AndreaBozzo/ceres-open-data-index huggingface dataset:
ROSETTA-ORBITER 67P RPCICA 4 EXT3 CORR-CTS V1.0

This dataset contains corrected and RESAMPLED RAW DATA from theRPCICA instrument on mission ROSETTA during Rosetta extension 3.The data has been corrected for cross-talk using an automatic algorithm,and noise has been treated to be even regardless of onward noisesuppression. The data is the same as L4 CORR but in counts, not physicalunits. The data may due to noise treatment have negative values.Data contains measurements of solar wind interactionwith the atmosphere of target comet 67P.

Tags: __
Organization: National Aeronautics and Space Administration
MMS 1 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Ions, Level 2 (L2), Burst Mode, 0.3025 s Data

Fly's Eye Electron Proton Spectrometer (FEEPS) Burst Data. The Energetic Particle Detector (EPD) investigation aboard the four MMS spacecraft consists of two instrument designs, the FEEPS and the EIS (Energetic Ion Spectrometer). A FEEPS consists of six Heads, each composed of two Eyes. Each eye is a particle telescope with a single silicon detector. There are nine electron eyes and three ion eyes per FEEPS. The energy coverage is from 25 keV to 650 keV for electrons and 45 keV to 650 keV for ions. Each eye has sixteen energy channels, the spacing of which can be modified by command. The fields of view and pointing of each eye are designed to provide a broad, instantaneous field of view for the twelve eyes per FEEPS.

Tags: energeticparticles, magneticfield
Organization: National Aeronautics and Space Administration
Mars Global Surveyor Solar Wind Proxy Pressures

Derivation of the solar wind dynamic pressure at Mars using Mars Global Surveyor data. There is no upstream solar wind monitor at Mars (as of the release of this data set). This data set is a proxy for the solar wind dynamic pressure derived from Mars Global Surveyor (MGS) Magnetometer (MAG) measurements. The rationale behind the proxy is that pressure is conserved in the solar wind interaction with Mars. At altitudes from ~400-800 km, the dominant pressure term is magnetic field pressure. We measure the magnetic field with MAG, calculate the pressure (B2/2µo) in that altitude range and assume that it balances the incident solar wind pressure. This proxy is reliable for determining relative solar wind pressure at Mars. Absolute values may deviate from the proxy. The pressure does drop with solar zenith angle (SZA). This affect is accounted for by fitting a function of SZA to the dayside, northern hemisphere data from an MGS pass. The number of points included in the fit is provided in the file. The standard deviation from the fit is also provided. Because we do a fit to one orbit's worth of dayside, northern hemisphere data, we obtain one value for PSW every orbit, which has a period of ~2 hr.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
MARS EXPRESS SUN MRS 1/2/3                                     EXTENDED MISSION 8 4363 V1.0

This is a Mars Express                                     Radio Science data set, collected                                     during the extended mission phase                                     2023-01-01 to 2023-12-31.                                     It is a Solar Conjunction                                     measurement and covers the time                                     2023-11-05T08:00:43.000 to                                     2023-11-05T10:07:33.100.

Tags: __
Organization: National Aeronautics and Space Administration
MMS 1 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Ions, Level 2 (L2), Survey Mode, 2.42 s Data

Fly's Eye Electron Proton Spectrometer (FEEPS) Survey Data. The Energetic Particle Detector (EPD) investigation aboard the four MMS spacecraft consists of two instrument designs, the FEEPS and the EIS (Energetic Ion Spectrometer). A FEEPS consists of six Heads, each composed of two Eyes. Each eye is a particle telescope with a single silicon detector. There are nine electron eyes and three ion eyes per FEEPS. The energy coverage is from 25 keV to 650 keV for electrons and 45 keV to 650 keV for ions. Each eye has sixteen energy channels, the spacing of which can be modified by command. The fields of view and pointing of each eye are designed to provide a broad, instantaneous field of view for the twelve eyes per FEEPS.

