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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.

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VG2 NEP PLS DERIVED RDR ELECTRON MAGNETOSPHERE 96SEC V1.0

The electron spectra are fit using several isotropic Maxwellian distribution functions to find electron parameters. The spacecraft charge may seriously affect the density measurements. The temperature of each component is, however, independent of the spacecraft potential. To obtain the best estimate of the electron density, the encounter period is divided into four regions and four different analysis methods are used.

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GO JUPITER MAG MAGNETOSPHERIC SURVEY V1.0

This data set contains magnetic field vectors acquired by the Galileo Orbiter magnetometer during the magnetospheric survey portion of the mission. These data were acquired in the optimal averager (opt/avg) and real-time survey (RTS) modes beginning during the Jupiter approach and continuing throughout Jupiter orbital operations. The data set covers the time period from 1995-11-06T00:21:30 UT (Jupiter approach) until the end of mission (September 2003). Sampling rates are variable and depended upon the downlink capabilities. With few exceptions, the data are provided at the full downlink resolution. The data are provided in five coordinate systems (IRC, System III [1965], JSE, JSO, and JSM).

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VG2 NEP PLS DERIVED RDR ION MAGNETOSPHERE 48SEC V1.0

IBEX High Energy Neutral Atom Imager (ENA-Hi) Data Release-12, Magnetospheric Maps, Level H3 (H3), 24 min Data

This data set is from the IBEX-Hi Release 12 Count Data for Magnetospheric Imaging. This release provides data for various IBEX orbits from orbit 23 which started on 2009-03-26 to orbit 207b which ended on 2013-05-30. The data include 21 orbits from IBEX-Hi 6° histogram ENA count data, which is primarily what have been used in IBEX magnetospheric studies. 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 IBEX-Hi Count Data for Magnetospheric Imaging during instrument pointing in spin angle from 0° to 360° between the north and south Ecliptic poles. A spin angle equal to 0° corresponds to the north Ecliptic pole. Counts come from IBEX-Hi energy band 2 through 6: +-----------------------------------------------------+ 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 +-----------------------------------------------------+ Background counts have not been removed. Counts are separated into 6° latitudinal bins, with each angle label representing the center of the bin. Details of the data and enabled science from Release 12 are given in the following journal publications: McComas et al. 2011, 2012b; Fuselier et al. 2010, 2015; Petrinec et al. 2011; Ogasawara et al. 2013, 2019; and Dayeh et al. 2015. Data Location: http://ibex.swri.edu/ibexpublicdata/Data_Release_12/index.html. Contact: Maher Dayeh, Southwest Research Institute, San Antonio, TX, e-mail: maldayeh@swri.edu. +-----------------------------------------------------------+ Orbit Start Date/Time End Date/Time ----------------------------------------------------------- 23 2009-03-26T21:09:00.318 2009-04-03T16:07:51.743 24 2009-04-03T12:10:21.253 2009-04-11T08:15:09.669 25 2009-04-11T05:06:40.967 2009-04-18T22:05:11.125 27 2009-04-26T08:27:40.916 2009-05-04T05:31:06.519 28 2009-05-04T02:02:57.673 2009-05-11T21:13:47.596 29 2009-05-11T17:27:02.484 2009-05-19T19:27:18.831 51 2009-10-26T08:19:34.905 2009-11-03T02:38:01.730 52 2009-11-02T22:34:07.792 2009-11-10T19:03:55.230 53 2009-11-10T15:46:22.161 2009-11-18T10:58:17.674 55 2009-11-25T23:44:19.069 2009-12-03T11:26:37.151 56 2009-12-03T08:22:31.792 2009-12-10T22:03:52.604 57 2009-12-10T18:55:33.969 2009-12-18T06:58:47.247 72 2010-04-04T11:17:28.386 2010-04-12T09:13:51.008 74 2010-04-19T14:09:01.851 2010-04-27T03:44:14.913 77 2010-05-12T01:33:51.796 2010-05-19T20:43:01.583 78 2010-05-19T17:33:48.047 2010-05-27T13:02:03.396 103 2010-11-26T07:56:05.324 2010-12-04T04:11:44.879 187a 2012-11-21T00:17:13.430 2012-11-25T00:40:26.707 188b 2012-12-03T12:46:18.859 2012-12-08T00:44:50.846 206a 2013-05-13T23:15:27.433 2013-05-17T12:19:58.215 207b 2013-05-26T12:21:08.868 2013-05-30T23:14:44.989 +-----------------------------------------------------------+ For the first two and a half years of science operations, which corresponds to from Orbit 1 through Orbit 127), the IBEX orbital period was approximately 7.5 days and the spin axis was repointed once each orbit around perigee, leading to bands of sky viewing centered 7.5° apart. In June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously unknown, long-term stable lunar synchronous orbit with apogee still close to 50 Earth radii (McComas et al. 2011a). Since then, the IBEX orbital period has been approximately 9.1 days, which is one third of the lunar sidereal period of 27.3 days. Orbit numbers from 130 onward are split into two segments, 'a' and 'b'. Furthermore, starting in orbit segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and eliminated the lowest energy step, ESA1, in exchange for doubling the statistical sampling of ESA3, center energy ~1.1 keV.

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ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSM, Coordinates, Level 2 (H2), 1 h Data

This Data Product contains Measurements from the ACE Magnetic Field Instrument (MAG). The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. MAG References: http://www.srl.caltech.edu/ACE/.

TWINS 1, TWINS 2 Storm Time Equatorial Magnetospheric Ion Temperatures derived from Energetic Neutral Fluxes (ENA), Modified Data 2 (MD2), 10 min Data

Two Wide-angle Imaging Neutral-atom Spectrometers, TWINS, energetic neutral atom, ENA, derived equatorial magnetospheric ion temperatures, see Katus et al. (2017)

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Energy-Resolved Pitch-Angle Distributions (ERPAs), Level 2 (L2), 30-minute Data in Magnetosphere

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 magnetosphere. 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.

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ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSM, Coordinates, Level 2 (H1), 4 min Data

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Angular Flux Maps (AFMs), Level 2 (L2), 30-minute Data in Magnetosphere

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 magnetosphere. 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.

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

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 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.

restrictednotspecifiedAug 2025View details →

ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSM, Coordinates, Level 2 (H3), 1 s Data

LANL1997 Magnetospheric Plasma Analyzer (MPA) at 87 sec Resolution in Spacecraft Coordinates

The LANL 1997-97A MPA data set contains various parameters in a variety of coordinates systems including GEI, spacecraft, polar geographic, and polar magnetic coordinates at about 87 s resolution. These parameters include universal time, denisty, velocity, and temperature for both low and high energy ions and electrons as well as position information and instrument status flags.

VG2 NEP PLS DERIVED RDR ION MAGNETOSPHERE 48SEC V1.0

This data set gives the best available values for ion densities, temperatures, and velocities near Neptune derived from data obtained by the Voyager 2 plasma experiment. All parameters are obtained by fitting the observed spectra (current as a function of energy) with Maxwellian plasma distributions, using a non-linear least squares fitting routine to find the plasma parameters which, when coupled with the full instrument response, best simulate the data. The PLS instrument measures energy/charge, so composition is not uniquely determined but can be deduced in some cases by the separation of the observed current peaks in energy (assuming the plasma is co-moving). In the upstream solar wind protons are fit to the M-long data since high energy resolution is needed to obtain accurate plasma parameters. In the magnetosheath the ion flux so low that several L-long spectra (3-5) had to be averaged to increase the signal-to-noise ratio to a level at which the data could be reliably fit. These averaged spectra were fit using 2 proton maxwellians with the same velocity. The values given in the upstream magnetosheath are the total density and the density-weighted temperature. In both the upstream solar wind and magnetosheath full vector velocities, densities and temperatures are derived for each fit component. In the magnetosphere spectra do not contain enough information to obtain full velocity vectors, so flow is assumed to be purely azimuthal. In some cases the azimuthal velocity is a fit parameter, in some cases rigid corotation is assumed. In the 'outer' magnetosphere (L>5) two distinct current peaks appear in the spectra H+ and N+. In the inner magnetosphere the plasma is hot and the composition is ambiguous, although two superimposed Maxwellians are still required to fit the data. These spectra are fit using two compositions, one with H+ and N+ and the second with two H+ components. The N+ composition is preferred by the data provider. All fit values in the magnetosphere come with one sigma errors. It should be noted that no attempt has been made to account for the spacecraft potential, which is probably about -10 V in this region and will effect the density and velocity values. In the outbound magnetosheath and solar wind both moment and fit values are given for velocity, density, and thermal speed. The signal-to-noise ratio in the M-longs is very low, especially near the magnetopause, which can result in the analysis giving incorrect values. The L-long spectra have too low an energy resolution to permit accurate determinations parameters in many regions temperature and non-radial velocity components may be inaccurate.

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VG2 NEP PLS DERIVED RDR ELECTRON MAGNETOSPHERE 96SEC V1.0

LANL 2002 Magnetospheric Plasma Analyzer (MPA) at 87 sec Resolution in Spacecraft Coordinates

The LANL 02A MPA data set contains numerical moments computed from measurements of the Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., Rev. Sci. Inst., in press 1993]. The moments are presented in s/c coordinates: the z-axis is aligned with the spin axis, which points radially toward the center of the Earth; the x-axis is in the plane containing the spacecraft spin axis and the spin axis of the Earth, with +X generally northward; and the y-axis points generally eastward. Polar angles are measured relative to the spin axis (+Z), and azimuthal angles are measured around the z-axis, with zero along the +X direction. The moments are computed for three 'species': lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 21.5 secs after the ion measurements. Epoch is the measurement time appropriate for the ions. The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined. Tperp and Tpara are obtained from diagonalization of the 3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by non-zero 'SCALEMIN' values in this file. A quality flag value of 1 indicates that the values are suspect because of unreliable location info.

LANL 1989 Magnetospheric Plasma Analyzer (MPA) at 87 sec Resolution in Spacecraft Coordinates

The LANL 1989-046 MPA data set contains various parameters in a variety of coordinates systems including GEI, spacecraft, polar geographic, and polar magnetic coordinates at about 87 s resolution. These parameters include universal time, denisty, velocity, and temperature for both low and high energy ions and electrons as well as position information and instrument status flags.

LANL1991 Magnetospheric Plasma Analyzer (MPA) at 87 sec Resolution in Spacecraft Coordinates

The LANL 1991-080 MPA data set contains various parameters in a variety of coordinates systems including GEI, spacecraft, polar geographic, and polar magnetic coordinates at about 87 s resolution. These parameters include universal time, denisty, velocity, and temperature for both low and high energy ions and electrons as well as position information and instrument status flags.

LANL1990 Magnetospheric Plasma Analyzer (MPA) at 87 sec Resolution in Spacecraft Coordinates

The LANL 1990-095 MPA data set contains various parameters in a variety of coordinates systems including GEI, spacecraft, polar geographic, and polar magnetic coordinates at about 87 s resolution. These parameters include universal time, denisty, velocity, and temperature for both low and high energy ions and electrons as well as position information and instrument status flags.