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THEMIS-C (P2/ARTEMIS-P2) Electron and Ion Moments (GMOM) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure and Temperature

THEMIS-C Electrostatic Analyzer (ESA) and Solid State Telescope (SST) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure, and Temperature. Generated from ESA and SST Combined Distributions. Data include Electron/Ion Ground-Calculated Fluxes and Spectrograms for Ions from 5 eV to 4 MeV and Electrons from 6 eV to 700 keV.

STEREO-A PLasma and Supra-Thermal Ion Composition (PLASTIC) He⁺ Counts and Relative Energy Flux in four Velocity Ranges normalized by the Solar Wind Speed, Level 3 (L3), Daily Data

STEREO-A Plasma and Suprathermal Ion Composition, Singly-charged Helium, He⁺, counts and relative differential energy fluxes binned by the ion speed relative to the solar wind bulk speed, four speed ratio bins. STEREO PLASTIC daily suprathermal He⁺ pickup ion signatures include He⁺ energy spectra, directional information, and contenxt information, such as the H⁺ plasma velocity. The four speed ratio, V/Vsw, bin ranges of are: 1.44 to 1.85, 1.85 to 2.50, 2.50 to 3.50, and 3.50 to 8.00. The identification of He⁺ is based on the measurement of energy per charge, E/q, time-of-flight, TOF, and total energy deposited in the solid state detector, SSD. These data include double coincidence measurements by using E/Qi and TOF and triple coincidence measurements by using E/Q, TOF, and SSD, see for example Galvin et al., Space Sci. Rev. 136, p 437-468, 2008. The proton bulk parameters including speed, Vsw, thermal velocity, Vth, and Density, Np, in this file are derived from a one-deminsional, 1-D, Maxwellian fit to a single detector rate with no coincidence required. These proton bulk parameters are corrected for background and dead time. The software version number used to derive the proton bulk parameters is shown in the file header and is described in the section on file formats. The most recent update of the proton bulk parameters can be found on the following STEREO website: http://stereo-ssc.nascom.nasa.gov/data/ins_data/plastic/level2/Protons/ For a full explanation, see the description at: https://stereo-ssc.nascom.nasa.gov/data/ins_data/plastic/level3/HePlus/HePlus_flux/READ_ME_PLASTIC_HePlus_Fluxes.pdf The singly-charged Helium, He⁺, flux data are also available from the STEREO Science Center in ASCII format via: https://stereo-ssc.nascom.nasa.gov/data/ins_data/plastic/level3/HePlus/ Note that this SPASE Numerical Description only describes the MESSENGER Magnetometer data stored in Common Data Files.

Voyager 1 Low-Energy Charged Particle (LECP) Background-Corrected Electron Differential Fluxes, Daily Data in CDF Format

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-- Electron fluxes and uncertainties (one st. dev.) in units: (cm^2 s sr MeV)^-1-- 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

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Proton Differential Energy Flux for each Deflector Step, Energy, and Anode, Level 2 (L2), 7 s Data

SPI Level 2 Data----------------File Naming Format: psp_swp_spi_sf00_l2_8dx32ex8a_YYYYMMDD_v01.cdfThis data product contains measurements of differential proton energy flux at each measured deflector step, energy, and anode for the SPAN Ion instrument.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPC Ion Charge Flux Distributions, Electrical Current versus Time and Energy-per-Charge, Level 2 (L2), 0.2185 s Data

SPC Level 2 Ion Data--------------------File Naming Format: psp_swp_spc_l2i_yyyymmdd_v01.cdfSolar 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 data product contains measurements of ion flux as a function of energy organized into spectra. The SPC instrument measures one-dimensional distributions with a wide field of view. Please refer to the instrument paper for details.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation.The MODE_FLAG variable contains information about the type of spectrum being measured. "Ion Full Scan" spectra are marked with MODE_FLAG.DAT = 1. These spectra comprise a broad energy range typically with lower signal-to-noise than the more frequent "Ion Peak Tracking" spectra, which are marked with MODE_FLAG.DAT equal to zero. In the most frequent operating mode, ion full scans are executed about once every 30 s or whenever the peak signal from the solar wind is poorly defined.SPC Encounter 1 Remarks-----------------------Data quality is very good for the duration of the encounter. The solar wind flow was within the optimal field of view for the SPC instrument for nearly the entire encounter. See the data flags for specific exceptions. As with all encounters, signal-to-noise is higher during ingress than egress, which is reflected in the typically smaller uncertainties and less frequent "primary peak low signal" flag events.SPC Cruise Phase Remarks------------------------Measurements recorded during cruise phase are not all transmitted to Earth. The typical return is one spectrum out of every 32.SPC Encounter 2 Remarks-----------------------Due to an erroneous setting in the operating mode for this encounter, ion full scan spectra and certain spectra immediately following ion full scans are of reduced quality. In the affected full scan spectra, the energy steps over an initial portion of the measurement spectra have zero width, i.e. the Level 2 ion variables MV_LO.DAT = MV_HI.DAT, and the corresponding measurements are purely noise. In some cases, this results in a poor determination of the proton "primary peak" energy, which renders additional subsequent full scans that follow subject to the same incompleteness. In other cases, the energy range for the subsequent "ion peak tracking mode" scan is not ideal. The affected Level 3 ion measurements have been flagged with DQF.DAT[22]=1, which stands for "energy ranging/peak tracking error" and/or set to fill. The operating mode has been revised such that future encounters will not be so affected.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

