.8448% of the 20964 timesteps. 

B-Magnitude by Method 1 (F1): 9.6 second average of 1.92 second magnitudes

B-Magnitude by Method 2 (F2): average derived from 9.6 second component averages=sqrt(B1^2+B2^2+B3^2)

BR (B1): 9.6 second average of 1.92 second averages of the B-radial component in HG coords

BT (B2): 9.6 second average of 1.92 second averages of the B-tangential component in HG coords

BN (B3): 9.6 second average of 1.92 second averages of the B-normal component in HG coords

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/mag_10s/1977/voyager1_10s_mag_19770905_v01.cdf. The most common cadence, 48000 [ms] = PT48S, occurred for 94.2231% of the 3996 timesteps. 

Matrix1: transforms 3-element vector from Inertial Heliographic (IHG) to Heliographic (HG)coordinates.

Matrix2: transforms 3-element vector from Earth Mean ecliptic, Equinox of 1950 (EME 50) to Heliographic (HG) coordinates.

Matrix3: transforms 3-element vector from payload coordinates to Heliographic (HG) coordinates.

This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength F1 computed from high-resolution magnitudes, the elevation and azimuth angles (degrees) in heliographic (RTN) coordinates, and the magnetic field strength F2 computed from hour averages of the components. The vector components of B can be computed from F2 and the two angles. Elevation angle is the latitude angle above or below the solar equatorial plane, and azimuth angle is in the direction orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication:  Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977...At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al. 1977). ..At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. [1994] and in Appendix A of Burlaga et al. [2002]. ..References: ..Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. ..Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. ..Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. ..Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. ..Ness et al., 1973At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting  about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. [1994] and in Appendix A of Burlaga et al. [2002].

 Please acknowledge the Principal Investigator, Norman F. Ness of the Bartol Research Institute, University of Delaware, and the NASA National Space Science Data Center (NSSDC) for usage of data from this site in publications and presentations.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/mag_1hr/1990/voyager1_1hr_mag_19900101_v01.cdf. The most common cadence, 3600150 [ms] = PT1H0.15S, occurred for 32.2684% of the 101 timesteps. 

TRIAXIAL FLUXGATE MAGNETOMETER (from all.xml/instrument/description/@short)

Decimal Year (90.00000 is at the start of day 001 for year 1990).

Magnetic field strength from hourly average of high-resolution magnitudes

Magnetic field strength from magnitude of the hourly averaged vector field

Counts based on variable 'Epoch2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/mag_2s/1977/voyager1_2s_mag_19770908_v01.cdf. The most common cadence, 1920 [ms] = PT1.92S, occurred for 99.7706% of the 209193 timesteps. 

1.92 second resolution (from Master/CDFglobalAttributes/Data_type)

This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength F1 computed from high-resolution magnitudes, the elevation and azimuth angles (degrees) in heliographic (RTN) coordinates, and the magnetic field strength F2 computed from hour averages of the components. The vector components of B can be computed from F2 and the two angles. Elevation angle is the latitude angle above or below the solar equatorial plane, and azimuth angle is in the direction orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication:  Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977...At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al. 1977). ..At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. [1994] and in Appendix A of Burlaga et al. [2002]. ..References: ..Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. ..Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. ..Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. ..Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. ..Ness et al., 1973At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting  about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. [1994] and in Appendix A of Burlaga et al. [2002].COORDINATE SYSTEMS:  Interplanetary magnetic field studies make use of two important coordinate systems, the Inertial Heliographic (IHG) coordinate system and the Heliographic (HG) coordinate system.The IHG coordinate system is use to define the spacecraft's position.  The IHG system is defined with its origin at the Sun.  There are three orthogonal axes, X(IHG), Y(IHG), and Z(IHG).  The Z(IHG) axis points northward along the Sun's  spin axis.  The X(IHG) - Y(IHG) plane lays in the solar equatorial plane.  The intersection of the solar equatorial plane with the ecliptic plane defines a line, the longitude of the ascending node, which is taken to be the X(IHG) axis. The X(IHG) axis drifts slowly with time, approximately one degree per 72 years.Magnetic field orientation is defined in relation to the spacecraft.  Drawing a line from the Sun's center (IHG origin) to the spacecraft defines the X axis of the HG coordinate system.  The HG coordinate system is defined with its origin centered at the spacecraft.  Three orthogonal axes are defined, X(HG), Y(HG), and Z(HG).  The X(HG) axis points radially away from the Sun and the Y(HG) axis is parallel to the solar equatorial plane and therefore parallel to the X(IHG)-Y(IHG) plane too.  The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the IHG and HG systems may be found in Space and Science Reviews, Volume 39 (1984), pages 255-316, MHD Processes in the Outer Heliosphere,  L. F. Burlaga.Support data calib_flag_on, calib_flag_MF and calib_flag_offset are added to file version 2. Variable calib_flag_on consists of points where bit 4 or 5 in variable magStatus equal 1. Variable calib_flag_MF represents observations where magnetometer was in cailbration mode. Variable calib_flag_offset represent delay between data points where magnetometer was in calibration mode and data points where magStatus variable indicated calibration periods.Due to specific shape of magnetometer data profile variable calibration_flag_MF may cover larger intervals than calibration_flag_on.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/mag_48s/1977/voyager1_48s_mag_19770905_v02.cdf. The most common cadence, 48000 [ms] = PT48S, occurred for 94.2231% of the 3996 timesteps. 

48 second resolution (from Master/CDFglobalAttributes/Data_type)

B-Magnitude by Method 1 (F1): 48 second average of 9.6 second magnitudes

B-Magnitude by Method 2 (F2): average derived from 48 second component averages=sqrt(B1**2+B2**2+B3**2)

BR (B1): 48 second average of 9.6 second averages of the B-radial component in HG coords

---> BT (B2): 48 second average of 9.6 second averages of the B-tangential component in HG coords

---> BN (B3): 48 second average of 9.6 second averages of the B-normal component in HG coords

---> Matrix2: transforms 3-element vector from Earth Mean ecliptic, Equinox of 1950 (EME 50) to Heliographic (HG) coordinates.

---> Matrix3: transforms 3-element vector from payload coordinates to Heliographic (HG) coordinates.

The  main science objectives for the VOYAGER interplanetary mission are as   follows: - investigate the structure of the solar wind magnetic fields and plasma in the inner and outer heliosphere; - conduct long term study of heliospheric evolution during different phases of the twenty-two year solar magnetic cycle and the eleven-year solar activity cycle;- study the long term solar modulation and determine the elemental and isotopic abundances of galactic cosmic ray particles in the heliosphere;- measure  radial gradients, spectra, and nuclear abundances of the anomalous component of cosmic rays  from  acceleration at the solar wind termination shock; - investigate local particle acceleration in the interplanetary medium from solar flare shocks and corotating interaction regions; - study propagation of solar energetic particles in the heliosphere.The average magnetic field strength produced by the spacecraft at the location of the outboard magnetometer of the dual magnetometers system on V1 and V2 is about 0.1 - 0.2 nT, comparable to the most probable magnetic field strength in the inner heliosheath and significantly larger than the most probable magnetic field strength in the distant supersonic solar wind. The spacecraft magnetic field is a complex, time-dependent signal that must be removed from the measured magnetic field signal in order to derive the ambient magnetic fields of the solar wind and heliosheath. Corrections must also be made for spurious magnetic signals and noise associated with the telemetry system, ground tracking systems, and other factors. Extracting the signal describing the solar wind and heliosheath from the many sources of uncertainty is a complex and partly subjective process that requires understanding of the instrument and judgment based on experience in dealing with the ever-changing extraneous signals. We estimate that for the V1 MAG data the 1-sigma the uncertainty the 48 sec averages for each of the components of the magnetic field  BR, BT, and BN is typically +/- 0.02 nT; the uncertainty in magnitude F1 is typically +/- 0.03 nT. F1, BR, BT, and BN can differ from one another and they may vary with time, but there is no practical way to determine these uncertainties more precisely at present.ReferencesDaniel B. Berdichevsky, Voyager Mission, Detailed processing of weak magnetic fields; I - Constraints to the uncertainties of the calibrated magnetic field signal in the Voyager missions , 2009; https://vgrmag.gsfc.nasa.gov/Berdichevsky-VOY_sensor_opu090518.pdfBehannon, K.W., M.H. Acu..a, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994.Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002.Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., , 76, 3564, 1971.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_ephem.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch_ephem.)

48 second Time Resolution (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/vim_48secmag/voyager1_48s_mag-vim_20090101_v01.cdf. The most common cadence, 47520 [ms] = PT47.52S, occurred for 31.9860% of the 86398 timesteps. 

BR in RTN (Radial-Tangential-Normal) coordinate system (w/ uncertainty)

Counts based on variable 'Epoch_ephem' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/magnetic_fields_cdaweb/vim_48secmag/voyager1_48s_mag-vim_20090101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 364 timesteps. 

Merged hourly magnetic field, plasma, proton fluxes, and ephemeris data

The  main science objectives for the VOYAGER interplanetary mission are as   follows: - investigate the structure of the solar wind magnetic fields and plasma in the inner and outer heliosphere; - conduct long term study of heliospheric evolution during different phases of the twenty-two year solar magnetic cycle and the eleven-year solar activity cycle;- study the long term solar modulation and determine the elemental and isotopic abundances of galactic cosmic ray particles in the heliosphere;- measure  radial gradients, spectra, and nuclear abundances of the anomalous component of cosmic rays  from  acceleration at the solar wind termination shock; - investigate local particle acceleration in the interplanetary medium from solar flare shocks and corotating interaction regions; - study propagation of solar energetic particles in the heliosphere.This directory contains hourly averages of parameters for the interplanetary magnetic field, solar wind plasma and spacecraft trajectory coordinatesVOYAGER-1 data have been reprocessed to ensure a uniformity of content and coordinate systems relative to data from other deep-space missions: - All spacecraft trajectory data were transformed to a Heliographic Inertial (HGI) coordinate system.- calculation of the RTN Cartesian components of interplanetary magnetic field from the RTN spherical components:          BR=|B|*cos(THETA)*cos(PHI)          BT=|B|*cos(THETA)*sin(PHI)          BN=|B|*sin(THETA)          where THETA - spherical RTN latitude, PHI- spherical RTN longtitude - calculation of RTN Spherical components of the solar wind velocity from RTN cartesian components:         V = (Vr^2 + Vt^2 + Vn^2)^0.5         THETA=asin(Vn/V)         PHI=atan(Vt/Vr)where THETA - spherical RTN latitude, PHI- spherical RTN longtitude- calculation of given thermal speed Vth into temperature T (Kelvin):         T=60.5*Vth^2 (Vth in km/s)- merging of trajectory coordinates, magnetic field data, and plasma data files into a single annual file VY1_YR.DAT, where YR is the year- Data gaps were filled with dummy numbers for the missing hours or entire days to make all files of equal length.  The character \'9\' is used to fill all fields for missing data according to their format, e.g. \' 9999.9\' for a field with the FORTRAN format F7.1. Note that format F7.1 below really means (1X,F6.1),etc.aNotes on Voyager 1 and 2 Magnetometer Data After 1989.  At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field.  The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971; Behannon et al. 1977).  At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is ..0.15 nT and ..0.05 nT, respectively. The use of roll calibrations lasting ..6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radius vector to the Sun) at intervals of ..3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 nT - 0.05 nT. further informaion look at https://omniweb.gsfc.nasa.gov/coho/html/cw_data.htmlThe Heliographic Inertial (HGI) coordinates are Sun-centered and inertially fixed with respect to an X-axis directed along the intersection line of the ecliptic and solar equatorial planes.  The solar equator plane is inclined at 7.25 degrees from the ecliptic.  This direction was towards ecliptic longitude of 74.36 degrees on 1 January 1900 at 1200 UT; because of precession of the celestial equator, this longitude increases by 1.4 degrees/century. The Z axis is directed perpendicular and northward from the solar equator, and the  Y-axis completes the right-handed set. This system differs from the usual  heliographic  coordinates  (e.g. Carrington longitudes) which are fixed in the frame of the rotating Sun. The RTN system is fixed at a spacecraft (or the planet). The R axis is  directed radially away from the Sun, the T axis is the cross product of the solar rotation axis and the R axis, and the N axis is the cross product of R and T.  At zero Heliographic Latitude when the spacecraft is in the solar equatorial plane the N and solar rotation axes are parallel.Hour averages of the interplanetary solar wind data from, and hourly heliocentric coordinates of, Voyager1/2 and other interplanetary spacecraft may be also be accessed and plotted on-line through the COHOWeb service  http://cohoweb.gsfc.nasa.gov/Acknowledgement: Use of these data in publications should be accompanied at minimum by acknowledgements of the National Space Science Data Center and the responsible Principal Investigator defined in the experiment documentation provided here.  Citation of NSSDC's Coordinated Heliospheric Observations (COHO) data base would also be appreciated, so that other potential users will be made aware of this service. For questions about this data set, please contact: Dr. N. Papitashvili, natalia.e.papitashvili@nasa.gov, GSFC-Code 672 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/coho1hr_magplasma/1977/voyager1_coho1hr_merged_mag_plasma_19770101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Merged Trajectory, Magnetic Field, Plasma, and Fluxes (from all.xml/instrument/description/@short)

Proton Temperature (calculated from thermal speed width T=60.5*Vth*Vth)

General information concerning the Voyager 1 Cosmic Ray System, CRS, instrument

Voyager Cosmic Ray System, CRS, instrument web site, with information concerning two High Energy Telescopes, HET-I and HET-II, four Low Energy Telscopes, LET A-D, and The Electron Telescope, TET, hosted by GSFC, NASA

Voyager Cosmic Ray System, CRS, instrument description and scientific objectives web site, hosted by JPL, NASA

Voyager Cosmic Ray System, CRS, instrument description, Space Science Reviews publication

Stone, E.C., R.E. Vogt, F.B. McDonald, B.J. Teegarden, J.H. Trainor, J.R. Jokipii, and W.R. Webber, Cosmic Ray Investigation for the Voyager Missions: Energetic Particle Studies in the Outer Heliosphere - and Beyond, Space Sci. Rev. 21, 355-376w, 1977.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/particle/crs/cdfs/one_day/voyager1_crs_daily_flux_19770908_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for 92.6471% of the 63 timesteps. 

