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DMSP F18 Special Sensor J, SESS/SSJ5, Precipitating Electrons and Ions Observed at 850 km, 1 s Data

Precipitating Electrons And ions observed at nominally 850 km Altitude and over a Range of Energies from 30 eV to 30 keV by 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.

ULYSSES JUPITER HISCALE COMPOSITION APERTURE ION COUNTS

This data set consists of HISCALE Composition Aperture (WARTD) ion counts. These measurements were taken during the Ulysses Jupiter encounter 1991-12-31 to 1992-02-16, and include 1 hour averaged inbound cruise data (1991-12-31 to 1992-02-01), and 15 minute averaged encounter data (1992-02-02 to 1992-02-16).

PVO VENUS ONMS BROWSE SUPRTHRML ION MAX COUNT RATE 12S V1.0

This data set contains PVO Neutral Mass Spectrometer superthermal ion data. Each record contains the maximum count rate per second in a 12 second period beginning with the time of the first data point for a given mass number.

STEREO-A Plasma and Suprathermal Ion Composition (PLASTIC) 1-min Proton Plasma Parameters

This data product contains 1-minute values of solar wind proton flow speed, density, and temperature and corresponding thermal speed. The records also hold flow velocity vector components and direction angles in HERTN and RTN coordinates. Chi-squared and statistical uncertainties are included, as are various flags. STEREO position information is given in radial distance and HEE, HEEQ and HCI direction angles.

ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, Daily Averages

Daily-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS60 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.

ACE Electron Proton Alpha Monitor (EPAM) LEMS30 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, Hourly Averages

Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEMS30 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.

THEMIS-C: ESA electron/ion energy fluxes and moments

THEMIS-C: Electrostatic Analyzers (ESA): Electron/Ion Ground-Calculated Energy Fluxes (5eV - 25 keV for Ions and 6eV - 30 KeV for Electrons) and Moments (density, velocity, pressure, and temperature). The satellite has 2 modes Fast and Slow survey and 3 data types: FULL, REDUCED and BURST. FULL: 88 angles x 32 energies, time resolution of 128 spins(395 seconds) in slow survey and 32 spins(98 seconds) in fast survey. REDUCED: spin time resolution(3 sec) but angles averaged into 1 angular spectra x 32 energies in slow survey or 6 angular spectra(90 degree x 90 degree window) x 32 energies in fast survey. BURST: 88 angles x 32 energies and spin time resolution(3 sec) but only available sporadically and for short duration. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. These moments are processed on the ground. They should be regarded as approximations but will improve in quality as our processing routines are improved over the course of the mission to account for additional sources of variance.

THEMIS-B: ESA electron/ion energy fluxes and moments

THEMIS-B: Electrostatic Analyzers (ESA): Electron/Ion Ground-Calculated Energy Fluxes (5eV - 25 keV for Ions and 6eV - 30 KeV for Electrons) and Moments (density, velocity, pressure, and temperature). The satellite has 2 modes Fast and Slow survey and 3 data types: FULL, REDUCED and BURST. FULL: 88 angles x 32 energies, time resolution of 128 spins(395 seconds) in slow survey and 32 spins(98 seconds) in fast survey. REDUCED: spin time resolution(3 sec) but angles averaged into 1 angular spectra x 32 energies in slow survey or 6 angular spectra(90 degree x 90 degree window) x 32 energies in fast survey. BURST: 88 angles x 32 energies and spin time resolution(3 sec) but only available sporadically and for short duration. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. These moments are processed on the ground. They should be regarded as approximations but will improve in quality as our processing routines are improved over the course of the mission to account for additional sources of variance.