Voyager 2 Low-Energy Charged Particle (LECP) Background-Corrected Electron Differential Fluxes, Daily Data in CDF Format

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-- Electron fluxes and uncertainties (one st. dev.) in units: (cm^2 s sr MeV)^-1-- 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

STEREO-B IMPACT (In-Situ Measurements of Particles and CME Transients) Low Energy Telescope (LET) 1-min Level 1 Ion Fluxes

The IMPACT Low Energy Telescope (LET) data consist of 1-min resolution unsectored fluxes and counts for each of 15 single-Z ionic species at each of a species-dependent number of energy bins ranging between 9 and 16, plus 16-sectored fluxes and counts for 5 ionic species or Z groups in one (H) or two (He4, CNO, NiMgSi, Fe) energy ranges. There is much fill data. (

THEMIS-B (P1/ARTEMIS-P1) Electron and Ion Moments (GMOM) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure and Temperature

THEMIS-B Electrostatic Analyzer (ESA) and Solid State Telescope (SST) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure, and Temperature. Generated from ESA and SST Combined Distributions. Data include Electron/Ion Ground-Calculated Fluxes and Spectrograms for Ions from 5 eV to 4 MeV and Electrons from 6 eV to 700 keV.

THEMIS-A (P5) Electron and Ion Moments (GMOM) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure and Temperature

THEMIS-A Electrostatic Analyzer (ESA) and Solid State Telescope (SST) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure, and Temperature. Generated from ESA and SST Combined Distributions. Data include Electron/Ion Ground-Calculated Fluxes and Spectrograms for Ions from 5 eV to 4 MeV and Electrons from 6 eV to 700 keV.

STEREO-A IMPACT (In-Situ Measurements of Particles and CME Transients) Low Energy Telescope (LET) 1-min Level 1 Ion Fluxes

THEMIS-D (P3) Electron and Ion Moments (GMOM) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure and Temperature

THEMIS-D Electrostatic Analyzer (ESA) and Solid State Telescope (SST) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure, and Temperature. Generated from ESA and SST Combined Distributions. Data include Electron/Ion Ground-Calculated Fluxes and Spectrograms for Ions from 5 eV to 4 MeV and Electrons from 6 eV to 700 keV.

Voyager 1 Cosmic Ray Subsystem (CRS) Proton and Helium Energy Fluxes, Level H3 (H3), Daily Data

The joint California Institute of Technology, Caltech, Goddard Space Flight Center, GSFC, Cosmic Ray Subsystem, CRS, experiment on Voyager consists of three types of solid state detector telescopes: * Two High Energy Telescopes: HET-I and HET-II * Four Low Energy Telscopes (dE/dx versus E): LET A, LET B, LET C, and LET D * The Electron Telescope, TET The HETs and LETs are redundant and are designed to complement each other and to cover a broad range in energy, intensity, and charge spectra. The HETs covered an energy range between 6 MeV/n and 500 MeV/n for nuclei ranging in atomic numbers from 1 through 30. In addition, electrons in the energy range between 3 MeV and 100 MeV were measured by this telescope and an electron telescope. The LETs measured the energy and determined the identity of nuclei for energies between 0.15 MeV/n and 30 MeV/n and atomic numbers from 1 to 30. The instruments also measured the anisotropies of electrons and nuclei. The CRS looks only for very energetic particles in plasma, and has the highest sensitivity of the three particle detectors. Very energetic particles can often be found in the intense radiation fields surrounding some planets (like Jupiter). Particles with the highest-known energies come from other stars. The CRS looks for both. The CRS makes no attempt to slow or capture the super-energetic particles. They simply pass completely through the CRS. However, in passing through, the particles leave signs that they were there. Cosmic Ray Subsystem Science Objectives: * To measure the energy spectrum of electrons from 3 Mev to 110 MeV. * To measure the energy spectra and elemental composition of all cosmic ray nuclei from hydrogen through iron over an energy range from approximately 1 - 500MeV/nuc. * To provide information on the energy content, origin, acceleration process, life history, and dynamics of cosmic rays in the galaxy, and contribute to an understanding of the nucleosynthesis of elements in cosmic ray sources. * To provide information on the transport of cosmic rays, Jovian electrons, and low energy interplanetary particles over an extended region of interplanetary space. * To measure the three-dimensional streaming patterns of nuclei from Hydrogen through Iron and electrons over an extended range. * To measure particle charge compostion in the magnetosphere of Jupiter, Saturn, Uranus, and Neptune.

