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. .

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

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

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.

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.

The data include Wind STICS 30-minute Angular Flux Maps (AFMs) 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. AFMs give the flow direction of the measured plasma divided into 48 velocity vector components ranging over sixteen azimuthal sectors and three elevation bins. AFMs are formed by integrating the VDFs over E/q. 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.

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.

WIND Solar Wind Experiment, SWE, Faraday cup data: this data set contains three-dimensional measurements of ions in the energy range 150 eV to 8 keV. Placed 15° above and below equatorial plane of the spacecraft, the Faraday Cups measure ion charge flux as a function of epoch, cup number, orientation angle, and bias grid potential. For each time point, a full spectrum is comprised of charge flux measurements at the two Faraday cup sensors at 20 azimuth angles for each of 31 energy-per-charge windows with 1240 data points per spectrum. Spectra are built up over approximately 92 s intervals. The effective area of the Faraday cup sensor as a function of incidence angle onto the cup is also provided.

Wind SWE Key Parameter data: proton density, thermal speed, flow velocity vectors, and spacecraft position vectors. Various versions differ slightly from each other. The version at MIT has flow velocity vectors experessed bby using Geocentric Solar Ecliptic, GSE, Cartesian and spherical representations and GSE Cartesian position vectors. The version available via nssdcftp and FTPBrowser has temperature instead of thermal speed and has no flow direction angles. The CDAWeb version has flow velocity and spacecraft position vectors in both GSE and Geocentric Solar Magnetospheric, GSM, coordinates, flow dynamic pressure, NmV^2, and velocity and density quality flags. The data were progressively despiked in passing from CDAWeb to MIT to nssdcftp/FTPBrowser.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 equal to 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 first bit, add 1, the second bit, add 2, the third bit, add 4, the fourth bit, add 8, and so on. See the table below.+------------------------------------------------------------------------------------------------------------------------------+| Bit | Set Value | MEANING ||------------------------------------------------------------------------------------------------------------------------------|| 1 | 1 | Three point parabolic fits to proton peaks were not attempted. || 2 | 2 | Non-linear least squares fit was not attempted. || 3 | 4 | Three point parabolic fits to proton peaks failed. || 4 | 8 | Non-linear least squares fit failed. || 5 | 16 | Alpha parameters not valid since 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 mode. Key parameters are produced in mode 1, science mode. || 8 | 128 | Three point fits done for cup 1 only. Split collector ratio of currents used to get the north/south angle. || | | Either cup 2 turned off, or cup 2 densities were low indicating noise associated with vibration. || 9 | 256 | Fewer than ten fc_blocks in spectrum. Analysis skipped. || 10 | 512 | Alpha particle non-linear fit produced values of density and thermal speed that do not seem reasonable. || 11 | 1024 | Three point parabolic fits to proton peaks done for cup 2 only. Probably Cup 1 is turned off. || | | The ratio of currents on split collectors used to get north/south angle. || 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. |+------------------------------------------------------------------------------------------------------------------------------+Particular flag settings:+-------------------------------------------------------------------------------------------+| Flag Value | Meaning ||-------------------------------------------------------------------------------------------|| 4098 | Tracking mode operation is full scan (4096) and No non-linear fits (2) || 14338 | Tracking mode operation is full scan (4096) and Limited tracking mode (8192) |+-------------------------------------------------------------------------------------------+Comments:* Note that in bit 4 of the quality flag the non-linear fit may be reported as good for protons and, at the same time, not good for alphas.* 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 are available in this data product,

The data include Wind STICS 30-minute Energy-Resolved Pitch-Angle Distributions (ERPAs) 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. ERPAs organize the data by the angle relative to the magnetic field vector direction, in 7.5 degree bins. The energy separation is preserved at the native resolution of the E/q bins. 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.