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New Horizons Solar Wind Around Pluto (SWAP) Proton Moments, Validated Summary Data (VS), 64 s Data

Solar Wind Plasma Moment Validated Summary (VS) Data from the New Horizons Solar Wind Around Pluto (SWAP) Instrument. References: Elliott, H.A., D.J. McComas, P. Valek, G. Nicolaou, S. Weidner, and G. Livadiotis, New Horizons Solar Wind Around Pluto (SWAP) Observations of the Solar Wind From 11-33 AU, ApJS, 223(2), 1-21, 2016, doi:10.3847/0067-0049/223/2/19.

Wind Magnetic Field Investigation (MFI) 15-sec magnetic field data, solar wind only

Data consist of 15-sec averages of magnetic field magnitude and GSE Cartesian components, from the MFI magnetometer on Wind. Data are for only the solar wind phases of the Wind orbit.

STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) 3-Dimensional Electron Distributions, Burst Mode, Level 1 (L1), 2 s Data

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.

ACE Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM) Plasma Moments, Level 2 (H2), 1 h Data

This Data Product contains Measurements from the ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM) Instrument. The Quality of the ACE Level 2 Data are 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. SWEPAM References: https://izw1.caltech.edu/ACE/

SOHO Charge, Element, and Isotope Analysis System (CELIAS) Proton Monitor (PM) 5-minute Solar Wind Data in CDF Format

The data include 5-minute proton speed, density, most probable thermal speed, and arrival direction, as well as predicted alpha-particle speed. Also included are the SOHO spacecraft predicted positon in GSE coordinates, Heliocentric Range, Heliographic Latitude and Longitude, and Earth Carrington Rotation Number. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. Description of the CELIAS-PM instrument and scientific scope can be found on the CELIAS instrument home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO mission home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.

Wind Definitive Orbit, 10 min Data, Spacecraft Position and Velocity in GCI, GSE, GSM, HEC, and HG Coordinates

Wind Definitive Orbit, Spacecraft Position and Velocity in Geocentric Celestial Inertial, GCI, Geocentric Solar Ecliptic, GSE, Geocentric Solar Magnetospheric, GSM, Heliospheric Ecliptic, HEC, and Heliographic, HG, Coordinates

Wind Predicted Attitude, 10 min Data, Spin Axis Orientation Angles in GCI, GSE and GSM Coordinates

Wind Predicted Attitude Body Spin Rate and Spin Axis Orientation Right Ascension and Declination Angles in Geocentric Celestial Inertial, GCI, Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSE, Coordinates

STEREO-A PLasma and Supra-Thermal Ion Composition (PLASTIC) He+ Pickup Ion (PUI) Solar Wind Frame Velocity Count Distributions and Proton Plasma Densities and Velocities, Level 3 (L3), 5 min Data

This data set presents STEREO-A PLASTIC PickUp Ion, PUI, He⁺ velocity distributions defined at a 5 min time resolution in the solar wind, SW, frame of reference. The velocity distributions are defined as a function of magnitude of the He⁺ PUI velocity vector divided by the solar wind speed in 69 velocity bins. This data set is not efficiency corrected, which has been shown to cause an increased relative count rate in the suprathermal tail region. Observations using this data set should be limited to the core PUI distribution. This data set is released in conjunction with the publication of Bower et al. (2019) to satisfy the American Geophysical Union, AGU, fair use data policy. Funding for this data release was provided by the SR&T Grant NNX16AF79G and the Heliophysics Grand Challenge 80NSSC17K000 at the University of New Hampshire and under DLR-Grant 50 OC 1103 at the Universität Kiel. CJF funded by NASA STEREO Quadrature grant. If these data are used in presentation or publications, we strongly suggest contacting J.S. Bower at jonathan.bower@unh.edu to ensure you are working with the latest release. For reporting purposes, we request bibliography information for any publication, etc., using these data. Please send information on the use of this data to the PLASTIC PI A.B. Galvin at toni.galvin@unh.edu. If you have questions regarding the data availability, please contact the PLASTIC Data System Manager Lorna Ellis at lorna.ellis@unh.edu.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPE Electron Pitch Angle Distribution, Level 3 (L3), 13.981 s Data

* SPAN-Electron, SPAN-E, Instrument SPE Level 3 Data* --------------------------------------------------File Naming Format: psp_swp_spe_sf0_l3_pad_YYYYMMDD_v01.cdfThis data product contains measurements of the Electron Pitch Angle Distribution from the SPAN-Electron 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.