Cosmic Ray Subsystem (from all.xml/instrument/description/@short)

These data are from a re-analysis of the Voyager Plasma Spectrometer (PLS) data at Jupiter by the PLS group at the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado. Density, temperature, and flow velocity fits for total and individual ions were done using the Voyager Ion PLS Experiment Response (VIPER) code and error analysis as described at http://lasp.colorado.edu/home.mop/missions/voyager/viper/. Fits are determined from processing of the ion currents from the A, B, C, and D cups of the instrument.. As per the Fit Case variable, one of five different constraints were used in the VIPER fits for each 96-sec time interval: (1) free variation of all parameters (mainly for the cold ion torus); (2) constraint of the ion abundances for the five major species (O+, O++, S+, S++, S+++) to standard composition as determined from Delamere et al. (2005); (3) fixed ion composition and flow speed; (4) cold blobs in the plasma sheet where resolved peaks can be fit with allowance for some variance in composition; (5) interpolation between composition of cold torus and standard abundances at 6 RJ from Delamere et al. (2005). Reference: Delamere, P. A., Bagenal, F., and Steffl, A. (2005), Radial Variations in the Io Plasma Torus During the Cassini Era, Journal of Geophysical Research Space Physics, 110(A12), A12223, doi: 10.1029/2005JA011251. 

Please acknowledge the Voyager 1 PLS PI, Dr. John D. Richardson of the MIT, and the data set producer, Dr. Fran Bagenal of the University of Colorado.

Fits to Spectra Source Data at the Laboratory of Atmospheric and Space Physics, LASP, University of Colorado, Boulder

Documentation for the Voyager PLS Instrument, hosted at the Massachusetts Institute of Technology, MIT

The VIPER, Voyager Ion PLS Experiment Response, Web Page at the Laboratory of Atmospheric and Space Physics, LASP, University of Colorado, Boulder

The VIPER, Voyager Ion PLS Experiment Response, Instruction Manual available from the Laboratory of Atmospheric and Space Physics, LASP, University of Colorado, Boulder

For public distribution but users are advised to contact Dr. Bagenal on questions about how the data were produced. 

SPDF/CDAWeb. Please also acknowledge the data producer: Dr. John D. Richardson at MIT Kavli Institute

SPDF/SSCWeb. Please also acknowledge the data producer: Dr. John D. Richardson at MIT Kavli Institute

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Dr. John D. Richardson at MIT Kavli Institute

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/plasma_cdaweb/composition/1979/voyager1_pls_composition_19790303_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 55.0781% of the 423 timesteps. 

Plasma Composition Data near Jupiter (from all.xml/instrument/description/@short)

Fit Case Number 1-5 for how the fit parameters were handled by the VIPER code. 

East longitude (Phi) velocity (km/s) of the bulk plasma flow in RHSIII coordinate system.

Northward component of bulk flow velocity (km/s) in RHSIII coordinate system.

1: These electron current spectra in the jovian magnetosphere are from the Plasma Spectrometer (PLS) instrument on Voyager 1 during March 1979 flyby of Jupiter. The instrument has four Faraday Cups A - D, the electron data come only from D. The data are specified in terms of current per cup in femto-amps (10^-15 A) versus channel number and energy (eV). 2: This data set is for the PLS E1 mode covering electron energies of 10 - 140 eV in 16 energy channels. PLS samples only one mode of electron (E1, E2) or ion (L, M) spectra in each time intervals, so the E1 data are not continuous but consecutive with the other modes in time. 3: Reference: Bridge et al. (1977). The Plasma Experiment on the the 1977 Voyager Mission, Space Science Reviews, 21, 259-287. 

Please acknowledge the Voyager 1 PLS PI, Dr. John D. Richardson of the Massacusetts Institute of Technology. 

Voyager Plasma Science, PLS, Experiment Web Page at the Massachusetts Institute of Technology

For public distribution but users are advised to contact Dr. Richardson on questions about how the data were produced. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/plasma_cdaweb/electrons/e1/voyager1_pls_electrons_e1_19790228_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 85.8325% of the 14934 timesteps. 

Electron current from D cup versus electron energy at 10 - 140 eV . 

These electron current spectra in the jovian magnetosphere are from the Plasma Spectrometer (PLS) instrument on Voyager 1 during the March 1979 flyby of Jupiter. The instrument has four Faraday Cups A - D, the electron data come only from D. The data are specified in terms of current per cup in femto-amps (10^-15 A) versus channel number and energy (eV). This data set is for the PLS E1 mode covering electron energies of 10 - 140 eV in 16 energy channels. PLS samples only one mode of electron (E1, E2) or ion (L, M) spectra in each time intervals, so the E1 data are not continuous but consecutive with the other modes in time. Reference: Bridge et al. (1977). The Plasma Experiment on the the 1977 Voyager Mission, Space Science Reviews, 21, 259-287. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/plasma_cdaweb/electrons/e2/voyager1_pls_electrons_e2_19790228_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 85.7619% of the 14926 timesteps. 

Electron current from D cup versus electron energy at 10 - 5950 eV  . 

The files in this directory contain the Voyager fine resolution plasma data. The plasma parameters are obtained by finding the best fit of a convected isotropic Maxwellian distribution to the data. One sigma errors are typically less than 0.5% in the speed and VR, less than 5% for the density and thermal speed, and vary greatly for VT and VN. Sampling times range from 12 to 192 sec., with sampling generally more frequent early in the mission.The velocity components are given in the RTN coordinate system, where R is radially outward, T is in a plane parallel to the solar equatorial plane and positive in the direction of solar rotation, and N completes a right-handed system.(WARNING: V_t, and V_n parameters are often NOT reliable after 1989)Please consult with us, or at least send preprints, when you use this data to prevent grievous errors or misconceptions. (John Richardson, jdr@space.mit.edu)

SPDF/CDAWeb. Please also acknowledge the data producer: John D. Richardson at Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology.

SPDF/SSCWeb. Please also acknowledge the data producer: John D. Richardson at Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: John D. Richardson at Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/plasma_cdaweb/hires_plasma/1977/voyager1_pls_hires_plasma_data_19770907_v01.cdf. The most common cadence, 12000 [ms] = PT12S, occurred for 90.0285% of the 266478 timesteps. 

Voyager high resolution plasma data. (from all.xml/instrument/description/@short)

Voyager HiRes Plasma (from Master/CDFglobalAttributes/Data_type)

These ion current spectra in the jovian magnetosphere are from the Plasma Spectrometer (PLS) instrument on Voyager 1 during the March 1979 flyby of Jupiter. The instrument has four Faraday Cups A - D, the electron data come only from D. The data are specified in terms of current per cup in femto-amps (10^-15 A) versus channel number and energy (eV). This data set is for the PLS L-mode covering H+ ion energies of 10 - 5950 eV at low energy resolution in 16 logarithmic energy channels. PLS samples only one mode of electron (E1, E2) or ion (L, M) spectra in each time interval, so the L-mode data are not continuous but consecutive with the other modes in time. Reference: Bridge et al. (1977). The Plasma Experiment on the the 1977 Voyager Mission, Space Science Reviews, 21, 259-287. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/plasma_cdaweb/ions/l/voyager1_pls_ions_l_19790228_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 86.9555% of the 15172 timesteps. 

These ion current spectra in the jovian magnetosphere are from the Plasma Spectrometer (PLS) instrument on Voyager 1 during the March 1979 flyby of Jupiter. The instrument has four Faraday Cups A - D, the electron data come only from D. The data are specified in terms of current per cup in femto-amps (10^-15 A) versus channel number and energy (eV). This data set is for the PLS M-mode covering H+ ion energies of 10 - 5950 eV at high energy resolution in 128 logarithmic energy channels. PLS samples only one mode of electron (E1, E2) or ion (L, M) spectra in each time interval, so the M-mode data are not continuous but consecutive with the other modes in time.Reference: Bridge et al. (1977). The Plasma Experiment on the the 1977 Voyager Mission, Space Science Reviews, 21, 259-287. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager1/plasma_cdaweb/ions/m/voyager1_pls_ions_m_19790228_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 86.5946% of the 15148 timesteps. 

Counts based on variable 'Epoch2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/mag_10s/1977/voyager2_10s_mag_19770820_v01.cdf. The most common cadence, 9600 [ms] = PT9.6S, occurred for 99.3371% of the 385740 timesteps. 

---> B-Magnitude by Method 2 (F2): average derived from 9.6 second component averages=sqrt(B1**2+B2**2+B3**2)

---> BR (B1): 9.6 second average of 1.92 second averages of the B-radial component in HG coords

---> BT (B2): 9.6 second average of 1.92 second averages of the B-tangential component in HG coords

---> BN (B3): 9.6 second average of 1.92 second averages of the B-normal component in HG coords

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/mag_10s/1977/voyager2_10s_mag_19770820_v01.cdf. The most common cadence, 48000 [ms] = PT48S, occurred for 96.6856% of the 75088 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/mag_1hr/1990/voyager2_1hr_mag_19900101_v01.cdf. The most common cadence, 3600150 [ms] = PT1H0.15S, occurred for 33.6088% of the 122 timesteps. 

Counts based on variable 'Epoch2' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/mag_2s/1977/voyager2_2s_mag_19770824_v01.cdf. The most common cadence, 1920 [ms] = PT1.92S, occurred for 99.7297% of the 129149 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/mag_48s/1977/voyager2_48s_mag_19770820_v02.cdf. The most common cadence, 48000 [ms] = PT48S, occurred for 91.8867% of the 4802 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/vim_48secmag/voyager2_48s_mag-vim_20090131_v02.cdf. The most common cadence, 47520 [ms] = PT47.52S, occurred for 22.1402% of the 39493 timesteps. 

Counts based on variable 'Epoch_ephem' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/magnetic_fields_cdaweb/vim_48secmag/voyager2_48s_mag-vim_20090131_v02.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 364 timesteps. 

Voyager-2 merged hourly magnetic field, plasma, proton fluxes, and ephemeris data

 Please acknowledge the Principal Investigator, Norman F. Ness of the Bartol Research Institute, University of Delaware, John Richardson of MIT and the NASA National Space Science Data Center (NSSDC) for usage of data from this site in publications and presentations.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/coho1hr_magplasma/1977/voyager2_coho1hr_merged_mag_plasma_19770101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 743 timesteps. 

Merged Trajectory, Magnetic Field, Plasma, and Flluxes (from all.xml/instrument/description/@short)

Please acknowledge the Voyager 2 PLS Principal Investigator, Dr. John D. Richardson of the MIT, and the data set producer, Dr. Fran Bagenal of the University of Colorado.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/composition/1979/voyager2_pls_composition_19790707_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 40.1961% of the 41 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/electrons/e1/voyager2_pls_electrons_e1_19790702_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 91.9735% of the 24854 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/electrons/e2/voyager2_pls_electrons_e2_19790702_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 91.9076% of the 24793 timesteps. 

Electron current from D cup versus electron energy at 10 - 5950 eV . 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/hires_plasma/1977/voyager2_pls_hires_plasma_data_19770821_v01.cdf. The most common cadence, 12000 [ms] = PT12S, occurred for 91.5038% of the 274151 timesteps. 

Voyager high resulution plasma data. (from all.xml/instrument/description/@short)

SPDF/CDAWeb. Please also acknowledge the data producer: John D. Richardson at Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology

SPDF/SSCWeb. Please also acknowledge the data producer: John D. Richardson at Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: John D. Richardson at Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/hires_plasma/heliosheath/voyager2_pls_hires_plasma_data_hsh_20070827_v01.cdf. The most common cadence, 192000 [ms] = PT3M12S, occurred for 43.8430% of the 1385 timesteps. 

Voyager high resolution plasma data in heliosheath (from all.xml/instrument/description/@short)

These ion current spectra in the jovian magnetosphere are from the Plasma Spectrometer (PLS) instrument on Voyager 2 during the July 1979 flyby of Jupiter. The instrument has four Faraday Cups A - D, the electron data come only from D. The data are specified in terms of current per cup in femto-amps (10^-15 A) versus channel number and energy (eV). This data set is for the PLS L-mode covering H+ ion energies of 10 - 5950 eV at low energy resolution in 16 logarithmic energy channels. PLS samples only one mode of electron (E1, E2) or ion (L, M) spectra in each time interval, so the L-mode data are not continuous but consecutive with the other modes in time. Reference: Bridge et al. (1977). The Plasma Experiment on the the 1977 Voyager Mission, Space Science Reviews, 21, 259-287. 

Please acknowledge the Voyager 2 PLS PI, Dr. John D. Richardson of the Massacusetts Institute of Technology. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/ions/l/voyager2_pls_ions_l_19790716_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 86.9555% of the 15172 timesteps. 

These ion current spectra in the jovian magnetosphere are from the Plasma Spectrometer (PLS) instrument on Voyager 2 during the July 1979 flyby of Jupiter. The instrument has four Faraday Cups A - D, the electron data come only from D. The data are specified in terms of current per cup in femto-amps (10^-15 A) versus channel number and energy (eV). This data set is for the PLS M-mode covering H+ ion energies of 10 - 5950 eV at high energy resolution in 128 logarithmic energy channels. PLS samples only one mode of electron (E1, E2) or ion (L, M) spectra in each time interval, so the M-mode data are not continuous but consecutive with the other modes in time.Reference: Bridge et al. (1977). The Plasma Experiment on the the 1977 Voyager Mission, Space Science Reviews, 21, 259-287. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/voyager/voyager2/plasma_cdaweb/ions/m/voyager2_pls_ions_m_19790716_v01.cdf. The most common cadence, 96000 [ms] = PT1M36S, occurred for 80.8195% of the 21717 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1day/wild2_helio1day_position_19950101_v01.cdf. The most common cadence, 86400000 [ms] = P1D, occurred for all 9496 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/planet_and_comet_positions/helio1hr/wild2_helio1hr_position_19960101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 306815 timesteps. 

These electron core halo and strahl parameters are moments of Wind 3DP EESA-L and EESA-H measurements, corrected for spacecraft potential and other instrumental effects.  More information can be found at:C. S. Salem et al., Precision Electron Measurements in the Solar Wind at 1AU from NASA’s Wind spacecraft, Astron. & Astrophys., 2023.M. Pulupa et al., Spin-modulated spacecraft floating potential: Observations and effects on electron moments, J. Geophys. Res. Space Physics, Vol. 119, 647-657, doi:10.1002/2013JA019359, 2014.R. P. Lin et al., A Three-dimensional plasma and energetic particle investigation for the Wind spacecraft, Space Science Reviews, Vol. 71, p125-153, 1995.

Salem, C. S., et al., Precision Electron Measurements in the Solar Wind at 1AU from NASA’s Wind spacecraft, Astron. & Astrophys. Note paper has been accepted in 2023

Pulupa, M., et al., Spin-modulated spacecraft floating potential: Observations and effects on electron moments, J. Geophys. Res. Space Physics, Vol. 119, 647-657, doi:10.1002/2013JA019359

Lin, R. P. et al., A Three-dimensional plasma and energetic particle investigation for the Wind spacecraft, Space Science Reviews, Vol. 71, p125-153, 1995.

