A floppy was received at IHW-Lead Center through Dr. Oyama. It contained the following description: ***SUISEI ESP / Solar Wind Parameters *** T. Mukai Institute of Space and Astronautical Science Sagamihara, Kanagawa 229 Japan

The original dataset was called MST5SOW. It was personally delivered by Dr. Oyama. The sample hardcopy listed the column headings with units for the solar wind parameters bulk ion velocity, ion density, and ion temperature. The data format of the tape was included. The recorded jumps in the measured parameters indicate a disturbance at encounter. .

The file contains Level 1 3D electron distributions from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Ahead spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

The file contains Level 1 3D electron distributions from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Behind spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

These data were used to create Fig. 1 of “Monte Carlo Evaluation of the Europa Clipper TID Margin based on the Variability of the Jovian Radiation Environment with Application for Mission Design” by Allen Andersen, Wousik Kim, Steven McClure, and Insoo Jun of the Jet Propulsion Laboratory, California Institute of Technology. This data set contains Galileo Energetic Particle Detector (EPD) average counts per second measurements of 3.2-10.1 MeV protons (B0), 1.5-10.5 MeV electrons (B1), and >11 MeV electrons (DC3) between 8-10 Jovian Radii (Rj) only. Each entry has a corresponding time stamp and orbit name. Further details regarding these data can be found in Jun, I., Garrett, H. B., Swimm, R., Evans, R. W., and Clough, G. (2005), Statistics of the variations of the high-energy electron population between 7 and 28 jovian radii as measured by the Galileo spacecraft, Icarus, 178(2), 386-394. https://doi.org/10.1016/j.icarus.2005.01.022 The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

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 s Cadence. The 12 Anodes of the Instrument are set in a vertical Pattern in a Plane that contains the Spacecraft Spin Axis, spanning a Field of View +/-28° centered around the Ecliptic (with uneven Angular spacing between Anodes). The Wind Spacecraft Spin Axis is set at a Right Angle with the Ecliptic Plane, allowing different Azimuthal Angles to be sampled as the Spacecraft Spins (3 s Spin Period). These Azimuthal Bins have a Fixed Separation of 3.53°. Each Strahl (and Antistrahl) Distribution measured by the Spacecraft consists of a 14 ⨯ 12 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.

The file contains Level 1 3D electron distributions in burst mode from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Ahead spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

The file contains Level 1 3D electron distributions in burst mode from the In-situ Measurements of Particles and CME Transients, IMPACT, SWEA instrument on the STEREO Behind spacecraft. For important usage caveats see https://cdaweb.gsfc.nasa.gov/stereo_swea_caveats.html.

SWE is a comprehensive plasma instrument for the WIND spacecraft, see K.W.Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995. This product provides solar wind proton parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. Data reported within this product 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 were 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 through.