AndreaBozzo/ceres-open-data-index huggingface dataset:
STEREO-B PLasma and Supra-Thermal Ion Composition (PLASTIC) Beacon Data

PLASTIC - PLasma And SupraThermal Ion and Composition. The PLASTIC Experiment provides Plasma Characteristics of Protons, Alpha Particles and Heavy Ions. PLASTIC provides Key Diagnostic Measurements of Mass and Charge State Composition of Heavy Ions and distinguishes Coronal Mass Ejection, CME, Plasma from Ambient Coronal Plasma. STEREO Beacon Data are Real-Time Estimated Data processed for Operational Use only. PLASTIC Beacon Data have not been validated and should not be used for Publication Purposes. Do not cite. References: http://stereo.sr.unh.edu/stereo.html.

Tags: electricfield, energeticparticles, instrumentstatus, thermalplasma
Organization: National Aeronautics and Space Administration
MRO CRISM DERIVED DATA RECORD V1.0

This dataset is intended to include information on observation conditions, physical properties and coordinates of IR and VNIR data cubes from the CRISM instrument on MRO when the data cubes are pointed at Mars' surface. The information is mapped to the sensor space of non-map-projected data, EDRs and TRDRs.

Tags: __
Organization: National Aeronautics and Space Administration
ACE SWICS 2.0 Solar Wind Protons 12-min Data

The SWICS 12-minute proton data contains densities, speeds, and thermal speeds from the beginning of the mission up to the present day. The densities have been cross-calibrated to the proton monitors ACE/SWEPAM and WIND/SWE, and represent a continuous data set that can be used in conjunction with other SWICS data, or as a stand-alone measurement. For details on the SWICS proton data, see the release notes provided by the instrument team: http://www.srl.caltech.edu/ACE/ASC/DATA/level2/ssprotons/swics_protons_release_notes.txt

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
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), 1 h Data

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, Fe/O Abundance Ratio, 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.

Tags: energeticparticles, ioncomposition, thermalplasma
Organization: National Aeronautics and Space Administration
Apollo 15 Solar Wind Measurements at the Lunar Surface 28-s Data

This data set contains the highest time resolution plasma data available (28 sec per spectrum) from the solar wind experiment onboard Apollo 15. Contained in each record are: time, proton density, alpha-to-proton ratio, bulk speed, angle of flow, most probable thermal speed, and various housekeeping and fit parameters relating to the reliability of the calculated plasma parameters. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
THEMIS-A: On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field measurements, for particle and wave burst survey modes.

On Board Fast Fourier Transform (FFT) power spectra of Electric (EFI) and Magnetic (SCM) field measurements for particle and wave burst survey modes. Spectra are produced only in Particle Burst and Wave Burst modes; only a preselected four of the signals listed in Table 1 are input at any time. Data fed through the FFT while not in Particle or Wave Burst modes is automatically disgarded. The FFTs (Cooley-Tukey algorithm) are conducted as an integral part of the power spectrum calculation by the Field Programable Gate Arrays (FPGAs). A CORDIC algorithm is used for sine/cosine calculations. The data has raw resolution of 1024 pts for 8,192 sample/sec signals and 2048 pts for 16,384 sample/sec signals (EAC measurements only). Signals at 8,192 samples/sec are handled by 1024-point FFTs, while those at 16,384 samples/sec go through 2048-point FFTs. Past and current signal configurations for specific spacecraft are listed bellow in Table 2. The spectra are arranged into log spaced frequency bins in steps of 16, 32, or 64. Cadence is adjusted to keep packet size constant (i.e. increasing the fequency resolution by a factor of 2 decreases the sampling rate by 1/2). The frequency bins cover a range of 0 Hz to 4 kHz. Table 1: FFT Input Signals. Signal   Description SCMX, SCMY, SCMZ: Three axis magnetic fiend from SCM V1 through V6: Probe-spacecraft voltage for all six EFI sensors E12DC, E34DC, E56DC: DC-coupled electric field measured from opposing EFI sensors E12AC, E34AV, E56AC: AC-coupled electric field measured from opposing EFI sensors E12HF: High frequency electric field from EFI Table 2: Spacecraft specific configurations. All probes were initially set to use EDC34, EDC56, SCM2, and SCM3 signals for both particle and wave burst modes. Output was set to 16 frequency bins at 4 Hz. Configuration Changes: 9 June 2008: Particle burst spectra resolution increased from 16 to 64 bins and cadence slowed from 4 Hz to 1 Hz for closer analysis of spectral features. N/A: Particle burst spectra on all probes reconfigured to 64 bins at 1 Hz. 15 Aug 2008: E34DC and E56DC inputs switched to E34AC and E56AC to reduce impact of wake fields on FFT spectral measurements. 15 Oct 2008: Particle burst spectra resolution reduced from 64 to 32 bins and the rate increased from 1 Hz to 2 Hz; a response to noise from plasma wake fields in the 64 bin spectra. Table 3: Instrument-Spacecraft Physical Configuration Instrument   Alignment in Spacecraft Geometric coordinates (SPG). See THEMIS website for coordinate system details and mechanical drawings. EFI boom 1: Along positive X-axis EFI boom 2: Along negative X-axis EFI boom 3: Along positive Y-axis EFI boom 4: Along negative Y-axis EFI boom 5: Along positive Z-axis EFI boom 6: Along negative Z-axis SCM *The SCM uses an instrument specific set of axes; an orthogonal system centered instrument with the X-axis 12.1 degrees from the SPG X-axis.