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.

ACE Electron, Proton, and Alpha Monitor (EPAM) Solar Wind Plasma Energetic Particle Fluxes, Key Parameter (K0), 5 min 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/.

STEREO-A 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-A 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).

ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental Charge State Distributions with Statistical Uncertainties and Data Quality Flags, Level 2 (L2), 2 h Data

This ACE SWICS/SWIMS Data Set contains actual Charge State, Q, Distributions of Carbon, Oxygen, Neon, Magnesium, Silicon and Iron as opposed to the averaged Charge States that have been available on CDAWeb for some time. 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.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Electron Pitch Angle Distributions, Level 3 (L3), 13.981 s Data

* SPAN-Electron, SPAN-E, Instrument SPE Level 3 Data* --------------------------------------------------File Naming Format: psp_swp_spa_sf0_l3_pad_YYYYMMDD_v01.cdfThis data product contains measurements of the Electron Pitch Angle Distribution from the SPAN-A 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.

Wind Hot Plasma and Charged Particles (3DP) Electron Electrostatic Analyzer (EESA) Low, Omnidirectional Flux Spectra, 5 eV to 1100 eV, 24 s Data

Wind Three-Dimensional Particle, 3DP, instrument, Electron Electrostatic Analyzer, EESA, Low Energy Spectra, ELSP, omni directional electron differential number flux spectra, 3 eV to 30 keV.

STEREO-A In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) 3-Dimensional Electron Distributions, Burst Mode, Level 1 (L1), 2 s Data

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.

Wind Plasma and Radio Waves (WAVES) Electric Field Intensities and Electron Plasma Densities, Key Parameter (K0), 3 min Data

Wind Waves instrument, Plasma and Radio Wave Key Parameter data: electric field average intensity in dB above background at 76 log-spaced frequencies from 250 Hz to 9.4 MHz that is determined from neural network analysis of the in situ electron plasma frequency, Fpe, line.

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GALILEO PROBE DOPPLER WIND EXPERIMENT DATA V1.0

A total of seven data sets are used to derive the wind profile. These include two trajectory data files (probe and orbiter), three frequency data files including the 'quicklook' data set comprising 1/2 resolution frequency data from the orbiter CDS, and two data files containing the full tape recorder (SDR) data. Additionally, the probe descent trajectory data are supplemented with probe descent velocity/altitude/pressure/time data from the Atmospheric Structure Instrument. Finally, the Jovian atmospheric structure, based on measurements by the Atmospheric Structure Instrument, is included.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Alpha Particle Distribution Function, Partial Moments, Instrument Frame, Level 3 (L3), 14 s Data

SPI Level 3 Data----------------File Naming Format: psp_swp_spi_sf0a_l3_mom_inst_YYMMDDDD_v01.cdfThis data product contains measurements of partial moments of the alpha particle 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.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPC Ion Number Density, Velocity, and Thermal Speed Momemts and Fits, Level 3 (L3), 0.2185 s Data

SPC Level 3 Ion Data--------------------File Naming Format: psp_swp_spc_l3i_YYYYMMDD_v01.cdfThis data product contains derived measurements of ion properties in the solar wind, including those for density, temperature, and velocity. These are determined both by a direct computation of the velocity moments of the reduced distribution function and by attempting to fit the primary peak in the ion I(V) curve with a Maxwellian model. These measurements correspond one to one with spectra in the psp_swp_spc_l2i file for the same date. It may be convenient for some applications to cross-reference the two. For example, the corresponding l3i file contains ephemeris and data quality flag information that may be useful for an investigator who is concerned only with l2i type measurements.Conditions that impact measurement quality are documented in the DQF variable, which contains a 32 element flag array for each measurement time. Each element of the array is reserved to signify a specific condition. These conditions are described in the DQF_FLAGNAMES variable. In this version, for example, DQF_FLAGNAMES.DAT[23] is set to "spacecraft maneuver". If measurement "i" was made during a spacecraft maneuver, it is thus flagged with DQF.DAT[23,i] = 1.In Version 01, measurements are not provided, i.e. variables are set to fill, during spacecraft maneuvers, under conditions of low signal-to-noise, and during certain observed transients. Such conditions are rare during encounters, but increasingly frequent in interplanetary cruise. These conditions are documented in the DQF variable. Remarks are also provided in the "SPC Reduced Data Quality Periods" table. In Version 01, the solar wind alpha particle component is not measured. Thus, variables are set equal to fill values.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.