THEMIS-E (P4) Electron and Ion Moments (GMOM) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure and Temperature

THEMIS-E Electrostatic Analyzer (ESA) and Solid State Telescope (SST) Ground-Calculated Particle Energy Fluxes and Moments: Density, Velocity, Pressure, and Temperature. Generated from ESA and SST Combined Distributions. Data include Electron/Ion Ground-Calculated Fluxes and Spectrograms for Ions from 5 eV to 4 MeV and Electrons from 6 eV to 700 keV.

IBEX High Energy Neutral Atom Imager (ENA-Hi) Data Release-14, Compton Getting corrected, not Survival Probability corrected, Ram direction, West Ecliptic Global Distributed Flux and Flux Power Law Slope Maps, Level H3 (H3), three year average Data

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 the years from 2009 to 2018. This data set is derived from the Release 14 three-year IBEX-Hi map data with two-year overlaps of adjacent maps, 2009-2011, 2010-2012, and so forth through 2015-2017 from ram-direction fluxes with corrections for spacecraft motion, cg: Compton-Getting, but with no corrections, sp, for Energetic Neutral Atom, ENA, survival probability between 1 and 100 AU. The data set parameters include line-of-sight, LOS, integrated pressures computed separately from the Global Distributed Flux, GDF, the Ribbon Flux, and the Total Flux from summing GDF and Ribbon LOS pressures. Additionally there are signal to noise ratios for the GDF, Ribbon, and Total LOS pressures. Finally, there are power law slope values for the GDF differential flux and signal to noise ratios of the slope. 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. The data consist of ram-direction sky maps in Solar Ecliptic Longitude, east and west, and Latitude angles for the above parameters. 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 Observations, DOI: 10.3847/1538-4365/aae48e. The following codes are used to define data set types in the multiple IBEX data releases: +-----------------------------------------------------------------------------------------------------------------------------------------------------------------+ Code Code definition --------- ------------------------------------------------------------------------------------------------------------------------------------------------------- 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 approximately 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 +-----------------------------------------------------------------------------------------------------------------------------------------------------------------+ This particular data set denoted in the original ASCII files as: +------------------------------------------------------------------------------------------------------------------------------------------------------------+ Directory Name File Content Description +---------------- -------------------------------------------------------------------------------------------------------------------------------------------+ 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 +------------------------------------------------------------------------------------------------------------------------------------------------------------+

IBEX High Energy Neutral Atom Imager (ENA-Hi) Data Release-13, Compton Getting, no Survival Probability, Antiram direction, West Ecliptic Pressure and Flux Power Law Slope Maps, Level H3 (H3), annually averaged Data