Tags: spectrum
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT 1 OSIWAC 3 RDR MTP011 V2.0

This data set contains images acquired by the OSIRIS Wide Angle Camera during the COMET ESCORT 1 phase of the Rosetta mission at the comet 67P, covering the period from 2014-12-19T23:25:00.000 to 2015-01-13T23:24:59.000. This version V2.0 supersedes previous deliveries of the same dataset.

Tags: __
Organization: National Aeronautics and Space Administration
ACE Electron Proton Alpha Monitor (EPAM) LEMS30 MFSA, Spacecraft Frame, Sectored Proton Fluxes, 17 min Averages

17-min-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEMS30 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
CLAMS ER-2 Moderate Resolution Imaging Spectrometer (MODIS) Airborne Simulator (MAS)

CLAMS_ER2_MAS data were collected during the Chesapeake Lighthouse and Aircraft Measurements for Satellites (CLAMS) experiment with the objective to combine long term ocean spectral surface observations with satellite and aircraft measurements to enhance our knowledge of ocean surface reflections and aerosols.The MODIS Airborne Simulator (MAS) is an airborne scanning spectrometer that acquires high spatial resolution imagery of cloud and surface features from its vantage point on-board a NASA ER-2 high-altitude research aircraft. Data acquired by the MAS help to define, develop, and test algorithms for the Moderate Resolution Imaging Spectroradiometer (MODIS), a key sensor of NASA's Earth Observing System (EOS). The MODIS program emphasizes the use of remotely sensed data to monitor variation in environmental conditions for assessing both natural and human-induced global change.The MAS spectrometer acquires high spatial resolution imagery in the range of 0.55 to 14.3 microns. A total of 50 spectral bands are available in this range. Pre-1995 the digitizer was configured for each mission to record a pre-selected group of 12 bands during the flight. For most of these missions the digitizer was configured to record four 10-bit channels and seven 8-bit channels. A 50-channel digitizer which records all 50 spectral bands at 12 bit resolution became operational in January 1995.The MAS spectrometer is mated to a scanner sub-assembly which collects image data with an IFOV of 2.5 mrad, giving a ground resolution of 50 meters from 20000 meters altitude, and a cross track scan width of 85.92 degrees.

Tags: earth-science-atmospheric-radiation-atmosphere-longwave-radiation, earth-science-atmospheric-radiation-atmosphere-shortwave-radiation
Organization: National Aeronautics and Space Administration
THEMIS-D: On Board spin fits (FIT) of Electric (EFI) and Magnetic (FGM) field. On-Board Spin-fit electric and magnetic field data

THEMIS-D: On Board spin fits of Electric (EFI) and Magnetic (FGM) fields. This file contains data EFI and FGM that has been despun on-board to 3 second resolution. It stores meta information like the number of points that contributed to each spin and the standard deviation of those points. For the EFI data it also stores variables with the Z component of the EFI data zeroed and the Z component of the EFI estimated using the E.B=0 equality. The need to use an estimated Z axis for the EFI is due to error in measurements from the EFI axial booms. These data are provided in DSL (despun spacecraft L-Z vector), GSM, and GSE coordinates.

Tags: electricfield, magneticfield
Organization: National Aeronautics and Space Administration
Apollo 15 Solar Wind Measurements at the Lunar Surface 1-HR Data

This data set contains hourly averaged plasma parameters from the Apollo 15 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
Aureol 3 VLF Data

This data set contains power of electromagnetic wave components from \nnarrow band (10%) filters at 140, 450, 800, 4500, and 15000 Hz.  For \nany given time segment the power for any one of five predefined pairs \nof the five measurable field components (EZ, EH, BZ, BX, BX45) were \nmeasured and are included. The components of electromagnetic field \nare named by their direction in the satellite frame.\nSpacecraft position in geographic and \nmagnetic coordinates are also included, along with time and an \nindication of which pair of components were measured.\n  Each data file corresponds to one memory readout, and \ntypically consists of a few continuous-data segments.  The first \nseveral records in each file constitute a header giving the time spans \nof the segments, the time resolution, and other common information.  \nThe data records are in ASCII.

Tags: waves
Organization: National Aeronautics and Space Administration
ARTEMIS-P1 Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

Heliocentric trajectories for ARTEMIS-P1 in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinates The original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth. The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch", which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage: +---------------------------------------------------------------------+   Method Name   FPA Longitude Definition    ---------------------------------------------------------------------    B1950.0   the actual FPA at 22:09 UT on December 31, 1949     J2000.0   the smoothed FPA at 12:00 UT on January 1, 2000     True of Date   the actual FPA at 00:00 UT on the date of interest     Mean of Date   the smoothed FPA at 00:00 UT on the date of interest   +---------------------------------------------------------------------+ The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method. More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.