SPDF/CDAWeb. Please also acknowledge the data producer: Chadi S. Salem at University of California, Berkeley

SPDF/SSCWeb. Please also acknowledge the data producer: Chadi S. Salem at University of California, Berkeley

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Chadi S. Salem at University of California, Berkeley

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/3dp/3dp_echsfits_e0-yr/1995/wind_3dp_echsfits_e0-yr_19950101_v01.cdf. The most common cadence, 96567 [ms] = PT1M36.567S, occurred for 4.6490% of the 3301 timesteps. 

Wind Interplanetary Plasma Laboratory (from all.xml/observatory/description/@short)

Three Dimensional Plasma Instrument Suite (from all.xml/instrument/description/@short)

Wind Interplanetary Plasma Laboratory (from Master/CDFglobalAttributes/Source_name)

Solar Wind Plasma Corrected Electron Core Halo and Strahl MomentsYearly Dataset (from Master/CDFglobalAttributes/Data_type)

Electron velocity vector moment in GSE coordinates in units of km/s

Parallel electron core drift velocity in the ion frame in units of km/s

Parallel electron halo drift velocity in the ion frame in units of km/s

Parallel electron strahl drift velocity in the ion frame in units of km/s

Q, Quality parameter for electron data. It is calculated from the properties of the input data and goodness-of-fit statistics from the nonlinear fitting process.  It varies between 0 and 10. Higher values of Q represent more confidence in the resulting electron parameters

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/helio1hr/wind_helio1hr_position_19941102_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 268775 timesteps. 

WIND Radio/Plasma Wave, (WAVES) Quasi-Thermal Noise Key Parameters

SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263, 1995.JGRA: Solar Wind Electron Parameters Determination on Wind Spacecraft Using Quasi Thermal Noise Spectroscopy, Vol 125, JA028113Variable note:  suprathermal parameters (fit_a, delta_a, coarse_a, fit_t, delta_t, coarse_t), have large uncertainties due to instruemntal limitations. Commonly, for science purposes, medians on a scale of 1-5 minutes should be used. 

SPDF/CDAWeb. Please also acknowledge the data producer: Keith Goetz at University of Minnesota

SPDF/SSCWeb. Please also acknowledge the data producer: Keith Goetz at University of Minnesota

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Keith Goetz at University of Minnesota

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/solar-wind_electron_quasi-thermal_noise_spectroscopy_qtnfit/2008/wind_waves_qtnfit_20080101_v01.cdf. The most common cadence, 4416000000 [ns] = PT4.416S, occurred for 87.7139% of the 15171 timesteps.

WIND Interplanetary Plasma Laboratory (from all.xml/observatory/description/@short)

WIND Interplanetary Plasma Laboratory (from Master/CDFglobalAttributes/Source_name)

Quasi-Thermal Noise Key Parameters (from Master/CDFglobalAttributes/Data_type)

Electron number density uncertainty from fits of selected QTN data

Electron core temperature uncertainty from fits of selected QTN data

Halo to core electron density ratio from fits of selected QTN data

Halo to core electron density ratio uncertainty from fits of selected QTN data

Halo to core electron temperature ratio from fits of selected QTN data

Halo to core electron temperature ratio uncertainty from fits of selected QTN data

Quality Flag of QTN fits of selected QTN data; from number of selected QTN channels

Quality Flag of QTN fits of selected QTN data; from fitting the plasma peak

Quality Flag of QTN fits of selected QTN data; from shifts between fit and data

Quality Flag of QTN fits of selected QTN data; from data levels lower then the fit

WIND Radio/Plasma Wave, (WAVES) Filtered Quasi-Thermal Noise Key Parameters

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/solar-wind_electron_quasi-thermal_noise_spectroscopy_qtnfit-filtered/2008/wind_waves_qtnfit-filtered_20080101_v01.cdf. The most common cadence, 4416000000 [ns] = PT4.416S, occurred for 80.2341% of the 3702 timesteps.

Homepage for the Wind mission. Contains links to data and instrument descriptions.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/orbit/def_at/1997/wi_at_def_19970701_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

WIND INTERPLANETARY PLASMA LABORATORY (from all.xml/observatory/description/@short)

WIND INTERPLANETARY PLASMA LABORATORY (from Master/CDFglobalAttributes/Source_name)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/orbit/pre_at/2025/wi_at_pre_20250607_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

Electron energy-angle distributions 100 eV - 30 keV, often at 24 sec, EESA High, Wind 3DP

Wind 3dp, EESA High electron pitch angle distributionsNote per Lynn Wilson Jan 2015 wrt time resolution: 24 sec timing changes and is not necessarily constant, depending on the mode that the instrument happens to be in.  Not only does the period/interval between each point change, the duration over which the data were taken can change as well.

SPDF/CDAWeb. Please also acknowledge the data producer: R. Lin/S. Bale at UC Berkeley

SPDF/SSCWeb. Please also acknowledge the data producer: R. Lin/S. Bale at UC Berkeley

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Lin/S. Bale at UC Berkeley

3-D PLASMA ANALYZER (from all.xml/instrument/description/@short)

EESA High Pitch Distributions and Moments (from Master/CDFglobalAttributes/Data_type)

Electron number flux 100eV-30keV in 15 energy and 8 angle bins (as energy-pitch angle displays)

Electron number flux 100eV-30keV as a stack_plot of 15 energies at the Bin1 angle (often ~15 deg

Electron number flux 100eV-30keV as a stack_plot of 8 pitch angles at the Ch1 energy (often ~28000 eV)

Electron omnidirectional fluxes 100 eV-30 keV, often at 24 sec, EESA High, Wind 3DP

Wind 3dp, EESA HIGH electron omni directional energy spectraNote per Lynn Wilson Jan 2015 wrt time resolution: 24 sec timing changes and is not necessarily constant, depending on the mode that the instrument happens to be in.  Not only does the period/interval between each point change, the duration over which the data were taken can change as well.

EESA High Electron Omnidirectional Fluxes (from Master/CDFglobalAttributes/Data_type)

Electron differential number flux 100 eV - 30 keV, as a function of energy [spectrogram] 

Wind 3dp, ELM2Lynn Wilson Note Feb2015 Correct spacecraft potential is important to scientifically useful results .No documentation found on how this potential has been calculated.

EESA Low Electron Moments (from Master/CDFglobalAttributes/Data_type)

[SC_POT] Spacecraft potential estimated from electron ONLY measurements

---> [SC_CURRENT?] Current contribution to the spacecraft from thermal electrons

---> [MAGF] magnetic field vector interpolated (linearly) to the time of the EESA Low distribution, in GSE cartesian components

[PTENS] electron Pressure Tensor calculated in the GSE coordinate basis.  The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ

---> [MFTENS] electron Momentum Flux Tensor calculated in the GSE coordinate basis.  The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ

---> [T3] electron Temperature eigenvalues after diagonalization of tensor, calculated in the GSE coordinate basis.  The elements correspond to:  XX, YY, ZZ

[SYMM] ZZ-component of the eigenvectors associated with the eigen values from the diagonalized .T3 (i.e., the eigenvector associated with the Z eigen value from .T3 or .T3[2])

---> [SYMM_ANG] angle between the ZZ-component of the eigenvectors associated with the eigen values from the diagonalized .T3 and the magnetic field vector (i.e., .MAGF vector)

---> [MAGT3] electron temperature tensor... rotated into a field-aligned coordinate basis and then taking the diagonal elements only

Electron energy-angle distributions 5-1100 eV, often at 24 sec, EESA Low, Wind 3DP

Wind 3dp, EESA Low electron pitch angle distributions with ion-derived moments

EESA Low Pitch Distributions and Moments (from Master/CDFglobalAttributes/Data_type)

Electron number flux 5-1100 eV in 15 energy and 8 angle bins (as energy-pitch angle displays)

Electron number flux 5-1100 eV as a stack_plot of 15 energies at the Bin1 angle (often ~15 deg

Electron number flux 5-1100 eV as a stack_plot of 8 pitch angles at the Ch1 energy (often ~1150 eV)

Electron omnidirectional fluxes 5-1100 eV, often at 24 sec, EESA Low, Wind 3DP

Wind Spacecraft general instrument web page with links to data, documentation, and home pages for all spacecraft instruments, hosted by NASA GSFC

Wind spacecraft General web page for data sources from all instruments, GSFC

Wind spacecraft general instrument web page with brief descriptions for data sources from all instruments, hosted by NASA GSFC

General information concerning the Wind, Hot Plasma and Charged Particles, 3DP, instrument

Wind Three-Dimensional Plasma and Energetic Particle Investigation, 3DP, instrument, Space Science Reviews publication

Lin, R.P., K.A. Anderson, S. Ashford, C. Carlson, D. Curtis, R. Ergun, D. Larson, J. McFadden, M. McCarthy, G.K. Parks, H. Rème, J.M. Bosqued, J. Coutelier, F. Cotin, C. D'Uston, K.-P. Wenzel, T.R. Sanderson, J. Henrion, J.C. Ronnet, and G. Paschmann, A three-dimensional plasma and energetic particle investigation for the wind spacecraft, Space Sci. Rev., 71, 125-153, 1995, DOI: 10.1007/BF00751328.

EESA Low Electron OMNI Spectra (from Master/CDFglobalAttributes/Data_type)

Electron differential number flux as function of time-varying energy  in range 5-1100 eV [as spectrogram]

Time-varying electron energies in 15 channels (center of 40% wide energy band)

These electron parameters are moments of Wind 3DP EESA-L and EESA-H measurements, corrected for spacecraft potential and other instrumental effects.  More information can be found at:R. P. Lin et al., A Three-dimensional plasma and energetic particle investigation for the Wind spacecraft, Space Science Reviews, Vol. 71, p125-153, 1995.C. S. Salem et al., Precision Electron Measurements in the Solar Wind at 1AU from NASA’s Wind spacecraft, J. Geophys. Res. Space Physics, 2017.M. Pulupa et al., Spin-modulated spacecraft floating potential: Observations and effects on electron moments, J. Geophys. Res. Space Physics, Vol. 119, 647-657, doi:10.1002/2013JA019359, 2014.

SPDF/CDAWeb. Please also acknowledge the data producer: Stuart D. Bale at University of California, Berkeley

SPDF/SSCWeb. Please also acknowledge the data producer: Stuart D. Bale at University of California, Berkeley

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Stuart D. Bale at University of California, Berkeley

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/3dp/3dp_emfits_e0/1995/wi_emfits_e0_3dp_19950101_v01.cdf. The most common cadence, 102356 [ms] = PT1M42.356S, occurred for 18.4906% of the 98 timesteps. 

Solar Wind Plasma Corrected Electron Moments (from Master/CDFglobalAttributes/Data_type)

Electron Plasma moments (computed on-board) (NOT CORRECTED FOR S/C POTENTIAL) @ 3 second (spin) resolution (version 3), EESA LOW, Wind 3DP

Wind 3dp, EESA LOW 1 spin resolution Plasma ( electron ) moments (computed on spacecraft)

EESA (On-Board) Electron Plasma Moments @ Spin Resolution (version 3), Wind 3DP (from Master/CDFglobalAttributes/Data_type)

---> Residual Variance in Electron Velocity (6 components in instrument coords)

The EPACT Instrument on Wind   STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field 

Wind Project Web Site - Comprehensive Solar Wind Laboratory for Long-Term Solar Wind Observations

Wind> Energetic Particle Acceleration Composition, and Transport

SPDF/CDAWeb. Please also acknowledge the data producer: Mihir Desai at University of Texas, San Antonio

SPDF/SSCWeb. Please also acknowledge the data producer: Mihir Desai at University of Texas, San Antonio

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Mihir Desai at University of Texas, San Antonio

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/step/differential-ion-flux-1hr/wi_epact_step-differential-ion-flux-1hr_19941121_v01.cdf. The most common cadence, 3612305 [ms] = PT1H12.305S, occurred for 16.2743% of the 159 timesteps. 

differential ion fluxes 1hrin (from all.xml/instrument/description/@short)

The EPACT Instrument on Wind   STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field of view with an angular acceptance of 44 deg in azimuth and 17 deg in polar angle. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/step/directional-diff-cno-flux-10min/wi_epact_step-directional-diff-cno-flux-10min_19941121_v01.cdf. The most common cadence, 645996 [ms] = PT10M45.996S, occurred for 22.6986% of the 1186 timesteps. 

directional differential cno fluxes 10min (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/step/directional-diff-fe-flux-10min/wi_epact_step-directional-diff-fe-flux-10min_19941121_v01.cdf. The most common cadence, 645996 [ms] = PT10M45.996S, occurred for 22.6986% of the 1186 timesteps. 

directional differential fe fluxes 10min (from all.xml/instrument/description/@short)

The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field of view with an angular acceptance of 44 deg in azimuth and 17 deg in polar angle. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/step/directional-diff-h-flux-10min/wi_epact_step-directional-diff-h-flux-10min_19941121_v01.cdf. The most common cadence, 645996 [ms] = PT10M45.996S, occurred for 22.6986% of the 1186 timesteps. 

directional differential h fluxes 10min (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/step/directional-diff-he-flux-10min/wi_epact_step-directional-diff-he-flux-10min_19941121_v01.cdf. The most common cadence, 645996 [ms] = PT10M45.996S, occurred for 22.6986% of the 1186 timesteps. 

directional differential he fluxes 10min (from all.xml/instrument/description/@short)

Wind Magnetic Fields Investigation: 3 sec, 1 min, and hourly Definitive Data.

WIND MFI Composite data file.  This file contains multiple time resolution data.1 Minute data averages                                                          3 Second data averages                                                          1 Hour   data averages                                                          WIND MFI Instrument turn on 11/12/1994                                          Data versions:                                                                  03 - Extrapolated Bz correction                                                 04 - Final Bz correction                                                        05 - Final orbit and Bz correction                                              References:                                                                     1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in     The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995                  2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.     3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   The International Solar-Terrestrial Physics (ISTP) Program Information          Processing Division Ground Data Processing System and The ISTP Mission          Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         Magnetometer Experiment, September 1987.                                        5. National Space Science Data Center, CDF User's Guide, Version 2.3.0,        October 1, 1992.                                                                6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter    Generation Software (KPGS) Standards & Conventions, September 1992.             7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972         

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch3, @2 => Epoch1.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 3 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch3, @2 => Epoch1.)