Tags: energeticparticles, magneticfield
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 4 PRL-MTP001 RDR-INF-REFL V1.0

This CODMAC level 4 data set contains solar stray-light corrected, in-field stray-light corrected,  radiometric calibrated and geometric distortion corrected  (resampled) image data in reflectance units (normalized  and thus without unit),  acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft  during the PRELANDING mission phase, covering the period  from 2014-01-20T10:00:00.000 to 2014-05-07T12:47:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V1.0 is the first version of this dataset: Lien corrected dataset after September 2019 PSA/PDS external peer review.

Tags: __
Organization: National Aeronautics and Space Administration
MMS 1 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Instrument Distributions, Level 2 (L2), Fast Mode, 4.5 s Data

The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. This Product contains Phase Space Distribution Maps of Results from surveying the High Resolution Observations during each 4.5 s Period. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Fast Survey Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
ICON Extreme Ultraviolet Spectrograph Images

This describes the data produce for ICON EUV Daytime O+ (DP 2.6), which is in NetCDF4 format. These files are named ICON_L2-6_EUV_YYYY-MM-DD_vXXrZZ.NC, where YYYY-MM-DD is the year month day and VXX shows the version number and rZZ shows the revision number of this file.  Each individual file nominally contains 1 day (24 hours) of data. The L2 EUV Daytime files are produced from the L1 EUV files, and their primary data product is the O+ profile derived from a retrieval that is detailed in a paper: https://doi.org/10.1007/s11214-017-0385-1. In addition, many other parameters and geophysical data products are included in the file.  The data are identified in one of 3 var_types: data – which contains the primary data product; support data – which contains parameters used in the retrieval such as geometry etc. that may also be useful in any analysis of this data; and ignore_data – which are recorded for debugging purposes and should not be used for publication without detailed discussion with the ICON team. The dimensions of the data also indicate its type.  For example, anything with epoch as a dimension means there is 1 value corresponding to each instrument exposure. Anything with dimension Input_data corresponds to the input data, passed from Level 1.  Anything with a dimension of model refers to the forward model parameters used as part of the inversion. Anything with dimension altitude corresponds to the altitude grid used for the inverted parameters.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
GPS Deduced ROTI Index, Standard Deviation of the Rate of Change of the Total Electron Content (TEC), World Maps and Movies, 15 min Data

The ROTI Index is the Standard Deviation of the Rate of Change of the Total Electron Content, TEC, during a 15 min Interval. The TEC Values are measured between a Global Positioning Satellite, GPS, and Ground Receiver Station.

Tags: activityindex
Organization: National Aeronautics and Space Administration
Mars Science Laboratory Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

Heliocentric trajectories for Mars Science Laboratory 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
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction B

The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength.  The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.

Tags: dopplergram
Organization: National Aeronautics and Space Administration
MAVEN Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

Heliocentric trajectories for MAVEN 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
MAVEN SWIA Calibrated Fine Survey 3D Data Collection

SWIA fine survey 3d files with time-ordered fully calibrated ion distributions in units of differential energy flux derived from the SWIA Fine distribution Survey telemetry, as well as a header of ancillary information needed to interpret the data. Description of the SWIA instrument can be found on the SWIA home page https://lasp.colorado.edu/maven/science/instrument-package/swia/ and in the SWIA instrument publication https://doi.org/10.1007/s11214-013-0029-z.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
MMS 1 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Distribution Moments, Level 2 (L2), Fast Mode, 4.5 s Data

The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually Operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Results from integrating the standard Moments of Phase Space Distributions formed from the indicated Data Type (DES/DIS Burst, FS or SS). For Convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

Tags: energeticparticles, spectrum, thermalplasma
Organization: National Aeronautics and Space Administration
MMS 1 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 2004 model, Dynamic conditions), Level 2 (L2), Burst Mode, 30 ms Data

Magnetospheric Multiscale 1 (MMS 1) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 2004 magnetic field model for disturbed magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.