The IBEX ENA-Hi data sets are from Release 13 of all-sky map data for the first ten years, 2009-2018, in the form of ram direction Hydrogen, H, energetic neutral atom fluxes with Compton-Getting corrections for spacecraft motion and with no corrections for ENA survival probability between 1 and 100 AU. All-sky maps have been compiled for the whole 1 yr time interval. 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 ENA-Hi and/or IBEX ENA-Lo data covering 2009-2018. The data consist of all-sky maps in Solar Ecliptic Longitude, east and west, and Latitude angles for Energetic Neutral Atom, ENA, Hydrogen fluxes from either IBEX ENA-Hi from energy band 2 through energy band 6, see the first table below, or from IBEX ENA-Lo from energy band 5 through energy band 8, see the second table below. Details of the data and enabled science from Release 13 are given in the following journal publications that describe the 1-yr data results and the IBEX-Hi and IBEX-Lo Instruments: McComas, D.J., et al. (2018), Heliosphere Responds to a Large Solar Wind Intensification: Decisive Observations from IBEX, Astrophys. J. Lett., 856(1), L10, (6 pp.), http://doi.org/10.3847/2041-8213/aab611 Funnsten, H.O., et al. (2009), The Interstellar Boundary Explorer High Energy (IBEX-Hi) Neutral Atom Imager, Space Sci. Rev., 146, 75-103, https://doi.org/10.1007/s11214-009-9504-y Fuselier, S.A., et al. (2009), The IBEX-Lo Sensor, Space Sci. Rev., 146, 117-147, https://doi.org/10.1007/s11214-009-9495-8 The IBEX ENA-Hi band/channel center energies and full width half maximum, FWHM, energy ranges are listed in a table below: +-----------------------------------------------------+ Energy Band Center Energy Energy Range ----------------------------------------------------- Channel 2 ~0.71 keV 0.52 keV to 0.95 keV Channel 3 ~1.11 keV 0.84 keV to 1.55 keV Channel 4 ~1.74 keV 1.36 keV to 2.50 keV Channel 5 ~2.73 keV 1.99 keV to 3.75 keV Channel 6 ~4.29 keV 3.13 keV to 6.00 keV +-----------------------------------------------------+ The IBEX ENA-Lo band/channel center energies are listed in a table below: +-----------------------------+ Energy Band Center Energy ----------------------------- Channel 1 0.015 keV Channel 2 0.029 keV Channel 3 0.055 keV Channel 4 0.110 keV Channel 5 0.209 keV Channel 6 0.439 keV Channel 7 0.872 keV Channel 8 1.821 keV +-----------------------------+ This particular IBEX-Hi CDF data product was constructed from the original ascii files named using the pattern hvset_noSP_antiram_cg_yearN for N=1,10, includes pixel map data from the antiram direction, with corrections, cg, for the Compton-Getting effect no corrections, nosp, for ENA survival probability between 1 AU and 100 AU, and a map compilation cadence equal to one year. In all, there are two IBEX ENA-Hi Release 13 CDF data products with one Compton-Getting correction setting, two survival probability settings, and one directional setting: ram. The table below defines how the file naming pattern is constructed for the two data products. Note that "ibex_h3_ena_hi_r13" is the file naming pattern root for these IBEX ENA-Hi CDF data products. The asterisk symbols in the last column of the table shows the line corresponding to this CDF data product within the expanded file naming pattern schema. +---------------------------------------------------------------------------------------------------+ C-G Corr. SP Corr. Dir. Acronym ENA Hi/Lo File Naming Pattern for 1 yr Skymaps --------------------------------------------------------------------------------------------------- cg nosp ram ENA Hi ibex_h3_ena_hi_r13_cg_nosp_ram_1yr cg nosp antiram ENA Hi ibex_h3_ena_hi_r13_cg_nosp_antiram_1yr *** +---------------------------------------------------------------------------------------------------+ The first column in the above table shows whether Compton-Getting, C-G, corrections have been applied to the data. C-G corrections account for how ENA measurements are affected by the the orientation of the IBEX spacecraft velocity vector relative to the arrival direction of the ENAs. * cg: Compton-Getting corrections applied * nocg: Compton-Getting corrections not applied The second column in the above table shows whether Survival Probability, SP, corrections have been applied to the data. SP corrections 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 approximately 100 AU. In the original data this mode is denoted as Tabular. * sp: Survival Probability corrections applied *

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ULY JUP COSPIN LOW ENERGY TELESCOPE 32 SEC PARTICLE FLUX

This data set contains COSPIN Low Energy Telescope (LET) particle flux rates from the Ulysses Jupiter encounter 1992-Jan-25 to 1992-Feb-16.

IMP 8 Goddard Medium Energy (GME) 30-min energetic particle rates and fluxes

This CDAWeb-accessible data set contains 30-minute, spin-averaged count rates and fluxes, and their statistical uncertainties, of energetic particles from the IMP8 GME experiment. Included are fluxes of: protons in 30 energy bins from 0.88-1.15 to 327-485 MeV; alpha particles in 21 energy bins from 1.14-1.36 to 63.3-81.0 MeV/n; and 0.3-18 MeV electrons. Also included are count rates for each of 7 sensors and for 11 multi-sensor coincidence modes. Proton and alpha particle fluxes, for every other energy bin, are given at the FTPBrowser and MSSP interfaces identified below.

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RENU2 Electron Plasma Detector (EPLAS) Precipitating Electron Total Energy Flux, (H0), 42 ms Data

RENU2 Electron Plasma Detector (EPLAS) Precipitating Electron Total Energy Flux