Magnetic Fields Investigation (from all.xml/instrument/description/@short)

3 sec, 1 min, and hourly Definitive Data (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h0/1994/wi_h0_mfi_19941113_v05.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Distance from the center of the earth (Define Re = 6378km) (1 min)

Counts based on variable 'Epoch3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h0/1994/wi_h0_mfi_19941113_v05.cdf. The most common cadence, 3000 [ms] = PT3S, occurred for all 28799 timesteps. 

Counts based on variable 'Epoch1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h0/1994/wi_h0_mfi_19941113_v05.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

Distance from the center of the earth (Define Re = 6378km) (1 hour)

Position vector in GSM coordinates (Define Re = 6378km) (1 hour)

Position vector in GSE coordinates (Define Re = 6378km) (1 hour)

Wind SWE (Solar Wind Experiment), 6 - 12 sec Solar Wind Electron Moments

Explanatory notes:The electron moments included in this data set are derived from the velocity moments integration of solar wind electron distributions measured by the WIND/SWE VEIS instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the WIND spacecraft", Space Sci. Rev., 71, 55, 1955). Moments parameters are computed from 3s measurements which are spaced either 6s or 12s in time.  Plots should therefore not exceed a time range of 2 or 3 hours in order to display the details of this high resolution data.  The moments parameters which will be of value to most users of this data set are the electron temperature, the electron temperature anisotropy, and the electron heat flux vector. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretation with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the prime quantities of this data set, the electron temperature, the electron temperature anisotropy, and the electron heat flux. (All vector quantities are in GSE coordinates.) The temperature and temperature anisotropy are normalized to the derived electron density and, therefore, are not sensitive to  the uncertainty in the density determination as discussed below. The electron temperature is derived from the pressure tensor divided by the electron density and the Boltzmann constant. The three eigenvalues of the diagonalized temperature tensor are the temperature parallel to the tensor principal axis and the two perpendicular components of the temperature. The temperature anisotropy is defined here as the ratio of the parallel temperature to the average of the two perpendicular temperature components. The electron temperature is one-third of the trace of the diagonalized temperaturetensor. Also included is the unit vector along the principal axis of the pressure tensor as well as the cosine of the angle between the principal axis and the magnetic field vector. An indication that the principal axis has been uniquely defined is that the temperature anisotropy is significantly different from unity and that the principal axis and the magnetic field are nearly parallel or anti-parallel.The heat flux vector included here is significant only when the magnitude rises above the noise level, i.e., above the level 0.002 to 0.005 ergs/cm/cm/s.  The heat flux may be low in magnitude either due to a nearly isotropic distribution, due to electron counter-streaming, or due to a  low counting rate of the instrument. An indicator of a significant net heat flux is that the heat flux direction should track with the magnetic field direction. For this purpose, the cosine of the angle between the heat flux vector and the magnetic field is included, and should be close to  -1 or  +1 in order for the heat flux to be significant. In some cases it will be necessary to use electron pitch angle distributions (available on request from the SWE team) to decide whether low electron flux or counterstreaming account for a low net heat flux. It is also strongly recommended that 3s magnetic field data from the WIND/MFI experiment (not included in this data set) be used inconjunction with the SWE electron heat flux data to ensure a correct interpretation of the heat flux.The electron density and electron bulk flow velocity are also included in this data set but no claim is made for their accuracy. The electron flow velocity is usually within 10% to 20% of the solar wind flow velocity derived from the SWE Faraday cup experiment and which are found in the SWE key parameter data set. The electron density, however,  cannot be absolutely determined due to the spacecraft potential and the fact that the electron instrument response has varied over time. The electron density determination includes a first order attempt to determine the spacecraft potential by imposing the charge neutrality condition on the derived electron density and Faraday cup ion density. The electron density will be within a few percent of the solar wind density derived from the Faraday cup early in the mission (1994-1997), while later in the mission (1998 and onward), depending on the state of the instrument,  there will be times when the derived electron densitymay be as much as a factor 2 too low. Although the electron density is not derived absolutely, relative changes in electron density can usually be relied on. Both the electron density and electron flow speed track with variations in the ion density and ion flow speed, respectively. However, the user is strongly advised to use the SWE ion key parameters for the bulk plasma density and flow speed. 

Wind/SWE (Solar Wind Experiment) electron instruments, history and data products

SPDF/CDAWeb. Please also acknowledge the data producer: K. Ogilvie at GSFC Code 692

SPDF/SSCWeb. Please also acknowledge the data producer: K. Ogilvie at GSFC Code 692

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Ogilvie at GSFC Code 692

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_h0/1994/wi_h0_swe_19941229_v01.cdf. The most common cadence, 6397 [ms] = PT6.397S, occurred for 58.0556% of the 7578 timesteps. 

Solar Wind Experiment (from all.xml/instrument/description/@short)

6 - 12 sec solar wind electron moments (from Master/CDFglobalAttributes/Data_type)

SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263,1995.

Home Page (including daily plots, 1-min avg IDL savesets and radio burst lists).

Wind WAVES home page, the Radio and Plasma Wave Investigation on the Wind Spacecraft with links to the WAVES instrument description and for data plotting and access including IDL savesets and radio burst lists, hosted by NASA GSFC

General information concerning the Wind, Plasma and Radio Waves, WAVES, instrument

Bougeret, J.-L., M.L. Kaiser, P.J. Kellogg, R. Manning, K. Goetz, S.J. Monson, N. Monge, L. Friel, C.A. Meetre, C. Perche, L. Sitruk, and S. Hoang, WAVES: The radio and plasma wave investigation on the wind spacecraft, Space Sci. Rev., 71, 231-263, 1995, DOI: 10.1007/BF00751331.

SPDF/CDAWeb. Please also acknowledge the data producer: M. L. Kaiser at GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: M. L. Kaiser at GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: M. L. Kaiser at GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/wav_h0/1994/wi_h0_wav_19941112_v01.cdf. The most common cadence, 8832 [ms] = PT8.832S, occurred for 78.5582% of the 7628 timesteps. 

High Res. Plasma Density (from Master/CDFglobalAttributes/Data_type)

Electron density determined from insitu Fpe 'line'; position recognized by a neural network.

Electric field power in dB at the peak frequency selected by the neural network algorithm

Electron Density data quality: <50=bad,>50=Fair,>150=ok,>200=good

Wind Solar Wind Experiment, 92-sec Solar Wind Alpha and Proton Anisotropy Analysis

SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W.Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995Solar wind proton parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques.Data reported within this file do not exceed the limits of various parameters listed in the following section.  There may be more valid data in the original dataset that requires additional work to interpret but was discarded due to the limits.  In particular we have tried to exclude non-solar wind data from these files. We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow angles or any other derived parameter.For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining parallel and perpendicular temperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and converting the result back to a thermal speed.  The uncertainties are also propagated throughNotes: Data reported within this file do not exceed the limits of various paremeters listed in the following section.  There  may be more valid data in the original dataset that require  additional work to interpret but was discarded due to the limits.  In particular we have tried to exclude non-solar wind data and questionable alpha data from these files. We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow angles or any other derived parameter.  For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining parallel and perpendicular tmperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and converting the result back to a thermal speed.  The uncertainties are also.    propagated through  Limits: Minimum mach number:        1.5000000; Maximum chisq/dof:             100000.00; Minimum distance; to bow shock:                      5.0000000 [Re]; Maximum uncertainty in any; parameter from non-linear;analysis:                               70.0000[%].

SPDF/CDAWeb. Please also acknowledge the data producer: K. Ogilvie at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: K. Ogilvie at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Ogilvie at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_h1/1994/wi_h1_swe_19941117_v01.cdf. The most common cadence, 74642 [ms] = PT1M14.642S, occurred for 73.5450% of the 139 timesteps. 

100-sec Proton Anisotropy Analysis (from Master/CDFglobalAttributes/Data_type)

CDF Epoch time at the beginning of each SWE spectrum (milliseconds)

This flag denotes the fit quality and encodes any contingencies in the ion VDF analysis (10=SW parameters OK)

---> Fractional day of year of start of spectrum (Noon on January 1 = 1.5)

VX_GSE component of the proton vector velocity [km/s], from non-linear analysis

VY_GSE component of the proton vector velocity [km/s], from non-linear analysis

VZ_GSE component of the proton vector velocity [km/s], from non-linear analysis

Scalar [isotropic] proton thermal speed [km/s], from the trace of the anisotropic temperatures.

Proton thermal speed perpendicular to the magnetic field direction [km/s].

1-sigma uncertainty in the perpendicular proton thermal speed [km/s].

---> 1-sigma uncertainty in the perpendicular proton thermal speed [km/s].

Proton thermal speed parallel to the magnetic field direction [km/s].

1-sigma uncertainty in the parallel proton thermal speed [km/s].

---> 1-sigma uncertainty in the parallel proton thermal speed [km/s].

Proton number density Np (n/cc) from non-linear analysis (linear scale)

Alpha velocity component Vx (GSE, km/s) from non-linear analysis

Alpha velocity component Vy (GSE, km/s) from non-linear analysis

Alpha velocity component Vz (GSE, km/s) from non-linear analysis

Alpha particle thermal speed perpendicular to the magnetic field direction [km/s].

1-sigma uncertainty in the perpendicular alpha thermal speed [km/s].

---> 1-sigma uncertainty in the perpendicular alpha thermal speed [km/s].

Alpha thermal speed parallel to the magnetic field direction [km/s].

Alpha particle thermal speed parallel to the magnetic field direction [km/s]

---> Time that the peak charge flux was observed for each spectrum (in fractional day of year)

1-sigma uncertainty in time of peak flux (in fractional day of year)

---> 1-sigma uncertainty in time of peak flux (in fractional day of year)

Proton thermal speed Wperpendicular (km/s) from bimax moment analysis

Proton thermal speed Wparallel (km/s) from bimax moment analysis

Magnetic field component Bx (GSE, nT) averaged over plasma measurement

Magnetic field component By (GSE, nT) averaged over plasma measurement

Magnetic field component Bz (GSE, nT) averaged over plasma measurement

Angluar deviation of magnetic field over plasma measurement [degrees]

Solar wind proton and alpha parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. Data in RTN

Notes:    - Data reported within this file do not exceed the limits of     various paremeters listed in the following section.  There     may be more valid data in the original dataset that requires     additional work to interpret but was discarded due to the     limits.  In particular we have tried to exclude non-solar     wind data and questionable alpha data from these files.   - We provide the one sigma uncertainty for each parameter     produced by the non-linear curve fitting analysis either     directly from the fitting or by propagating uncertainties     for bulk speeds, flow angles or any other derived parameter.   - For the non-linear anisotropic proton analysis, a scalar     thermal speed is produced by determining parallel and     perpendicular tmperatures, taking the trace,      Tscalar = (2Tperp + Tpara)/3 and converting the result     back to a thermal speed.  The uncertainties are also     propagated through   ; Limits: ;	Minimum mach number:        1.5000000 ;	Maximum chisq/dof:             100000.00 ;	Minimum distance  ;	  to bow shock:                      5.0000000 [Re] ;	Maximum uncertainty in any ;          	  parameter from non-linear ;          	  analysis:                               70.0000[%] 

SPDF/CDAWeb. Please also acknowledge the data producer: Bennett Maruca at University of Delaware

SPDF/SSCWeb. Please also acknowledge the data producer: Bennett Maruca at University of Delaware

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Bennett Maruca at University of Delaware

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_h1_rtn/1994/wi_h1_swe_rtn_19941117_v01.cdf. The most common cadence, 74642 [ms] = PT1M14.642S, occurred for 73.5450% of the 139 timesteps. 

R_RTN component of the proton vector velocity [km/s], from non-linear analysis

T_RTN component of the proton vector velocity [km/s], from non-linear analysis

N_RTN component of the proton vector velocity [km/s], from non-linear analysis

---> 1-sigma uncertainty in the proton trace thermal speed [km/s].

Alpha velocity component Vr (RTN, km/s) from non-linear analysis

Alpha velocity component Vt (RTN, km/s) from non-linear analysis

Alpha velocity component Vn (RTN, km/s) from non-linear analysis

Magnetic field component Br (RTN, nT) averaged over plasma measurement

Magnetic field component Bt (RTN, nT) averaged over plasma measurement

Magnetic field component Bn (RTN, nT) averaged over plasma measurement

 The Radio and Plasma Wave Investigation on the WIND Spacecraft, Sp.Sci.Rev.,Vol 71, pg,  231-263,1995.

Web Service to this product using the HAPI interface. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch2.)

Web Service user interface that generates scripts in IDL, Javascript, MATLAB, Python, Autoplot, curl, wget to access this product. See https://hapi-server.org/servers/api for the API. Note that HAPI dataset has a collection of parameters, each having the same time stamps. This CDAWeb dataset contains 2 HAPI-type datasets. The @0, @1, ... at the end of the ParameterKeys indicates the index of the CDAWeb dataset. (The dataset index <=> CDF file time variable pairs are @0 => Epoch, @1 => Epoch2.)

Radio/Plasma Wave,Radio (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/wav_h1/1994/wi_h1_wav_19941110_v01.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

[NO PLOTS] Daily receiver minimum voltage (RAD2, 1075-13825 kHz, non-zero values show active freqs)

[NO PLOTS] Daily receiver minimum voltage (RAD1, 20-1040 kHz, non-zero values show active freqs)

[NO PLOTS] Daily receiver minimum voltage (TNR, 4-245 kHz, non-zero values show active freqs)

Wind Magnetic Fields Investigation, High-resolution Definitive Data

WIND MFI high-resolution data file. Time resolution varies with instrument mode.Modes 0 & 10, low rate: .184s, high rate: .092s                                 Modes 1 & 11, low rate: Prim .092s Sec 1.84s, high rate: Prim .046s Sec .92s    Modes 2 & 12, Same as Modes 1 & 11                                              Calibration constants are 1 minute averages.                                    WIND MFI Instrument turn on 11/12/1994                                          Data versions:                                                                  03 - Extrapolated Bz correction                                                 04 - Final Bz correction                                                        05 - Final attitude and Bz correction                                              References:                                                                     1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in     The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995                  2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.     3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   The International Solar-Terrestrial Physics (ISTP) Program Information          Processing Division Ground Data Processing System and The ISTP Mission          Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         Magnetometer Experiment, September 1987.                                        5. National Space Science Data Center, CDF User's Guide, Version 2.3.0,        October 1, 1992.                                                                6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter    Generation Software (KPGS) Standards & Conventions, September 1992.             7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972         

WIND Magnetic Field Investigation (MFI) High-Resolution Production

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h2/1994/wi_h2_mfi_19941113_v05.cdf. The most common cadence, 92 [ms] = PT0.092S, occurred for 99.6859% of the 315163 timesteps. 

High-resolution Definitive Data (from Master/CDFglobalAttributes/Data_type)

Wind Magnetic Fields Investigation: 3 sec, 1 min, and hourly Definitive Data (RTN).

WIND Magnetic Field Investigation (MFI) Standard Production (RTN)

3 sec, 1 min, and hourly Definitive Data (RTN) (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h3-rtn/1994/wi_h3-rtn_mfi_19941113_v05.cdf. The most common cadence, 60000 [ms] = PT1M, occurred for all 1439 timesteps. 

Counts based on variable 'Epoch3' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h3-rtn/1994/wi_h3-rtn_mfi_19941113_v05.cdf. The most common cadence, 3000 [ms] = PT3S, occurred for all 28799 timesteps. 

Counts based on variable 'Epoch1' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h3-rtn/1994/wi_h3-rtn_mfi_19941113_v05.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 23 timesteps. 

Wind Solar Wind Experiment (SWE), 9 sec solar wind electron pitch-angle distributions at 12 sec cadence

Explanatory notes: The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., 'SWE, a comprehensive plasma instrument for the Wind spacecraft', Space Sci. Rev., 71, 55, 1955).Pitch-angle distrubutions, organized by energy, are computed from 9s measurements which are usually separated by one or more 3s spin-periods.  These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set.  For each 'energy spectrum', observations are made at 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV.  The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B).  A 'spin-averaged' set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel.  The value reported for any bin (including the spin-averaged 'energy bins' is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 13 spin-averaged energy bins).  For reference, the electron speeds (|V|, in cm/s) corresponding to the energy channels used, are reported in this   data set.

Additional information about instruments and parameters is available on the

SPDF/CDAWeb. Please also acknowledge the data producer: K. Ogilvie at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: K. Ogilvie at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Ogilvie at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_h3/2002/wi_h3_swe_20020816_v01.cdf. The most common cadence, 12684 [ms] = PT12.684S, occurred for 27.3897% of the 1788 timesteps. 

9 sec solar wind electron pitch-angle distributions (from Master/CDFglobalAttributes/Data_type)

Electron pitch-angle distributions (6 degrees/bin), energy channel 00 (19.34 eV, 2.60e+08 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 01 (38.68 eV, 3.68e+08 cm/s

Electron pitch-angle distributions (6 degrees/bin), energy channel 02 (58.03 eV, 4.51e+08 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 03 (77.37 eV, 5.21e+08 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 04 (96.71 eV, 5.82e+08 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 05 (116.1 eV, 6.38e+08 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 06 (193.4 eV, 8.23e+08 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 07 (290.1 eV, 1.00e+09 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 08 (425.5 eV, 1.22e+09 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 09 (580.3 eV, 1.42e+09 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 10 (773.7 eV, 1.64e+09 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 11 (1006 eV, 1.87e+09 cm/s)

Electron pitch-angle distributions (6 degrees/bin), energy channel 12 (1238 eV, 2.08e+09 cm/s)

Wind Magnetic Fields Investigation, High-resolution Definitive Data (RTN)

WIND Magnetic Field Investigation (MFI) High-Resolution Production (RTN)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_h4-rtn/1994/wi_h4-rtn_mfi_19941113_v05.cdf. The most common cadence, 92 [ms] = PT0.092S, occurred for 99.9718% of the 318846 timesteps. 

High-resolution Definitive Data (RTN) (from Master/CDFglobalAttributes/Data_type)

Wind Solar Wind Experiment (SWE), 3 sec solar wind electron pitch-angle distributions at 6-12 sec cadence

Explanatory notes: The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955).Pitch-angle distrubutions, organized by energy, are computed from 3s measurements which are spaced either 6s or 12s in time.  These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set.  For each 'energy spectrum', observations are made at 16 energy channels ranging from about 10 eV to as much as 3 keV.  The exact energies at which observations are made is time-varying, and this data set reports the energy each channel observes (along with the observations themselves) at any time.  The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B).  A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel.  The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors.The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12, f_pitch_E13, f_pitch_E14, f_pitch_E15 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 16 spin-averaged energy bins).For reference, the electron speeds (|V|, in cm/s) corresponding to the energy channels used, are reported in this data set.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_h4/1994/wi_h4_swe_19941130_v01.cdf. The most common cadence, 6220 [ms] = PT6.22S, occurred for 64.8772% of the 8109 timesteps. 

3 sec solar wind electron pitch-angle distributions (from Master/CDFglobalAttributes/Data_type)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 00 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 01 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 02 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 03 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 04 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 05 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 06 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 07 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 08 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 09 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 10 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 11 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 12 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 13 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 14 (time-varying energy value)

Electron pitch-angle distributions (6 degrees/bin), energy chanel 15 (time-varying energy value)

Wind Solar Wind Experiment (SWE), 9 sec solar wind electron moments at 12 sec cadence

Explanatory notes: The electron moments included in this data set are derived from quadrature integration of the solar wind electron distributions (w/ some fitting) measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955).Moments parameters are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing.The following comments are intended to aid in the use and interpretation of the prime quantities of this data set, the electron density, bulk-velocity and temperature.  We compensate for the limited nature of our observations under this instrument mode by combining electron observations with bulk-velocity estimates derived from corresponding ion observations.  The (13) energy channels over which observations are made are: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV; f(E,Az,El) [#/{cc*(cm/s)^3}] being obtained for each E, using an 8x6 grid of look-directions (Azimuth x Elevation, with ~45x9 deg. "pixels")--thus constituting an 'electron distribution'.  A fitted Maxwellian model supplements the "core" regime of each distribution.  N_elec [#/cc] gives the density value derived for the full distribution, while NcElec [#/cc] gives that of the core.  U_eGSE and UceGSE [km/s, GSE], resp. supply the full and core bulk-velocity.  P_eGSE [erg/cc, GSE] has the [Pxx, Pxy, Pxz, Pyy, Pyz, Pzz] components of the derived pressure-tensor.  T_elec and TcElec [K], resp. provide the full and core total-temperatures; W_elec and WcElec [eV] specifying the corresponding thermal-energies.  Te_pal, Te_per, TecPal and TecPer [K] give resp. full and core parallel- and perpendicular-temperatures (wrt B), with Te_ani and TecAni [unitless] furnishing the perpendicular/parallel temperature-anisotropies for each regime.  Finally, Gyrtrp [unitless] indicates the derived electron gyrotropy.The data set reported here contains: N_elec, NcElec, U_eGSE, UceGSE, P_eGSE, T_elec, TcElec, W_elec, WcElec, Te_pal, Te_per, TecPal, TecPer, Te_ani, TecAni, and Gyrtrp (as described above).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_h5/2002/wi_h5_swe_20020816_v01.cdf. The most common cadence, 12684 [ms] = PT12.684S, occurred for 28.5574% of the 1750 timesteps. 

9 sec solar wind electron moments (from Master/CDFglobalAttributes/Data_type)

Aniso_e core Electron temperature-anisotropy (TePer_core/TePal_core)

Electron flux energy levels: channel 1: 0.1-.4   keV      channel 2: 0.4-1.8  keV      channel 3: 1.9-8.0  keV      channel 4: 9.0-30   keV      channel 5: 20-48    keV      channel 6: 43-138   keV      channel 7: 127-225  keV      Ion flux energy levels:      channel 1: 0.07-.21 keV      channel 2: 0.25-1.1 keV      channel 3: 1.3-7    keV      channel 4: 8-30     keV      channel 5: 20-58    keV      channel 6: 58-126   keV      channel 7: 115-400  keV      pfu == 1/(cm^2-s-sr-keV)     

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/3dp/3dp_k0/2019/wi_k0_3dp_20190101_v04.cdf. The most common cadence, 92000 [ms] = PT1M32S, occurred for 99.0405% of the 929 timesteps. 

3-D Plasma Analyzer (from all.xml/instrument/description/@short)

Wind Energetic Particle Acceleration Composition Transport, Key Parameters [PRELIM]

The parameters contained in this data set are: low energy He, Oxygen, and Iron fluxes in the range 3.2 to 6.2 keV/n; electron flux in the range 1 to 10 Mev/n; proton flux in two contiguous channels from 19 to 72 Mev/n; He flux in four channels from 19 to 640 keV/n; CNO flux in two channels 80 to 640 keV/n; and Iron flux in two channels 80 to 1050 kev/n. The experiment home page at http://lheawww.gsfc.nasa.gov/docs/gamcosray/lecr/EPACT/epact.html gives more detailed information about the instrument. 

SPDF/CDAWeb. Please also acknowledge the data producer: T. Von Roseavinge at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: T. Von Roseavinge at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. Von Roseavinge at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/epact_k0/1994/wi_k0_epa_19941116_v02.cdf. The most common cadence, 46000 [ms] = PT46S, occurred for 99.9467% of the 1874 timesteps. 

Energetic Particle Acceleration Composition Transport (from all.xml/instrument/description/@short)

References:                                                                     1. Panetta P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.   2. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   The International Solar-Terrestrial Physics (ISTP) Program Information          Processing Division Ground Data Processing System and The ISTP Mission          Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        3. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         Magnetometer Experiment, September 1987.                                        

Wind Magnetic Field Innstrument, MFI, description, hosted by NASA GSFC

Wind MFI and SWE Key Parameter Data Access and Plotting web page, GSFC

Wind Magnetic Field Innstrument, MFI, and Solar Wind Experiment, SWE, Key Parameter data access and plotting web page with selectable overplotting of DSCOVR data and links to CDF data directories, hosted by NASA GSFC

General information concerning the Wind, Magnetic Fields Instrument, MFI, instrument

Wind Magnetic Field Investigation, MFI, instrument, Space Science Reviews publication

R.P. Lepping, M.H. Acũna, L.F. Burlaga, W.M. Farrell, J.A. Slavin, K.H. Schatten, F. Mariani, N.F. Ness, F.M. Neubauer, Y.C. Whang, J.B. Byrnes, R.S. Kennon, P.V. Panetta, J. Scheifele, and E.M. Worley, The WIND magnetic field investigation, Space Sci. Rev., 71, 207-229, 1995, DOI: 10.1007/BF00751330.

SPDF/CDAWeb. Please also acknowledge the data producer: R. Lepping at NASA/GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: R. Lepping at NASA/GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: R. Lepping at NASA/GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_k0/2017/wi_k0_mfi_20170701_v01.cdf. The most common cadence, 92000 [ms] = PT1M32S, occurred for 99.0395% of the 928 timesteps. 

Solar Wind and Suprathermal Ion Composition  Instrument, Key Parameters [PRELIM]

Time is for the start of the averaging interval. Computed are the avg alpha vel; avg C/O abundance ratio; avg carbon ionization temp in million degs K from C+6 & C+5 (using the tbls of Arnaud & Rothenflug, 1985); the avg oxygen ionization temp from O+7 & O+6 inmillion degs K (using tbls of Arnaud & Rothenflug, 1985)Above avgs are made over 4 hrs.He vel and He kinetic temp are computed every 3 min & are contained in the K1 CDFReferences:                   Space Science Reviews 71:79-124, 1995, Kluwer Academic Publishers, Belgium  Instrument consist of: Solar Wind Ion Composition Spectrometer (SWICS); high resolution mass  spectrometer (MASS); Supra-Thermal Ion Composition Spectrometer (STICS) & common DPU

Monthly and Daily Browse Plots (SWICS to 2/1998, STICS to 11/1998)

SPDF/CDAWeb. Please also acknowledge the data producer: G. Gloeckler at U of Maryland

SPDF/SSCWeb. Please also acknowledge the data producer: G. Gloeckler at U of Maryland

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: G. Gloeckler at U of Maryland

Solar Wind & Suprathermal Ion Composition Investigation (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/orbit/spha_k0/2025/wi_k0_spha_20250430_v01.cdf. The most common cadence, 92000 [ms] = PT1M32S, occurred for 99.8934% of the 937 timesteps. 

SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W.Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995 USE OF THE QUALITY VARIABLES:  *** Good data is indicated by a quality flag of 0. ***The quality flags for each parameter are given as integers 4 bytes long (integer*4).  The individual 'bits' for each quality value are set (or cleared) in the analysis code by adding (or subtracting) a power of 2 as follows: To set the 1st bit, add 1. To set the 2nd bit, add 2, To set the 3rd bit, add 4, To set the 4th bit, add 8, and so on.      BIT  TO_SET_BIT     MEANING     1    +1         = 3 point parabolic fits to proton peaks were not attempted.     2    +2         = non-linear least squares fit was not attempted.     3    +4         = 3 point parabolic fits to proton peaks FAILED.     4    +8         = non-linear least squares fit FAILED.  See https://cdaweb.gsfc.nasa.gov/wind_swe_quality.html For the complete guide to the quality flag values.  

Wind Solar Wind Experiment, SWE, web page hosted by the Massachusetts Institute of Technology Space Plasma group. Since the Summer of 2015, the responsibility for Wind plasma data has been assumed by the Harvard Smithsonian Astrophysics Lab.

