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ISEE-3 Linearly Interpolated 60 s Resolution Solar Wind Plasma data in GSE Coordinates

ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma 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.

VOYAGER 1 SOLAR WIND MAGNETIC FIELD HGCOORDS 48SEC AVG V1.0

This dataset contains Voyager 1 magnetometer data from the interplanetary cruise averaged to 48 second samples in Heliographic coordinates.

New Horizons Solar Wind Around Pluto (SWAP) Pick-Up Ions, Validated Summary Data (VS), Daily Data

Solar WInd Pick-Up Ion Plasma Moment Validated Summary (VS) Data from the New Horizons Solar Wind Around Pluto (SWAP) Instrument. Elliott, H.A., D.J. McComas, P. Valek, G. Nicolaou, S. Weidner, and G. Livadiotis (2016), ApJS, 223(2), 1-21, doi:10.3847/0067-0049/223/2/19. McComas, D.J., et al., (2008), The Solar Wind Around Pluto (SWAP) Instrument Aboard New Horizons, Space Sci Rev, 140(1), 261-313, doi:10.1007/s11214-007-9205-3.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Proton Differential Energy Flux for each Deflector Step, Energy, and Anode, Level 2 (L2), 7 s Data

SPI Level 2 Data----------------File Naming Format: psp_swp_spi_sf00_l2_8dx32ex8a_YYYYMMDD_v01.cdfThis data product contains measurements of differential proton energy flux at each measured deflector step, energy, and anode for the SPAN Ion instrument.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Full 3D Electron Spectra, Level 2 (L2), 14 s Data

SPAN-E Level 2 Electron Full 3D Spectra Data--------------------------------------------File Naming Format: psp_swp_spa_sf0_L2_16Ax8Dx32E_YYYYMMDD_v01.cdfThe SF0 products are the Full 3D Electron spectra from each individual SPAN-E instrument, SPAN-Ae and SPAN-B. Units are in differential energy flux, degrees, and eV. One spectrum comprises decreasing steps in Energy specified by the number in the filename, alternating sweeps in Theta/Deflection, also specified by the number in the filename, and a number of Phi/Anode directions, also specified by the number in the filename. The sample filename above includes 16 Anodes, 8 Deflections, and 32 Energies.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in "Full Sweep", normal cadence survey mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B during cruise phase periods when the spacecraft is pointed away from the sun are taken in sunlight.Parker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes--------------------------------------------------------------------------------November 19, 2019 Initial Data Release--------------------------------------Overview of Measurements------------------------The SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.The prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.Each SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.SPAN-E Level 2 Version 01 Release Notes---------------------------------------The SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of ±60° in Theta and 240° in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.The data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)General Remarks for Version 01 Data-----------------------------------Users interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.Due to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.The fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.The instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.A general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.Lastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is th

ROSETTA-ORBITER SOLAR WIND RPCIES 2 CR2 V1.0

This dataset contains EDITED RAW DATA of cruise 2 phase. Included are the data taken from 03 October 2005 to 7 March 2006.

VG1 SAT PLS DERIVED ION SOLAR WIND BROWSE 96SEC V1.0

This data set contains solar wind plasma browse data near the Voyager 1 Saturn encounter. Moment parameters are given. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second.

ISEE-3 Solar Wind Plasma Weimer Propagated 60 s Resolution in GSM Coordinates

ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. 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 References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

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Apollo 12 ALSEP ARCSAV Solar Wind Spectrometer Raw Cleaned ASCII Data Bundle

This bundle contains fixed-width ASCII files of daily, raw cleaned measurements acquired by the Solar Wind Spectrometer (SWS) at the Apollo 12 landing site for the time span of 03 April through 01 July 1975. These data were extracted from NASA's original Apollo Lunar Surface Experiments Package (ALSEP) archive tapes, also known as ARCSAV tapes.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Proton Distribution Function, Partial Moments, Instrument Frame, Level 3 (L3), 7 s Data

SPI Level 3 Data----------------File Naming Format: psp_swp_spi_sf00_l3_mom_inst_YYYYMMDD_v01.cdfThis data product contains measurements of partial moments of the proton distribution function in the instrument frame of reference. Users should be aware that the full ion distribution is typicaly not in the field of view, FOV, of the SPAN Ion instrument.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) 3-Dimensional Electron Distributions, Level 1 (L1), 30 s Data

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.

ACE Electron, Proton, and Alpha Monitor (EPAM) Solar Wind Plasma Energetic Particle Fluxes, Key Parameter (K1), 1 h Data

ACE Browse Data are designed for monitoring large-scale Particle and Field Behavior and for selecting interesting Time Periods. The Data are automatically generated from the Spacecraft Data Stream using simple Algorithms provided by the Instrument Teams. It is not routinely checked for Accuracy and is subject to Revision. Use this Data at your own Risk, and consult with the appropriate Instrument Teams about citing it. EPAM Browse Data are not validated by the Experimenters and should not be used except for Preliminary Examination prior to detailed Studies. ACE Electron, Proton, and Alpha Monitor (EPAM) References: http://www.srl.caltech.edu/ACE/.