VOYAGER 2 SATURN PLASMA DERIVED ION FITS 96 SEC

THIS DATA SET CONTAINS THE ION PARAMETERS IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) WITH FORMAL 1 SIGMA ERRORS OBTAINED FROM VOYAGER 2 DATA AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS TO OBTAIN PLASMA DENSITIES, TEMPERATURES, AND VELOCITY. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE NITROGEN OUTSIDE OF 14 RS AND OXYGEN ELSEWHERE. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. THE VALUES FOR POSITION AND MAGNETIC FIELD GIVEN IN THE DATA SET ARE ONLY APPROXIMATE AND SHOULD NOT BE USED FOR PUBLICATION. PARAMETERS WHICH ARE IDENTICALLY 0 AND HAVE UNCERTAINTIES OF 0 WERE NOT FIT DUE TO INSUFFICIENT DATA THESE NUMBERS ARE THUS NOT REAL VALUES. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: EACH DATA RECORD CONSISTS OF 5+2N LINES, WHERE N IS THE NUMBER OF IONS FIT. LINE 1: S (A1, INDICATES THE START OF A NEW FIT) TIME OF SPECTRUM SPACECRAFT LOCATION BRHO,BPHI,BZ(3F7.3) MONTHDAYYEAR(I7) ROUTINE USED INCORPORATING THE FULL RESPONSE FUNCTION OF THE INSTRUMENT FOR L MODES DATA): CHI-SQUARE FROM FIT (E7.3) (I2): LINES 2-5 TELL WHICH CHANNELS WERE FIT: CUP IDENTIFIER (A,B,C,D) (A1) AND ENDING CHANNEL OF EACH SET (2-20I3): LINE 6 FOR IONS: F (LINE IDENTIFIER) (A1) (I1)ION MASS, CHARGE (I3,I2) (6E10.3), WHERE THE X* VARIABLES ARE FORMAL 1 SIGMA UNCERTAINTIES: LINE 7 IDENTIFIER), ION SPECIES NUMBER (A1, I1) VZ,XVZ,WPAR,XWPAR,WPER, XWPER (6E10.3). LINES 6 AND 7 REPEAT ONCE FOR EACH ION SPECIES. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. V'S ARE VELOCITIES IN KM/S, W'S THERMAL SPEEDS IN KM/S, AND DEN'S DENSITIESIN CM-3. VALUES OF B AND POSITION INFORMATION MAY BE UNRELIABLE AND SHOULD BE VERIFIED BEFORE USE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

THEMIS-B: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV).

THEMIS-B: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Spacecraft Frame, Spin-Averaged Z>1 Ion Fluxes, 17 min Averages

17-min-averaged ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

VOYAGER 1 JUPITER PLASMA DERIVED ION MOMENTS 96 SEC

THIS DATA SET CONTAINS THE BEST ESTIMATES OF THE TOTAL ION DENSITY AT JUPITER DURING THE VOYAGER 1 ENCOUNTER IN THE PLS VOLTAGE RANGE (10-5950 EV/Q). IT IS CALCULATED USING THE METHOD OF MCNUTT ET AL. (1981) WHICH TO FIRST ORDER CONSISTS OF TAKING THE TOTAL MEASURED CURRENT AND DIVIDING BY THE COLLECTOR AREA AND PLASMA BULK VELOCITY. THIS METHOD IS ONLY ACCURATE FOR HIGH MACH NUMBER FLOWS DIRECTLY INTO THE DETECTOR, AND MAY RESULT IN UNDERESTIMATES OF THE TOTAL DENSITY OF A FACTOR OF 2 IN THE OUTER MAGNETOSPHERE. THUS ABSOLUTE DENSITIES SHOULD BE TREATED WITH CAUTION, BUT DENSITY VARIATIONS IN THE DATA SET CAN BE TRUSTED. THE LOW RESOLUTION MODE DENSITY IS USED BEFORE 1979 63 1300, AFTER THIS THE LARGER OF THE HIGH AND LOW RESOLUTION MODE DENSITIES IN A 96 SEC PERIOD IS USED SINCE THE L-MODE SPECTRA OFTEN ARE SATURATED. COROTATION IS ASSUMED INSIDE L=17.5, AND A CONSTANT VELOCITY COMPONENT OF 200 KM/S INTO THE D CUP IS USED OUTSIDE OF THIS. THESE ARE THE DENSITIES GIVEN IN THE MCNUTT ET AL. (1981) PAPER CORRECTED BY A FACTOR OF 1.209 (.9617) FOR DENSITIES OBTAINED FROM THE SIDE (MAIN) SENSOR. THIS CORRECTION IS DUE TO A BETTER CALCULATION OF THE EFFECTIVE AREA OF THE SENSORS. DATA FORMAT: COLUMNS 1-6 ARE TIME (YEAR, DAY, HOUR, MIN, SEC, MSEC) COLUMN 7 IS THE MOMENT DENSITY IN CM-3. EACH ROW HAS FORMAT (6I4, E12.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN MCNUTT ET AL. (1981) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Spacecraft Frame, Sectored Z>1 Ion Fluxes, Hourly Averages

Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

THEMIS-D: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV).

THEMIS-D: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

Voyager 2 Plasma Spectrometer (PLS) Faraday Cups A-D High Energy Resolution Current Ion Spectra, M Mode, for Proton Energies from 10 eV to 5950 eV, 96 s Data

These Ion Current Spectra in the Jovian Magnetosphere are from the Plasma Spectrometer (PLS) Instrument on Voyager 2 during July 1979 Flyby of Jupiter. The Instrument has four Faraday Cups A, B, C, and D, the Electron Data come only from Faraday Cup D. The Data are specified in Terms of Current per Faraday Cup in femto-amperes (10^-15 A equals 1 fA) versus Channel Number and Energy (eV). This Data Set is for the PLS M Mode covering Proton (H+ Ion) Energies from 10 eV to 5950 eV at High Energy Resolution in 128 logarithmic Energy Channels. The PLS Instrument 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, H.S., Belcher, J.W., Butler, R.J., Lazarus, A.J., Mavretic, A.M., Sullivan, J.D., Siscoe, G.L., and V.M. Vasyliunas, The Plasma Experiment on the 1977 Voyager Mission, Space Sci. Rev., 21, 259-287, 1977.

STEREO-A Plasma and Supra-Thermal Ion Composition (PLASTIC) He+ Daily Phase Space Densities

STEREO-A Plasma and Supra-Thermal Ion Composition, PLASTIC, He+ Phase Space Density, PSD, binned by V/Vsw, Level 3, Daily Resolution Data

ACE Electron Proton Alpha Monitor (EPAM) CA60 PHA Ion SEP Event Matrix Data, 17 min Averages

Pulse Height Analyzer matrix data for a single Solar Energetic Particle event from the ACE:EPAM instrument. Using the PHA data, one can quickly and very accurately determine composition.

GIOTTO ION MASS SPECTROMETER HIGH ENERGY RANGE DATA V1.0

A wide range of ion species and velocity distributions are expected to be found as the Giotto spacecraft traverses the coma of Halley's Comet. The outer coma is characterized by the interaction between solar wind and cometary plasmas, the inner coma by the outflow of cometary neutrals and their ionization products. The resultant demands on instrument dynamic range preclude use of a single sensor for measurements of ion composition. The Giotto Ion Mass Spectrometer (IMS) therefore consists of two sensors: one optimized for the outer and the other for the inner coma, with each obtaining complementary information in the region for which it is not optimized. Both sensors feature mass imaging characteristics, thereby permitting simultaneous measurements of several ion species by means of multi-detector arrays. The prime objective of the High-Energy Range Spectrometer (HERS) is to measure the ion abundances and three-dimensional velocity distributions outside the cometary contact surface.

VG2 URA PLS DERIVED RDR ION FIT 48SEC V1.0

This data set contains the ion densities and temperatures along with formal 1 Sigma errors obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions. Up to three isotropic proton components (warm, hot and intermediate) were used to match the observations. The plasma was assumed to be rigidly corotating. Uncertainties in plasma parameters are a factor of 2 in the charging region from 1939-2158 on day 24, less than 20% elsewhere. A complete description of this data set is given in McNutt et al. (1987) and Selesnick and McNutt (1987).

ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Spacecraft Frame, Sectored Z>1 Ion Fluxes, 17 min Averages

17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS60 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.