General information concerning the Wind, Solar Wind Experiment, SWE, instrument

Wind Solar Wind Experiment, SWE, Instrument description web page hosted by the Massachusetts Institute of Technology Space Plasma group

Ogilvie, K.W., D.J. Chornay, R.J. Fritzenreiter, F. Hunsaker, J. Keller, J. Lobell, G. Miller, J.D. Scudder, E.C. Sittler, Jr., R.B. Torbert, D. Bodet, G. Needell, A.J. Lazarus, J.T. Steinberg, J.H. Tappan, A. Mavretic, and E. Gergin, SWE, a comprehensive plasma instrument for the Wind spacecraft, Space Sci. Rev., 71, 55-77, 1995, DOI: 10.1007/BF00751326

Wind Solar Wind Experiment, SWE, Key Parameter Readme file, hosted by the Massachusetts Institute of Technology, MIT

Velocity Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID

Proton Density Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID

Ion Bulk Flow vector in GSE coord.,  3 comp. (speed, E/W flow, N/S flow)

SWE, a comprehensive plasma instrument for the WIND spacecraft,  K.W. Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995.USE OF THE QUALITY VARIABLES: Quality flags are set in the analysis program that generates the KP data.  Previous descriptions of their meaning were out of date.Good data is indicated by a quality flag of 0. The quality flags for each parameter are given as integers 4 bytes long (integer*4).  The individual 'bits' for each quality value are set (or cleared) in the analysis code by adding (or subtracting) a power of 2 as follows: To set the 1st bit, add 1.  To set the 2nd bit, add 2. To set the 3rd bit, add 4.  To set the 4th bit, add 8, and so on. BIT  TO_SET_BIT     MEANING 1    +1     = 3 point parabolic fits to proton peaks were not attempted. 2    +2     = non-linear least squares fit was not attempted. 3    +4     = 3 point parabolic fits to proton peaks FAILED.  4    +8     = non-linear least squares fit FAILED. (Non-linear fit may be reported as good for protons and, at the same time, not good for alphas.) 5    +16    = Alpha params not valid for reason that the non-linear least squares fit was done for protons only.  Not enough good energy channels to do simultaneous alpha fit. (This value applies to iqual_core(5) only.) 6    +32    = analysis code unable to get good value for spin period. 7    +64    = SWE instrument in mode 1 - calibration state.  Key parameters not produced this mode, only in mode 1 - science.  8   +128   = 3 point fits done for cup 1 only.  Split collector ratio of currents used to get n/s angle.  Either cup 2 turned off, or cup 2 densities were low indicating noise associated with vibration. 9   +256   = fewer than 10 fc_blocks in spectrum. Analysis skipped. 10  +512   = Alpha non-linear fit produced values of thermal speed and density that do not seem reasonable. 11  +1024   = 3 point parabolic fits to proton peaks done for cup 2 only. Ratio of currents on split collectors used to get n/s angle.  Probably Cup 1 is turned off. 12  +2048   = single width windows.  Delta E over E 6/5% instead of the default 13%.  13  +4096   = tracking mode operation 14  +8192   = Limited tracking mode scan (Not a full scan)Comments: Non-linear fits are not done for Key Parameters (KPs), but those parameter values are excellent and should be used to do science; non-linear fits are available, but they have problems which suggest strongly that the KP parameters should be used (see paper by Kasper et al., 'Physics-based tests to identify the accuracy of solar wind ion measurements: A case study with the Wind Faraday Cups', J. Geophys. Res., 111, A03105, doi:101029/2005JA011442. Examples (note that all are even numbers because non-linear fits were not attempted) FLAG   Meaning 4098   Tracking mode (4096) full scan  + no non-linear (2) 14338  Limited tracking mode (8192) + Tracking mode (4096) See http://cdaweb.gsfc.nasa.gov/wind_swe_quality.html for the complete guide to the quality flag values.  

Ion Bulk Flow vector in RTN coord.,  3 comp. (speed, E/W flow, N/S flow)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/wav_k0/1994/wi_k0_wav_19941110_v01.cdf. The most common cadence, 180000 [ms] = PT3M, occurred for all 479 timesteps. 

Electric field average intensity in dB above background at 76 log-spaced frequencies (250-9.4e6 Hz).

Transient electric field antenna max from Time Domain Sampler. 0 indicates no trigger.

Wind Magnetic Fields Investigation, Key Parameters in RTN [PRELIM]

SPDF/CDAWeb. Please also acknowledge the data producer: Andriy Koval at UMBC&GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Andriy Koval at UMBC&GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Andriy Koval at UMBC&GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/mfi/mfi_k1-rtn/2017/wi_k1-rtn_mfi_20170101_v01.cdf. The most common cadence, 92000 [ms] = PT1M32S, occurred for 99.0405% of the 929 timesteps. 

Key Parameters in RTN (from Master/CDFglobalAttributes/Data_type)

Wind EPACT-APE_B  H 18.90 -21.90 MeV Solar Energetic Particle Intensities, 1-Hour Level 2 Data

The Energetic Particles: Acceleration, Composition and Transport (EPACT) on Wind APE-B Telescope measures proton fluxes 18.90 to 21.90 MeV energetic particle energy 

Access to Wind Energetic Particles: Acceleration, Composition and Transport, EPACT, Solar Energetic Particle, SEP, ASCII Data Files

SPDF/CDAWeb. Please also acknowledge the data producer: T. Von Rosenvinge & D. Reames at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: T. Von Rosenvinge & D. Reames at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: T. Von Rosenvinge & D. Reames at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/epact_l2-1hour-ape_b/wi_l2-1hour-sep_epact-ape_b_19940101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 1415 timesteps. 

---> H intensity, at 1 energy 18.90-21.90 MeV/nuc (time-series with uncertainties)

Wind EPACT-LEMT He/C/O/Ne/Si/Fe 2-11 MeV/Nuc Solar Energetic Particle Intensities, 1-Hour Level 2 Data

The EPACT Instrument on Wind   LEMT - Low Energy Matrix Telescope measures ion fluxes over the charge range from He through Ni from about 0.1 MeV/nucleon to 30 MeV/nucleon, thus coveringenergetic particle energy ranges.Exploratory measurements of ultra-heavy species (mass range above Ni) will also be performed

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/epact_l2-1hour-sep/1994/wi_l2-1hour-sep_epact-lemt_19940101_v01.cdf. The most common cadence, 3600000 [ms] = PT1H, occurred for all 1415 timesteps. 

---> He intensity, at 7 energies 2.2-8.5 MeV/nuc (time-series with uncertainties)

---> C intensity, at 7 energies 2.9-11.4 MeV/nuc (time-series with uncertainties)

---> O intensity, at 7 energies 2.9-11.3 MeV/nuc (time-series with uncertainties)

---> Ne intensity, at 6 energies 3.6-11.3 MeV/nuc (time-series with uncertainties)

---> Si intensity, at 7 energies 2.8-11.6 MeV/nuc (time-series with uncertainties)

---> Fe intensity, at 7 energies 2.7-10.9 MeV/nuc (time-series with uncertainties)

Solar Wind and Suprathermal Ion Composition  Instrument, Key Parameters

The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space.  The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.

SPDF/CDAWeb. Please also acknowledge the data producer: S. T. Lepri at U of Michigan

SPDF/SSCWeb. Please also acknowledge the data producer: S. T. Lepri at U of Michigan

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: S. T. Lepri at U of Michigan

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/30min_afm_magnetosphere/1995/wi_l2-30min_sms-stics-afm-magnetosphere_19950801_v01.cdf. The most common cadence, 1840430 [ms] = PT30M40.43S, occurred for 19.1489% of the 9 timesteps. 

SMS Solar Wind & Suprathermal Ion Composition Investigation AFM magnetosphere (from all.xml/instrument/description/@short)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/30min_afm_solarwind/1995/wi_l2-30min_sms-stics-afm-solarwind_19950101_v01.cdf. The most common cadence, 1935362 [ms] = PT32M15.362S, occurred for 14.8936% of the 7 timesteps. 

SMS Solar Wind & Suprathermal Ion Composition Investigation solarwind AFM solarwind (from all.xml/instrument/description/@short)

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence H+

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence He+

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence He2+

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence O+

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence O6+

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence C5+

Angular flux map gives the flux of ions flowing in a given direction in triple coincidence Fe10+

Angular flux map gives the flux of ions flowing in a given direction in double coincidence H+

Angular flux map gives the flux of ions flowing in a given direction in double coincidence He+

Angular flux map gives the flux of ions flowing in a given direction in double coincidence He2+

Angular flux map gives the flux of ions flowing in a given direction in double coincidence O+

Angular flux map gives the flux of ions flowing in a given direction in double coincidence O6+

Magnetosphere and Suprathermal Ion Composition  Instrument, Key Parameters

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/30min_erpa_magnetosphere/1995/wi_l2-30min_sms-stics-erpa-magnetosphere_19950801_v01.cdf. The most common cadence, 1840430 [ms] = PT30M40.43S, occurred for 19.1489% of the 9 timesteps. 

SMS Magnetosphere & Suprathermal Ion Composition Investigation magnetosphere ERPA magnetosphere (from all.xml/instrument/description/@short)

Pitch-angle distributions triple coincidence H+ - summed over energy

Energy-resolved pitch-angle distributions triple coincidence He+

Pitch-angle distributions triple coincidence He+ - summed over energy

Energy-resolved pitch-angle distributions triple coincidence He2+

Pitch-angle distributions triple coincidence He2+ - summed over energy

Pitch-angle distributions triple coincidence O+ - summed over energy

Energy-resolved pitch-angle distributions triple coincidence O6+

Pitch-angle distributions triple coincidence O6+ - summed over energy

Energy-resolved pitch-angle distributions triple coincidence C5+

Pitch-angle distributions triple coincidence C5+ - summed over energy

Energy-resolved pitch-angle distributions triple coincidence Fe10+

Pitch-angle distributions triple coincidence Fe10+ - summed over energy

Pitch-angle distributions double coincidence H+ - summed over energy

Energy-resolved pitch-angle distributions double coincidence He+

Pitch-angle distributions double coincidence He+ - summed over energy

Energy-resolved pitch-angle distributions double coincidence He2+

Pitch-angle distributions double coincidence He2+ - summed over energy

Pitch-angle distributions double coincidence O+ - summed over energy

Energy-resolved pitch-angle distributions double coincidence O6+

Pitch-angle distributions double coincidence O6+ - summed over energy

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/30min_erpa_solarwind/1995/wi_l2-30min_sms-stics-erpa-solarwind_19950101_v01.cdf. The most common cadence, 1935362 [ms] = PT32M15.362S, occurred for 14.8936% of the 7 timesteps. 

SMS Solar Wind & Suprathermal Ion Composition Investigation solarwind ERPA solarwind (from all.xml/instrument/description/@short)

The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space.  The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�� steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/3min_vdf_magnetosphere/1995/wi_l2-3min_sms-stics-vdf-magnetosphere_19950801_v01.cdf. The most common cadence, 181934 [ms] = PT3M1.934S, occurred for 24.4681% of the 92 timesteps. 

SMS Magnetosphere & Suprathermal Ion Composition Investigation VDF magnetosphere (from all.xml/instrument/description/@short)

[no plot] Full 3-D VDF in phase space density for triple coincidence H+

Phase space density value triple coincidence H+ - summed over telescope and sector

Phase space density value triple coincidence H+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value triple coincidence H+

Counts for triple coincidence H+ - summed over telescope and sector

Counts for triple coincidence H+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence H+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence H+

Differential flux, dJ/dE triple coincidence H+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence H+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence H+

[no plot] Full 3-D VDF in phase space density for triple coincidence He+

Phase space density value triple coincidence He+ - summed over telescope and sector

Phase space density value triple coincidence He+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value triple coincidence He+

Counts for triple coincidence He+ - summed over telescope and sector

Counts for triple coincidence He+ - summed over telescope and eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence He+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence He+

Differential flux, dJ/dE triple coincidence He+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence He+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence He+

[no plot] Full 3-D VDF in phase space density for triple coincidence He2+

Phase space density value triple coincidence He2+ - summed over telescope and sector

Phase space density value triple coincidence He2+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value triple coincidence He2+

Counts for triple coincidence He2+ - summed over telescope and sector

Counts for triple coincidence He2+ - summed over telescope and eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence He2+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence He2+

Differential flux, dJ/dE triple coincidence He2+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence He2+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence He2+

[no plot] Full 3-D VDF in phase space density for triple coincidence O+

Phase space density value triple coincidence O+ - summed over telescope and sector

Phase space density value triple coincidence O+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value triple coincidence O+

Counts for triple coincidence O+ - summed over telescope and sector

Counts for triple coincidence O+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence O+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence O+

Differential flux, dJ/dE triple coincidence O+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence O+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence O+

[no plot] Full 3-D VDF in phase space density for triple coincidence O6+

Phase space density value triple coincidence O6+ - summed over telescope and sector

Phase space density value triple coincidence O6+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value triple coincidence O6+

Counts for triple coincidence O6+ - summed over telescope and sector

Counts for triple coincidence O6+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence O6+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence O6+

Differential flux, dJ/dE triple coincidence O6+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence O6+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence O6+

[no plot] Full 3-D VDF in phase space density for triple coincidence C5+

Phase space density value triple coincidence C5+ - summed over telescope and sector

Phase space density value triple coincidence C5+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value triple coincidence C5+

Counts for triple coincidence C5+ - summed over telescope and sector

Counts for triple coincidence C5+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence C5+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence C5+

Differential flux, dJ/dE triple coincidence C5+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence C5+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence C5+

[no plot] Full 3-D VDF in phase space density for triple coincidence Fe10+

Phase space density value triple coincidence Fe10+ - summed over telescope and sector

Phase space density value triple coincidence Fe10+ - summed over telescope and eoq (sorted sector)

Phase space density value triple coincidence Fe10+ (Telescope 2)

[no plot] Error in velocity distribution function value triple coincidence Fe10+

Counts for triple coincidence Fe10+ - summed over telescope and sector

Counts for triple coincidence Fe10+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics triple coincidence Fe10+

[no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence Fe10+

Differential flux, dJ/dE triple coincidence Fe10+ - summed over telescope and sector

Differential flux, dJ/dE triple coincidence Fe10+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value triple coincidence Fe10+

[no plot] Full 3-D VDF in phase space density for double coincidence H+

Phase space density value double coincidence H+ - summed over telescope and sector

Phase space density value double coincidence H+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value double coincidence H+

Counts for double coincidence H+ - summed over telescope and sector

Counts for double coincidence H+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics double coincidence H+

[no plot] Full 3-D VDF differential flux, dJ/dE double coincidence H+

Differential flux, dJ/dE double coincidence H+ - summed over telescope and sector

Differential flux, dJ/dE double coincidence H+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value double coincidence H+

[no plot] Full 3-D VDF in phase space density for double coincidence He+

Phase space density value double coincidence He+ - summed over telescope and sector

Phase space density value double coincidence He+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value double coincidence He+

Counts for double coincidence He+ - summed over telescope and sector

Counts for double coincidence He+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics double coincidence He+

[no plot] Full 3-D VDF differential flux, dJ/dE double coincidence He+

Differential flux, dJ/dE double coincidence He+ - summed over telescope and sector

Differential flux, dJ/dE double coincidence He+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value double coincidence He+

[no plot] Full 3-D VDF in phase space density for double coincidence He2+

Phase space density value double coincidence He2+ - summed over telescope and sector

Phase space density value double coincidence He2+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value double coincidence He2+

Counts for double coincidence He2+ - summed over telescope and sector

Counts for double coincidence He2+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics double coincidence He2+

[no plot] Full 3-D VDF differential flux, dJ/dE double coincidence He2+

Differential flux, dJ/dE double coincidence He2+ - summed over telescope and sector

Differential flux, dJ/dE double coincidence He2+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value double coincidence He2+

[no plot] Full 3-D VDF in phase space density for double coincidence O+

Phase space density value double coincidence O+ - summed over telescope and sector

Phase space density value double coincidence O+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value double coincidence O+

Counts for double coincidence O+ - summed over telescope and sector

Counts for double coincidence O+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics double coincidence O+

[no plot] Full 3-D VDF differential flux, dJ/dE double coincidence O+

Differential flux, dJ/dE double coincidence O+ - summed over telescope and sector

Differential flux, dJ/dE double coincidence O+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value double coincidence O+

[no plot] Full 3-D VDF in phase space density for double coincidence O6+

Phase space density value double coincidence O6+ - summed over telescope and sector

Phase space density value double coincidence O6+ - summed over telescope and eoq (sorted sector)

[no plot] Error in velocity distribution function value double coincidence O6+

Counts for double coincidence O6+ - summed over telescope and sector

Counts for double coincidence O6+ - summed over telescope & eoq (sorted sector)

[no plot] Error in counts estimated assuming Poisson statistics double coincidence O6+

[no plot] Full 3-D VDF differential flux, dJ/dE double coincidence O6+

Differential flux, dJ/dE double coincidence O6+ - summed over telescope and sector

Differential flux, dJ/dE double coincidence O6+ - summed over telescope and eoq (sorted sector)

[no plot] Error in the differential flux value double coincidence O6+

Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/3min_vdf_solarwind/1995/wi_l2-3min_sms-stics-vdf-solarwind_19950101_v01.cdf. The most common cadence, 181439 [ms] = PT3M1.439S, occurred for 41.5138% of the 181 timesteps. 

SMS Solar Wind & Suprathermal Ion Composition Investigation VDF solarwind (from all.xml/instrument/description/@short)

Wind EPACT-LEMT He/C/O/Ne/Si/Fe 2-11 MeV/Nuc Solar Energetic Particle Intensities, 5min Level 2 Data

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/epact/epact_l2-5min-sept/1994/wi_l2-5min-sep_epact-lemt_19940101_v01.cdf. The most common cadence, 300000 [ms] = PT5M, occurred for 97.4178% of the 16411 timesteps. 

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/3min_nvt_magnetosphere/1995/wi_l2_3min_sms-stics-nvt-magnetosphere_19950801_v01.cdf. The most common cadence, 181934 [ms] = PT3M1.934S, occurred for 24.4681% of the 92 timesteps. 

SMS Solar Wind & Suprathermal Ion Composition Investigation (from all.xml/instrument/description/@short)

--- Error in the density value assuming Poisson statistics H+ triple coincidence

--- Error in the density value assuming Poisson statistics He+ triple coincidence

--- Error in the density value assuming Poisson statistics He2+ triple coincidence

--- Error in the density value assuming Poisson statistics O+ triple coincidence

--- Error in the density value assuming Poisson statistics O6+ triple coincidence

--- Error in the density value assuming Poisson statistics C5+ triple coincidence

--- Error in the density value assuming Poisson statistics Fe10+ triple coincidence

--- Error in the density value assuming Poisson statistics H+ double coincidence

--- Error in the density value assuming Poisson statistics He+ double coincidence

--- Error in the density value assuming Poisson statistics He2+ double coincidence

--- Error in the density value assuming Poisson statistics O+ double coincidence

--- Error in the density value assuming Poisson statistics O6+ double coincidence

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/sms/l2/stics_cdf/3min_nvt_solarwind/1995/wi_l2_3min_sms-stics-nvt-solarwind_19950101_v01.cdf. The most common cadence, 181439 [ms] = PT3M1.439S, occurred for 41.5138% of the 181 timesteps. 

This file includes radio measurements recorded by the Wind/WAVES/RAD1 instrument. Time resolution varies with instrument mode ranging from few tenth of seconds to 192 seconds

Please acknowledge the Principal Investigators, Dr. Karine Issautier (LESIA, Observatoire de Paris-PSL, CNRS) and Keith Goetz (University of Minnesota)

Data provided are publicly available. If used in presentations or publications, please acknowledge Wind/Waves Investigation (Karine Issautier, PI). Please read carefully the caveats attached to the data. For reporting purposes, we request bibliography information for any publication, etc., using these data. Please send information on the use of this data to: Karine Issautier (PI).

SPDF/CDAWeb. Please also acknowledge the data producer: Karine Issautier (Karine.Issautier@@obspm.fr) & Keith Goetz (goetz@@umn.edu) at LESIA, Observatoire de Paris-PSL, CNRS and University of Minnesota, respectively.

SPDF/SSCWeb. Please also acknowledge the data producer: Karine Issautier (Karine.Issautier@@obspm.fr) & Keith Goetz (goetz@@umn.edu) at LESIA, Observatoire de Paris-PSL, CNRS and University of Minnesota, respectively.

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Karine Issautier (Karine.Issautier@@obspm.fr) & Keith Goetz (goetz@@umn.edu) at LESIA, Observatoire de Paris-PSL, CNRS and University of Minnesota, respectively.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/rad1_l2/1995/wi_l2_wav_rad1_19950914_v01.cdf. The most common cadence, 45806752145 [ns] = PT45.806752S, occurred for 25.6182% of the 259 timesteps.

This file includes radio measurements recorded by the Wind/WAVES/RAD2 instrument. Time resolution varies with instrument mode ranging from few tenth of seconds to 192 seconds.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/rad2_l2/1994/wi_l2_wav_rad2_19941112_v01.cdf. The most common cadence, 16191986203 [ns] = PT16.191986S, occurred for 52.9712% of the 2799 timesteps.

This file includes radio measurements recorded by the Wind/WAVES/TNR instrument

Please acknowledge the Principal Investigators, Dr. Karine Issautier (LIRA, Observatoire de Paris-PSL, CNRS) and Keith Goetz (University of Minnesota)

SPDF/CDAWeb. Please also acknowledge the data producer: Karine Issautier (Karine.Issautier@obspm.fr) & Keith Goetz (goetz@umn.edu) at LIRA, Observatoire de Paris-PSL, CNRS & University of Minnesota

SPDF/SSCWeb. Please also acknowledge the data producer: Karine Issautier (Karine.Issautier@obspm.fr) & Keith Goetz (goetz@umn.edu) at LIRA, Observatoire de Paris-PSL, CNRS & University of Minnesota

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Karine Issautier (Karine.Issautier@obspm.fr) & Keith Goetz (goetz@umn.edu) at LIRA, Observatoire de Paris-PSL, CNRS & University of Minnesota

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/tnr_l2/1994/wi_l2_wav_tnr_19941110_v01.cdf. The most common cadence, 4415999936 [ns] = PT4.416S, occurred for 29.2817% of the 1390 timesteps.

Wind WAVES Time Domain Sampler (TDS) Dust Data File                 References:                                                         1)  Bougeret, J.-L., et al. `WAVES:  The Radio and Plasma Wave          Investigation on the Wind Spacecraft,` Space Sci. Rev. Vol. 71,     pp. 231-263, doi:10.1007/BF00751331, (1995).                    2)  Malaspina, D.M., M. Horanyi, A. Zaslavsky, K. Goetz,                L.B. Wilson III, and K. Kersten `Interplanetary and interstellar    dust observed by the Wind/WAVES electric field instrument,`         Geophys. Res. Lett. Vol. 41, pp. 266-272,                           doi:10.1002/2013GL058786, (2014).                               3)  Malaspina, D.M., and L.B. Wilson III `A Database of                 Interplanetary and Interstellar Dust Detected by the Wind           Spacecraft, J. Geophys. Res., doi:10.1002/2016JA023209, (2016).

We would like to thank the Wind/WAVES team, especially Keith Goetz, Paul J. Kellogg, Kris Kersten, and Josh Lynch for their support with data retrieval and calibration.

The Wind Database of Interplanetary and Interstellar Dust Events, JGR Article

Please cite/reference the Wind/WAVES paper by J.-L. Bougeret et al., [1995] in Space Science Reviews and work by Malaspina et al., [2014] in Geophysical Research Letters (doi:10.1002/2013GL058786).  We would also appreciate a reference to the Wind dust impact database paper:  Malaspina et al. [2016], in Journal of Geophysical Research (doi:10.1002/2016JA023209).

SPDF/CDAWeb. Please also acknowledge the data producer: D.M. Malaspina at U. Colorado at Boulder, LASP

SPDF/SSCWeb. Please also acknowledge the data producer: D.M. Malaspina at U. Colorado at Boulder, LASP

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: D.M. Malaspina at U. Colorado at Boulder, LASP

Time Domain Sampler (TDS) Fast Receiver (from all.xml/instrument/description/@short)

Dust Impact Information from WAVES TDS (from Master/CDFglobalAttributes/Data_type)

Avg. clockwise angle (degrees) of closest Ex antenna (to dust impact on spacecraft bus) from Earth-sun line (i.e., roughly +X-GSE)

Avg. clockwise angle (degrees) of closest Ey antenna (to dust impact on spacecraft bus) from Earth-sun line (i.e., roughly +X-GSE)

Avg. clockwise angle (degrees) of +Ex antenna from spacecraft-sun line

Avg. clockwise angle (degrees) of +Ex antenna from Earth-sun line (i.e., roughly +X-GSE)

Avg. clockwise angle (degrees) of +Ey antenna from Earth-sun line (i.e., roughly +X-GSE)

Wind Solar Wind Experiment (SWE), 9 sec solar wind electron pitch-angle distribution averages

Explanatory notes: The electron pitch-angle distribution averages included in this data set are derived from integrating the electron pitch-angle distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955).Averages of phase-space density (f) over key regions of the unit sphere     (the set of all possible electron velocity directions) are computed from 9s measurements which are usually separated by one or more 3s spin-periods.  These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing.The following comments are intended to aid in the use and interpretation of the averages reported in this data set.  We begin this analysis with a measure of f for each pitch-angle bin, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B).  The f values for pitch-angles from 0-90 degrees (parallel streaming) are integrated (with angluar weighting and assumptions of gyrotropy) over this half-sphere, then averaged by dividing out the 2-pi solid angle of the half-sphere; the result being referred to as the 'f_para' average.  Similarly, the 'f_perp' (flux nearly perpendicular to B) average is the result of integrating f for pitch-angles from 60-120 degrees (a region also 2-pi in solid angle).  Next, the 'f_anti' (flux nearly anti-parallel to B) average covers the half-sphere of "backward" streaming electrons; having pitch-angles from 90-180 degrees.  Finally, the 'f_omni' (omni-directional) average provides the integral of f over the full sphere, divided by the full 4-pi solid angle; providing a measure of total electron flux into the region of observation. The above analysis is carried out for each of 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV.  For reference, the electron speeds (|V|, in cm/s) corresponding to these energies are reported in this data set.  Hence the data set reported here contains: f_para, f_perp, f_anti, f_omni (for each of 13 values of E), and the 13 values of |V| (constant, included for reference).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_m0/2002/wi_m0_swe_20020816_v01.cdf. The most common cadence, 12684 [ms] = PT12.684S, occurred for 27.3897% of the 1788 timesteps. 

9 sec electron pitch-angle distribution averages (from Master/CDFglobalAttributes/Data_type)

Wind Solar Wind Experiment (SWE), 3 sec solar wind electron pitch-angle distribution averages

Explanatory notes:The electron pitch-angle distribution averages included in this data set are derived from integrating the electron pitch-angle distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955).Averages of phase-space density (f) over key regions of the unit sphere     (the set of all possible electron velocity directions) are computed from 3s measurements which are spaced either 6s or 12s in time.  These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing.The following comments are intended to aid in the use and interpretation of the averages reported in this data set.  We begin this analysis with a measure of f for each pitch-angle bin, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B).  The f values for pitch-angles from 0-90 degrees (parallel streaming) are integrated (with angluar weighting and assumptions of gyrotropy) over this half-sphere, then averaged by dividing out the 2-pi solid angle of the half-sphere; the result being referred to as the 'f_para' average.  Similarly, the 'f_perp' (flux nearly perpendicular to B) average is the result of integrating f for pitch-angles from 60-120 degrees (a region also 2-pi in solid angle).  Next, the 'f_anti' (flux nearly anti-parallel to B) average covers the half-sphere of "backward" streaming electrons; having pitch-angles from 90-180 degrees. Finally, the 'f_omni' (omni-directional) average provides the integral of f over the full sphere, divided by the full 4-pi solid angle; providing a measure of total electron flux into the region of observation.  The above analysis is carried out for each of 16 energy channels ranging from about 10 eV to as much as 3 keV.  The exact energies at which observations are made is time-varying, and this data set reports the electron speeds each channel observes (|V|, in cm/s, along with the observations themselves) at any time.  Hence the data set reported here contains: f_para, f_perp, f_anti, f_omni (for each of 16 values of |V|), and the 16 values of |V| (time-varying, although usually much more slowly than the order of a day).

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_m2/1994/wi_m2_swe_19941229_v01.cdf. The most common cadence, 6397 [ms] = PT6.397S, occurred for 70.4720% of the 9198 timesteps. 

3 sec electron pitch-angle distribution averages (from Master/CDFglobalAttributes/Data_type)

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/orbit/def_or/1997/wi_or_def_19970701_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

HEC Cartesian Position [available starting around 1995/05/01]                 

HEC Cartesian Velocity [available starting around 1995/05/01]                 

Carrington Rotation Number [available starting after 1996/03/01]

Heliographic Long of Earth [available starting around 1995/05/01]         

Heliographic Lat of Earth [available starting around 1995/05/01]          

Heliographic Long of Craft [available starting around 1995/05/01]              

Heliographic Lat of Craft [available starting around 1995/05/01]          

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/orbit/pre_or/2025/wi_or_pre_20250705_v01.cdf. The most common cadence, 600000 [ms] = PT10M, occurred for all 143 timesteps. 