Tags: activityindex, ephemeris, magneticfield
Organization: National Aeronautics and Space Administration
GO JUPITER PWS EDITED EDR 10KHZ WAVEFORM RECEIVER V1.0

This data set includes wideband waveform measurements from the      Galileo plasma wave receiver obtained during Jupiter orbital      operations. These data were obtained during selected observation      periods near perijove, satellite encounters and other select times.      These measurements are electric waveforms obtained by rapidly      sampling the potential at the input to the receiver from the      electric dipole antenna.  The sample rates are 201,600/s, 25,200/s,      or 3,150/s taken through bandpass filters of 80, 10, or 1 kHz,      respectively.

Tags: __
Organization: National Aeronautics and Space Administration
IMAGE Radio Plasma Imager (RPI) Plasmagram Full Resolution Binary Data

RPI plasmagram full resolution data (received signal strength in the frequency-range frame), uncalibrated. Presented as instrument packets wrapped in the standard CCSDS headers. Description of the RPI instrument-level data model can be found at http://ulcar.uml.edu/RPI/RPITelemetryDataFormat_V2.8.pdf. Data are viewed/calibrated/edited by BinBrowser software, see http://ulcar.uml.edu/rpi.html for download and users' guide. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the radar pulses. Echoes from important magnetospheric structures, such as the magnetopause and the plasmapause, appear as traces on plasmagrams. Plasmagram traces are intermixed with vertical signatures corresponding to the locally excited plasma resonances and various natural emissions propagating in space.

Tags: waves-active
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 4 EXT2-MTP028 RDR V1.0

This CODMAC level 4 data set contains radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm acquired by the OSIRIS Wide Angle Camera during the ROSETTA EXTENSION 2 phase of the Rosetta mission, covering the period from 2016-04-05T23:25:00.000 to 2016-05-03T23:25:00.000.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET PRELANDING OSIWAC 3 RDR MTP 004B V1.0

This data set contains calibrated images acquired by the OSIRIS Wide AngleCamera during the prelanding phase of the Rosetta mission at the comet 67P,covering the period from 2014-06-18 to 2014-07-02.

Tags: __
Organization: National Aeronautics and Space Administration
MMS 1 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 2004 model, Dynamic conditions), Level 2 (L2), Survey Mode, 30 s Data

Magnetospheric Multiscale 1 (MMS 1) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Quick-Look (30 s) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 2004 magnetic field model for disturbed magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 6 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.

Tags: activityindex, ephemeris, magneticfield
Organization: National Aeronautics and Space Administration
IMAGE RPI Monthly Electron Density Values

The electron density values listed in this file are derived from the IMAGE Radio Plasma Imager (B.W. Reinisch, PI) data using an automatic fitting program written by Phillip Webb with manual correction. The electron number densities were produced using an automated procedure (with manual correction when necessary) which attempted to self-consistently fit an enhancement in the IMAGE RPI Dynamic Spectra to either 1) the Upper Hybrid Resonance band, 2) the Z-mode or 3) the continuum edge. The automatic algorithm works by rules determined by comparison of the active and passive RPI data [Benson et al., GRL, vol. 31, L20803, doi:10.1029/2004GL020847, 2004]. The manual data points are not from frequencies chosen freely by a human. Rather the human specifies that the computer should search for a peak or continuum edge in a certain frequency region. Thus even the manual points are determined, in part, by the automatic algorithms. Of course that does not guarantee that the data points are right, but it does eliminate some human bias.

Tags: waves-active
Organization: National Aeronautics and Space Administration
MMS 1 Fast Plasma Investigation, Dual Ion Spectrometer (FPI, DIS) Instrument Distributions, Level 2 (L2), Fast Mode, 4.5 s Data

The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. This Product contains Phase Space Distribution Maps of Results from surveying the High Resolution Observations during each 4.5 s Period. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Fast Survey Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration