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ULYSSES JUPITER HISCALE W ION COUNTS

This data set consists of HISCALE W ion counts from the Ulysses Jupiter encounter 1991-Dec-31 to 1992-Feb-16. This includes 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 RPA PROC THERM ELEC, ION, PHOTOELEC, LOW RES. V1.0

The ORPA processed data consist of 4 file types: high resolution thermal electrons, high resolution superthermal electrons, high resolution ions, and a key parameters file at 12 second sampling.

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Velocity Distribution Functions (VDFs), Level 2 (L2), 3-minute Data in Solar Wind

The data include Wind STICS 3-minute 3D velocity distribution functions (VDFs) in three units (phase space density, differential number flux and counts), together with their statistical errors, for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the solar wind. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.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 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π 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.

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

This data set contains the total ion density obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions.

MMS 1 Hot Plasma Composition Analyzer (HPCA) Ions, Level 2 (L2), Burst Mode, 0.625 s Data

Hot Plasma Composition Analyzer (HPCA) Ions, Level 2, Burst Survey, 0.625 s Data. The MMS HPCA instruments measure the energy and composition of magnetospheric plasmas in the energy range from 1 eV to 40 keV. An electrostatic energy analyzer (ESA) that is optically coupled to a carbon-foil based Time-of-Flight (TOF) section comprises each HPCA. The basic HPCA data product is an array of counts for 5 ion species, at 63 energies, for each of 16 elevation anodes. Sixteen basic products, also called azimuths, are acquired every 0.625 s; half a spacecraft spin period nominally has 16 azimuths. The five ion species are protons (H+), alpha particles (He++), helium ions (He+), singly charged Oxygen (O+), and background counts.

MMS 1 Fast Plasma Investigation, Dual Ion Spectrometer (FPI, DIS) Distribution Moments, Level 2 (L2), Fast Mode, 4.5 s Data

The Fast Plasma Instrument (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 are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. 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 Results from integrating the standard Moments of Phase Space Distributions 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.

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Velocity Distribution Functions (VDFs), Level 2 (L2), 3-minute Data in Magnetosphere

The data include Wind STICS 3-minute 3D velocity distribution functions (VDFs) in three units (phase space density, differential number flux and counts), together with their statistical errors, for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the magnetosphere. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.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 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π 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.

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 19:39-21:58 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).

Interball Tail Wide-range 3D Ion Spectrometer (CORALL) Linearly Interpolated 60 s Resolution data in GSE Coordinates

Interball-1 Wide-range 3D Ion Spectrometer (CORALL) linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.

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.

MMS 3 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Ions, Level 2 (L2), Burst Mode, 0.3025 s Data

Fly's Eye Electron Proton Spectrometer (FEEPS) Burst Data. The Energetic Particle Detector (EPD) investigation aboard the four MMS spacecraft consists of two instrument designs, the FEEPS and the EIS (Energetic Ion Spectrometer). A FEEPS consists of six Heads, each composed of two Eyes. Each eye is a particle telescope with a single silicon detector. There are nine electron eyes and three ion eyes per FEEPS. The energy coverage is from 25 keV to 650 keV for electrons and 45 keV to 650 keV for ions. Each eye has sixteen energy channels, the spacing of which can be modified by command. The fields of view and pointing of each eye are designed to provide a broad, instantaneous field of view for the twelve eyes per FEEPS.

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.

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Moments, Level 2 (L2), 3-minute Data in Solar Wind

The data include Wind STICS 3-minute density (0th moment) and mean value of the energy distribution (1st moment), together with their statistical errors, for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the solar wind. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.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 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π 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.

PVO VENUS ION MASS SPECTROMETER CALIB HIGH RES ION DENS V1.0

The PV-OIMS high resolution dataset contains data from the Orbiter Ion Mass Spectrometer (OIMS) experiment and orbit attitude data for orbits 1-5055, including data for the period periapsis +/- 30 minutes for each orbit. The dataset is divided into multiple files which contain 1 orbit.

FAST Electrostatic Analyzer (ESA), Ion Burst 0.078 s Data

The FAST IES and EES measure 32 pitch angle directions simultaneously, 11.25° resolution, and sweep over 48 energy steps in 1/64 of a spacecraft spin. The energy range is nominally 3 eV to 25 keV for ions and 4 eV to 30 keV for electrons, respectively. Each spectrometer consists of two half sensor heads each with 180° by 10° field-of-view, FOV, that are mounted on opposite sides of the spacecraft to form a 360° planar FOV. The out-of-plane response is roughly Gaussian with a full width, half maximum, FWHM, of about 5°. The planar FOV is within the spacecraft spin plane, which is oriented with the spin vector normal to the nominal magnetic field direction. This orientation facilitates continuous pitch angle measurements. Deflectors are used to steer the sensor FOV out of this plane by up to 10° to account for variations of the magnetic field direction during the orbit. In general, the pitch angle distribution always includes both the parallel and Anti-parallel magnetic field directions. Burst data consists of a 32 angle by 48 anergy bin array of counts. Counts are pseudo-log compressed from 16 to 8 bits onboard. The first energy step is a high voltage retrace and should be ignored. Detector anodes rotate by half an anode or 5.625° each sweep. Survey data is averaged burst data that has been despun onboard. Slow survey is averaged into a 32 angle by 48 energy array each half spin or about 2.5 s. Some blurring of the angular resolution results from the half anode rotation on alternate sweeps. Fast survey is averaged into a 64 angle by 48 energy array that maintains the angular resolution. Fast survey time resolution varies from 1/16 to 1/4 of a spin.

TWINS 1 Images of Plasma Sheet Ion Temperature during Storms calculated from Energetic Neutral Atom (ENA) Measurements

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 were turned in May 2008; the Exact Launch Dates are not available. The Data, including both Science Data and Spacecraft Ephemeris and Attitude Information, from the two NASA-Funded Science Instruments are publicly available to the Scientific Research Community. See https://earth.esa.int/web/eoportal/satellite-missions/t/twins/. 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 from 1 keV ro 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°, 7.2 Re Apogee, 1000 km Perigee and Period 12 hr. The TWINS Spacecraft are 3-Axis stabilized and with Nadir-Pointing. Each acquires Image Data with Time Resolution of 60 s. The Time required to change Actuator Direction between Scans, an Interval with no Data Collection, was 25 s from June 2008 to July 2009, and 12 s at all other Times. This gives an Effective Cadence of 72 or 85 s. 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-alpha Detector consists of two independent Sensors to measure Lyman-alpha Radiation being emitted by Neutral Hydrogen Atoms. The Sensors oriented at Angles of 40° with respect to the Actuator Spin Axis. Each Sensor has a Full Width, Half Maximum, FWHM, Field-of-View of 4°, defined by Collimation Hole Baffles, uses Lyman-alpha Interference Filters as Narrow Band Transmissions Filters, and applies a KBr or CsI Photodiode for Photon Detection. The Lyman-alpha Detector is located on the rotating Actuator Platform to provide Full 360° Azimuthal Angle Coverage Time resolution is 60 s.

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).

STEREO-A Plasma and Suprathermal Ion Composition (PLASTIC) 2-hour Iron Plasma Parameters

This data product contains 2-hour averaged values of solar wind iron flow speed, density, thermal speed, iron to proton density ratio, and quality flags for each of these parameters. It also contains the iron charge state used in the V and Vth (1D Maxwellian) fitting algorithm

MMS 2 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Pulse Height by Time of Flight, Level 2 (L2), Survey Mode, 2.42 s Data

Energetic Particle Detector (EPD), Energetic Ion Spectrometer (EPD EIS) Pulse Height by Time of Flight, Level 2, Quick-Look Survey, 2.42 s Data. The EIS provides ion composition measurements (protons versus oxygen ions) and angular distributions over the energy range from approximately 45 to 500 keV.

MMS 2 Fast Plasma Investigation, Dual Ion Spectrometer (FPI, DIS) Instrument Distributions, Level 2 (L2), Fast Mode, 4.5 s Data

The Fast Plasma Instrument (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 are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. This Product contains Phase Space Distribution Maps of Results from surveying the High Resolution Observations during each 4.5 s Period. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Fast Survey Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.