HEC Cartesian Position (orbit display, available after 1995/05/10)

Carrington Rotation Number (available from 1995/05/10 - 1996/03/19 and 1996/11/20 on)

Ion omnidirectional fluxes 0.4-3 keV and moments, often at ~24 second resolution, PESA Low, Wind 3DP

Wind 3dp, PESA Low (~24 sec resolution) energy spectra with ion moments 

PESA (proton/ion electro-static analyzer) Low - Spectra Protons (from Master/CDFglobalAttributes/Data_type)

[FLUX] Proton number flux, 15 energy channels populated approximately 0.4-3 keV [spectrogram]

[P.SC_CURRENT?] Current contribution to the spacecraft from thermal protons

---> [P.MAGF] magnetic field vector interpolated (linearly) to the time of the PESA Low distribution, in GSE cartesian components

[P.PTENS] Proton Pressure Tensor calculated in the GSE coordinate basis.  The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ

---> [P.MFTENS] Proton Momentum Flux Tensor calculated in the GSE coordinate basis.  The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ

---> [P.T3] Proton Temperature eigenvalues after diagonalization of tensor, calculated in the GSE coordinate basis.  The elements correspond to:  XX, YY, ZZ

[P.SYMM] Symmetry direction of proton pressure tensor, calculated in the GSE coordinate basis.  The elements correspond to:  XX, YY, ZZ and are defined by the largest eigenvalue in .T3

---> [P.SYMM_ANG] Angle between proton symmetry direction and the magnetic field vector

---> [P.SYMM_MAGT3] Proton temperature tensor... rotated into a field-aligned coordinate basis and then taking the diagonal elements only

[A.SC_CURRENT]  Current contribution to the spacecraft from thermal alphas

---> [A.MAGF] magnetic field vector interpolated (linearly) to the time of the PESA Low distribution, in GSE cartesian components

[A.PTENS] Alpha Pressure Tensor calculated in the GSE coordinate basis.  The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ

---> [A.MFTENS] Alpha Momentum Flux Tensor calculated in the GSE coordinate basis.  The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ

---> [A.T3] Alpha Temperature eigenvalues after diagonalization of tensor, calculated in the GSE coordinate basis.  The elements correspond to:  XX, YY, ZZ

[A.SYMM] Symmetry direction of alpha pressure tensor, calculated in the GSE coordinate basis.  The elements correspond to:  XX, YY, ZZ and are defined by the largest eigenvalue in .T3

---> [A.SYMM_ANG] Angle between alpha symmetry direction and magnetic field vector

---> [A.SYMM_MAGT3] Alpha temperature tensor... rotated into a field-aligned coordinate basis and then taking the diagonal elements only

 Ion moments (computed on-board) @ 3 second (spin) resolution, PESA LOW, Wind 3DP

Wind 3dp, PESA LOW 1 spin resolution ion (proton and alpha) moments (computed on spacecraft)

PESA (On-Board) Ion Moments @ Spin Resolution (version 3), Wind 3DP (from Master/CDFglobalAttributes/Data_type)

Proton number density [values fill-noisy 5/19/2009-5/11/2010; 3/8-5/15/2012] 

---> Residual Variance in Proton Velocity (6 components in instrument coords)

Alpha number density [values fill-noisy 5/19/2009-5/11/2010; 3/8-5/15/2012]

---> Residual Variance in Alpha Velocity (6 components in instrument coords)

Electron energy-angle distributions 27 keV to 520 keV, often at 24 sec, SST Foil, Wind 3DP

Wind 3dp, SST Foil energetic electron pitch angle distributions.General Notes per Lynn Wilson Jan 2015:  The solid-state telescope (SST) for Wind 3DP electrons returns a velocity distribution function containing 7 energy bins and 48 solid-angle bins.  The automated CDF routine appears to remove all the following solid-angle bins: [7,8,9,15,31,32,33] = sun/anti-sun look directions, and [20,21,22,23,44,45,46,47] = low geometry factor bins (also correspond to the SST Thick anti-coincidence detector bins).  The sun/anti-sun directions are removed to avoid X-ray and EUV contamination, which is often seen during solar flares.  The onset looks exactly like the GOES X-ray observations, which is kind of fun but not what we want to look at.  Unfortunately, these look directions can correspond to the magnetic field direction, which can limit the times when we would like to examine SEP events.General Notes per Lynn Wilson Jan 2015:   Note that SST Open (e.g., wi_sopd_3dp_00000000_v01.cdf) software removes the following additional solid-angle bins:  [0,1,24,25] = noisy.  Additionally, SST Open has 9 energy channels from ~70 keV to ~6.7 or 7.1 MeV, depending on the mode the instrument is in.  It does not appear that the routine mk_sosp_cdf.pro removes any of these ...bad... look directions, so that should be noted as well.General Notes per Lynn Wilson Jan 2015:  Inside the radiation belts, both Foil and Open saturate and suffer from penetrating particles.  The instruments are not shielded, so they can only provide relative changes when in these regions.General Notes per Lynn Wilson Jan 2015:  The data all look like they are in units of number flux or # cm-2 s-1 sr-1 eV-1.

SST Foil Energetic Electron Distributions (from Master/CDFglobalAttributes/Data_type)

Electron number flux 27 keV to 520 keV in 7 energy and 8 pitch angle bins (as energy-angle displays)

Electron number flux 27 keV to 520 keV as a stack_plot of 7 energies at the Bin1 angle (often ~15 deg)

Electron number flux 27 keV to 520 keV as a stack plot of 8 pitch angles at the Ch1 energy (often ~27 keV)

Electron omnidirectional fluxes 27 keV - 520 keV, often at 24 sec, SST Foil,  Wind 3DP

Wind 3dp, SST Foil energetic electron omni directional energy spectraGeneral Notes per Lynn Wilson Jan 2015:  The solid-state telescope (SST) for Wind 3DP electrons returns a velocity distribution function containing 7 energy bins and 48 solid-angle bins.  The automated CDF routine appears to remove all the following solid-angle bins: [7,8,9,15,31,32,33] = sun/anti-sun look directions, and [20,21,22,23,44,45,46,47] = low geometry factor bins (also correspond to the SST Thick anti-coincidence detector bins).  The sun/anti-sun directions are removed to avoid X-ray and EUV contamination, which is often seen during solar flares.  The onset looks exactly like the GOES X-ray observations, which is kind of fun but not what we want to look at.  Unfortunately, these look directions can correspond to the magnetic field direction, which can limit the times when we would like to examine SEP events.General Notes per Lynn Wilson Jan 2015:   Note that SST Open (e.g., wi_sopd_3dp_00000000_v01.cdf) software removes the following additional solid-angle bins:  [0,1,24,25] = noisy.  Additionally, SST Open has 9 energy channels from ~70 keV to ~6.7 or 7.1 MeV, depending on the mode the instrument is in.  It does not appear that the routine mk_sosp_cdf.pro removes any of these ...bad... look directions, so that should be noted as well.General Notes per Lynn Wilson Jan 2015:  Inside the radiation belts, both Foil and Open saturate and suffer from penetrating particles.  The instruments are not shielded, so they can only provide relative changes when in these regions.General Notes per Lynn Wilson Jan 2015:  The data below all look like they are in units of number flux or # cm-2 s-1 sr-1 eV-1.  I believe the CDAWeb  units are correct for most of these.

SST Foil Energetic Electron Omnidirectional Fluxes (from Master/CDFglobalAttributes/Data_type)

Electron number flux 27 keV - 520 keV as a function of energy in 7 channels (spectrogram)

Proton energy-angle distributions 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP

SST Open Proton Pitch Angle Distributions and Moments (from Master/CDFglobalAttributes/Data_type)

Proton number flux 70-6800 keV in 9 energy and 8 pitch angle bins (as energy-angle displays)

Proton number flux as a stack_plot of 9 energies at the Bin1 angle (often ~15 deg)

Proton number flux as a stack plot of 8 pitch angles at the Ch1 energy (often ~70 keV)

Proton omnidirectional fluxes 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP

Wind 3dp, SST Open energetic Proton omni directional energy spectraGeneral Notes per Lynn Wilson Jan 2015:  The solid-state telescope (SST) for Wind 3DP electrons returns a velocity distribution function containing 7 energy bins and 48 solid-angle bins.  The automated CDF routine appears to remove all the following solid-angle bins: [7,8,9,15,31,32,33] = sun/anti-sun look directions, and [20,21,22,23,44,45,46,47] = low geometry factor bins (also correspond to the SST Thick anti-coincidence detector bins).  The sun/anti-sun directions are removed to avoid X-ray and EUV contamination, which is often seen during solar flares.  The onset looks exactly like the GOES X-ray observations, which is kind of fun but not what we want to look at.  Unfortunately, these look directions can correspond to the magnetic field direction, which can limit the times when we would like to examine SEP events.General Notes per Lynn Wilson Jan 2015:   Note that SST Open (e.g., wi_sopd_3dp_00000000_v01.cdf) software removes the following additional solid-angle bins:  [0,1,24,25] = noisy.  Additionally, SST Open has 9 energy channels from ~70 keV to ~6.7 or 7.1 MeV, depending on the mode the instrument is in.  It does not appear that the routine mk_sosp_cdf.pro removes any of these ...bad... look directions, so that should be noted as well.General Notes per Lynn Wilson Jan 2015:  Inside the radiation belts, both Foil and Open saturate and suffer from penetrating particles.  The instruments are not shielded, so they can only provide relative changes when in these regions.General Notes per Lynn Wilson Jan 2015:  The data below all look like they are in units of number flux or # cm-2 s-1 sr-1 eV-1.  I believe the CDAWeb  units are correct for most of these.

SST Open Proton Omnidirectional Fluxes (from Master/CDFglobalAttributes/Data_type)

Proton number flux 70 keV - 6.8 MeV as a function of energy in 9 channels (spectrogram)

Wind Solar Wind Experiment (SWE) strahl detector, ~1/2 sec solar wind electron pitch-angle distributions at ~12 sec cadence

Explanatory notes:The 2D electron angular distributions included in this data set were measured by the Wind/SWE strahl detector (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995).Each angular distribution was measured at a single electron energy. The energy was selected by applying a voltage between the electrostatic analyzer plates. The detector sampled 32 energies between 19 eV and 1238 eV, and during normal operation would sweep through these energies one at a time with approximately 12 second cadence.The instrument's 12 anodes are set in a vertical pattern in a plane that contains the spacecraft spin axis, spanning a field of view +/-28 degrees centered around the ecliptic (with uneven angular spacing between anodes). Wind's spin axis is set at a right angle with the ecliptic plane, allowing different azimuthal angles to be sampled as the spacecraft spins (3 sec spin period). These azimuthal bins have a fixed separation of 3.53 degrees. Each strahl (and antistrahl) distribution measured by the spacecraft consists of a 14x12 angular grid of electron counts, that was measured at a fixed energy during a single spacecraft spin. Counts are converted into physical units of f (v) (e.g., cm^-6s^3) in the standard fashion by accounting for the detector efficiency and geometric factor.The data set reported here contains: f_strahl, f_antistrahl, f_strahl_counts, f_antistrahl_counts, phi_strahl, phi_antistrahl, theta, energy.

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/strahl0/1995/wi_strahl0_swe_19950101_v01.cdf. The most common cadence, 6397 [ms] = PT6.397S, occurred for 57.1966% of the 7451 timesteps. 

2D angular distributions measured by SWE strahl detector (from Master/CDFglobalAttributes/Data_type)

f_strahl intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs)

f_antistrahl intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs)

f_strahl_counts intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs)

f_antistrahl_counts intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs)

Phi (GSE) associated with unit vector pointing in electron velocity direction, for the strahl distribution.

Phi (GSE) associated with unit vector pointing in electron velocity direction, for the antistrahl distribution.

Theta (GSE) associated with unit vector pointing in electron velocity direction

energy (in eV) of the sampled electrons used to construct the f_strahl and f_antistrahl distributions

Wind Solar Wind Experiment, SWE: reduced charge flux distributions data release notes, version: 1.0. format: CDF 3.4.0. release Date: June 10, 2012

SPDF/CDAWeb. Please also acknowledge the data producer: Keith Ogilvie at NASA GSFC

SPDF/SSCWeb. Please also acknowledge the data producer: Keith Ogilvie at NASA GSFC

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: Keith Ogilvie at NASA GSFC

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/swe/swe_faraday/1994/wi_sw-ion-dist_swe-faraday_19941117_v01.cdf. The most common cadence, 74642 [ms] = PT1M14.642S, occurred for 61.0619% of the 138 timesteps. 

Solar Wind Experiment Faraday Cup (from all.xml/instrument/description/@short)

Solar Wind Plasma Reduced Ion Distribution Functions (from Master/CDFglobalAttributes/Data_type)

[CDAWEB PLOTS NOT SUPPORTED] The total charge flux (current) incident on the collector of cup 1, in picoAmperes (E/Q-azimuth display)

The total charge flux (current) incident on the collector of cup 1, in picoAmperes (E/Q-azimuth display) [data monotonically sorted based on dependencies]

---> Spectrograms by azimuth at sample E/Q [data monotonically sorted based on dependencies]

---> Spectrograms by E/Q at sample azimuths [data monotonically sorted based on dependencies]

[CDAWEB PLOTS NOT SUPPORTED] The total charge flux (current) incident on the collector of cup 2, in picoAmperes (E/Q-azimuth display)

The total charge flux (current) incident on the collector of cup 2, in picoAmperes (E/Q-azimuth display) [data monotonically sorted based on dependencies]

Azimuthal angle of the cup 1 normal. [data monotonically sorted]

---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 1 (in Volts).

---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 1 (in Volts). [data monotonically sorted]

---> Range of Energy-per-charge of admitted ions, i.e. the range of the bias potential of cup 1 (in Volts).

Azimuthal angle of the cup 2 normal. [data monotonically sorted]

---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 2 (in Volts).

---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 2veri (in Volts). [data monotonically sorted]

---> Range of Energy-per-charge of admitted ions, i.e. the range of the bias potential of cup 2 (in Volts).

This file contains goniopolarimetry analytical inversion dataset for Wind/Waves, assuming an unpolarized extended radio source (U=V=Q=0). Data are calibrated in W/m^2/Hz.

The authors must acknowledge the Plasma Physics Data Centre (CDPP) and Wind/WAVES teams for access to data.

Data are open access, with CC-BY 4.0 license. If usedin presentations or publications, cite the data collection with its DOI, and acknowledge Wind/Waves Investigation (K.Issautier and K. Goetz, PIs). Please read carefully the caveats attached to the data. We recommend the data users to contact the Wind/Waves team early in their study (Data inversion and limitation contacts: B. Cecconi and X.Bonnin). For reporting purposes, we request bibliography information for any publication, etc., using these data. Please send information on the use of this data to PIs: K.Issautier and K. Goetz. 

SPDF/CDAWeb. Please also acknowledge the data producer: K. Issautier at LESIA, Observatoire de Paris-PSL, CNRS

SPDF/SSCWeb. Please also acknowledge the data producer: K. Issautier at LESIA, Observatoire de Paris-PSL, CNRS

SPDF/CDAWeb and the HAPI project. Please also acknowledge the data producer: K. Issautier at LESIA, Observatoire de Paris-PSL, CNRS

Counts based on variable 'Epoch' in https://cdaweb.gsfc.nasa.gov/sp_phys/data/wind/waves/rad1_l3_df/1994/wi_wa_rad1_l3_df_19941110_v02.cdf. The most common cadence, 2862909436 [ns] = PT2.862909S, occurred for 49.8569% of the 3483 timesteps. 

Radio and Plasma Waves experiment, RAD1 receiver (from all.xml/instrument/description/@short)

Quality flag; 3=Good, 1=problems, 2=survey, 4=received special treatment