ISEE-3 Solar Wind Plasma Weimer Propagated 60 s Resolution in GSE Coordinates

ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSE coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. 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 References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

VG2 SAT PLS DERIVED ION SOLAR WIND 96SEC V1.0

This Voyagers 2 data set contains two solar wind plasma data, one spanning from August 19 to September 4 , 1981, and near encounter specific data covering August 24-25. Moment parameters are given in the broader data while the near encounter data is more detailed. The fit parameters assume a convected isotropic proton Maxwellian distribution. Use of fit parameters is recommended as these are normally more accurate. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second.

STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) Pitch Angle Distribution, Level 2 (L2), 30 s Data in CDF format

STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) electron pitch angle distribution (PAD) in phase space density (in units of s^3/km^6) as a function of 12 pitch angle bins (centered at 7.5, 22.5, 37.5, 52.5, 67.5, 82.5, 97.5, 112.5, 127.5, 142.5, 157.5, 172.5 deg) and 10 variable energy bins (PAD values for energies < 50 eV are forced to fill values).

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPC Ion Charge Flux Distributions, Electrical Current versus Time and Energy-per-Charge, Level 2 (L2), 0.2185 s Data

SPC Level 2 Ion Data--------------------File Naming Format: psp_swp_spc_l2i_yyyymmdd_v01.cdfSolar Probe Cup, SPC, charge flux distributions comprise electrical current as a function of time and energy-per-charge, with appropriate instrument response elements considered and calibrations applied. This data product contains measurements of ion flux as a function of energy organized into spectra. The SPC instrument measures one-dimensional distributions with a wide field of view. Please refer to the instrument paper for details.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation.The MODE_FLAG variable contains information about the type of spectrum being measured. "Ion Full Scan" spectra are marked with MODE_FLAG.DAT = 1. These spectra comprise a broad energy range typically with lower signal-to-noise than the more frequent "Ion Peak Tracking" spectra, which are marked with MODE_FLAG.DAT equal to zero. In the most frequent operating mode, ion full scans are executed about once every 30 s or whenever the peak signal from the solar wind is poorly defined.SPC Encounter 1 Remarks-----------------------Data quality is very good for the duration of the encounter. The solar wind flow was within the optimal field of view for the SPC instrument for nearly the entire encounter. See the data flags for specific exceptions. As with all encounters, signal-to-noise is higher during ingress than egress, which is reflected in the typically smaller uncertainties and less frequent "primary peak low signal" flag events.SPC Cruise Phase Remarks------------------------Measurements recorded during cruise phase are not all transmitted to Earth. The typical return is one spectrum out of every 32.SPC Encounter 2 Remarks-----------------------Due to an erroneous setting in the operating mode for this encounter, ion full scan spectra and certain spectra immediately following ion full scans are of reduced quality. In the affected full scan spectra, the energy steps over an initial portion of the measurement spectra have zero width, i.e. the Level 2 ion variables MV_LO.DAT = MV_HI.DAT, and the corresponding measurements are purely noise. In some cases, this results in a poor determination of the proton "primary peak" energy, which renders additional subsequent full scans that follow subject to the same incompleteness. In other cases, the energy range for the subsequent "ion peak tracking mode" scan is not ideal. The affected Level 3 ion measurements have been flagged with DQF.DAT[22]=1, which stands for "energy ranging/peak tracking error" and/or set to fill. The operating mode has been revised such that future encounters will not be so affected.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

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

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.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Electron Energy Spectra, Level 2 (L2), 1.74 s Data

SPAN-E Level 2 ELectron Energy Spectra Data-------------------------------------------File Naming Format: psp_swp_spa_sf1_L2_32E_YYYYMMDD_v01.cdfThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.The larger Theta angles (deflection angles) are artificially enhanced in the "sf1" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.Parker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes--------------------------------------------------------------------------------November 19, 2019 Initial Data Release--------------------------------------Overview of Measurements------------------------The SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.The prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.Each SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.SPAN-E Level 2 Version 01 Release Notes---------------------------------------The SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of ±60° in Theta and 240° in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.The data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)General Remarks for Version 01 Data-----------------------------------Users interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.Due to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.The fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.The instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.A general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.Lastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.SPAN-E Encounter 1 Remarks--------------------------SPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an inst

OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 5 min Data

Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 5 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005

ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental and Isotopic Density, Speed, Thermal Speed, Charge State, and Ratio Parameters, Level 2 (L2), 2 h Data

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, He/O, C/O, Ne/O, Mg/O, Si/O, Fe/O Abundance Ratios, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. 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. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.