Tags: ephemeris
Organization: National Aeronautics and Space Administration
VOYAGER 1 SATURN PLASMA DERIVED ION                                      FITS BROWSE 96 SEC

THIS DATA SET CONTAINS ESTIMATES OF THE     ION MOMENT DENSITY IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) AT SATURN     DURING THE VOYAGER 1 ENCOUNTER.  RIGID COROTATION IS ASSUMED, WHICH LEADS     TO AN UNDERESTIMATE OF THE DENSITY IN SOME REGIONS, AS DOES THE USE OF     AN ACCEPTANCE AREA RELEVANT FOR A COLD BEAM FOR PLASMA WHICH IS TRANSONIC     IN SOME REGIONS.  DENSITIES MAY BE UNDERESTIMATED BY A FACTOR OF 2-3 IN     THE INNER MAGNETOSPHERE, SO THIS DATA SET SHOULD BE USED PRIMARILY FOR     STUDIES USING VARIATIONS IN PLASMA DENSITY.  THE FIT DENSITIES GIVE A     BETTER ESTIMATE OF THE ABSOLUTE DENSITY.  THIS IS THE DATA SHOWN AND     DESCRIBED IN DETAIL IN LAZARUS AND MCNUTT (1983).

Tags: __
Organization: National Aeronautics and Space Administration
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), Daily Data

This ACE SWICS/SWIMS Data Set contains the He/O, C/O, N/O, Ne/O, Mg/O, Si/O, S/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.

Tags: energeticparticles, ioncomposition, thermalplasma
Organization: National Aeronautics and Space Administration
THEMIS-D: ESA electron/ion energy fluxes and moments

THEMIS-D: Electrostatic Analyzers (ESA): Electron/Ion Ground-Calculated Energy Fluxes (5eV - 25 keV for Ions and 6eV - 30 KeV for Electrons) and Moments (density, velocity, pressure, and temperature). The satellite has 2 modes Fast and Slow survey and 3 data types: FULL, REDUCED and BURST. FULL: 88 angles x 32 energies, time resolution of 128 spins(395 seconds) in slow survey and 32 spins(98 seconds) in fast survey. REDUCED: spin time resolution(3 sec) but angles averaged into 1 angular spectra x 32 energies in slow survey or 6 angular spectra(90 degree x 90 degree window) x 32 energies in fast survey. BURST: 88 angles x 32 energies and spin time resolution(3 sec) but only available sporadically and for short duration. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. These moments are processed on the ground. They should be regarded as approximations but will improve in quality as our processing routines are improved over the course of the mission to account for additional sources of variance.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
ACE Electron Proton Alpha Monitor (EPAM) LEMS30 MFSA, Spacecraft Frame, Sectored Proton Fluxes, Hourly Averages

Hourly-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEMS30 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
Alouette 1 Topside Electron Density Profiles Manually Scaled at CRC

This data set, provided by the Communications Research Centre (CRC) in Ottawa, Canada, consists of electron density profiles derived from Alouette 1 Sweep-Frequency Sounder measurements for the ionosphere above the F2 maximum (topside ionosphere). The data set is in chronological order, and includes about 27,000 profiles obtained primarily during the period 1963 to 1967. The electron density profiles were computed from digital values of frequency and virtual height, which had in turn been scaled from the ionograms. Profiles were selected because of their scientific interest. Telemetry stations are not identified, but satellite location, time of observation, solar zenith angle at the satellite, magnetic dip at the satellite, total content down to the lowest altitude of topside ionospheric reflection, and other relevant information are listed for each profile. The format gives sequences of numbers for each point scaled from the ionogram. These sequences include electron density at the successive points, and the coefficients a2, b3, b4, b5, etc. from which geometric heights can be calculated, using formulas 40 and 41 in J. E. Jackson, "The reduction of topside ionograms to electron-density profiles," Proceedings of the IEEE., p. 960, June 1969. These formulas can also be used to calculate interpolated density-height values. A CRC interpolation program (available at NSSDC) can be used with this data set. These data make up a very small portion of the recorded Alouette 1 ionograms. Latitudinal coverage is widespread, but data at longitudes near 80 deg W are more numerous than others. The data were originally provided on 9-track, 1600-bpi, odd-parity, EBCDIC tape written on a MODCOMP-4 computer. NSSDC prepared an ASCII version using the Jackson formulas to compute electron density profiles.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT 3 OSIWAC 2 EDR MTP021 V1.0

This data set contains images acquired by the OSIRIS Wide Angle Camera during the COMET ESCORT 3 phase of the Rosetta mission at the comet 67P, covering the period from 2015-09-22T23:25:00.000 to 2015-10-20T23:24:59.000.

Tags: __
Organization: National Aeronautics and Space Administration