AndreaBozzo/ceres-open-data-index huggingface dataset:
Parker Solar Probe, FIELDS Radio Frequency Spectrometer, RFS, High Frequency Receiver, HFR, Spectra, Level 2 (L2), 7 s and 56 s Data

PSP FIELDS Radio Frequency Spectrometer, RFS, High Frequency Receiver, HFR, Data:\n\nThe RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1]. For a full description of the FIELDS experiment, see reference [2]. For a description of the RFS, see reference [3].\n\nThe RFS produces auto and cross spectral data products in two frequency ranges, the Low Frequency Reciever range and the High Frequency Receiver range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR high-resolution spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.\n\nThe Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the Polyphase Filter Bank, PFB, and the Fast Fourier Transform, FFT, spectral processing as described in reference [3]. Corrections for base capacitance and antenna effective length have not been applied. These corrections will be applied in Level 3 RFS data. Therefore, the units for all spectral quantities are given in V^2/Hz.\n\nThe time resolution of the RFS data vary with instrument mode. During encounter, which is when PSP is within 0.25 astronomical units, AU, of the Sun, the cadence for RFS HFR and LFR spectra is typically about 7 s. During cruise mode, which is the default mode for operations outside of 0.25 AU, the cadence for HFR and LFR spectra is about 56 s.\n\nReferences:\n\n* 1) Fox, N.J., Velli, M.C., Bale, S.D., et al., Space Sci Rev (2016), 204:7, DOI:10.1007/s11214-015-0211-6\n* 2) Bale, S.D., Goetz, K., Harvey, P.R., et al., Space Sci Rev (2016), 204:49, DOI:10.1007/s11214-016-0244-5\n* 3) Pulupa, M., Bale, S.D., Bonnell, J.W., et al., JGR Space Physics (2017), 122, 2836-2854, DOI:10.1002/2016JA023345

Tags: instrumentstatus, spectrum, waves-passive
Organization: National Aeronautics and Space Administration
Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) High Energy Telescope (HET) Proton and Helium PHA based Fluxes in ASCII Format, Daily Average Data

This Data Set contains Daily Average Proton and Helium PHA based Fluxes and Errors from the COSPIN High Energy Telescope (HET) in the approximate Energy Ranges 39-70 MeV/n and 71-94 MeV/n from Day 296, 1990 through Day 181, 2009

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
Characteristics of Reconnection Sites and Fast Flow Channels in an MHD Simulation: Simulation Results

The simulation outputs are asci files containing out from the MHD simulation mapped to the minimum magnetic field surface in the magnetotail during the March 14,2008 substorms. There is one time in each file and 2161 files each separated by 10s. The results span 6 hours from 0200 to 0800. The results are in GSM coordinates.  \n

Tags: electricfield, energeticparticles, ephemeris, magneticfield
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 6 3933 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2017-01-01 to 2018-12-31. It is a Occultation measurement and covers the time 2018-03-26T06:56:22.000 to 2018-03-26T07:22:49.949.

Tags: __
Organization: National Aeronautics and Space Administration
TWINS-2 Ephemeris, Definitive Spacecraft Attitude, PT0.512S Data

Two Wide-angle Imaging Neutral-atom Spectrometers 2, TWINS 2, Spacecraft Attitude data, Earth Centered Inertial, ECI, coordinates. This TWINS data set contains spacecraft attitude data as polar and azimuthal instrument pointing vectors. The polar vector points along the TWINS rotation axis. The azimuthal vector lies in the plane normal to the polar vector and points toward the central scanning position, which is defined as the zero-point location. Such pointing is derived from both the spacecraft attitude history, SAH, file and the sensor mounting orientation. The computation employed is designed to achieve a pointing accuracy of 0.5°. Any deviation from this accuracy level is indicated in the header record metadata.

Tags: ephemeris
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 4 EXT2-MTP030 RDR-STRLIGHT V1.0

This CODMAC level 4 data set contains solar stray light corrected, radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm, acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft during the ROSETTA EXTENSION 2 mission phase, covering the period from 2016-05-31T23:25:00.000 to 2016-06-28T23:24:59.000. 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 October 2018 PSA/PDS external peer review.

Tags: __
Organization: National Aeronautics and Space Administration
Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) High Energy Telescope (HET) Ion and Electron Eight-Sectored Coincidence Counting Rates in ASCII Format, 10 min Data

This Data Set contains 10 min Average Ion and Electron Eight-Sectored Coincidence Counting Rates from the COSPIN High Energy Telescope (HET). These Data provide a Measure of the Anisotropy of Particle Arrival Directions in the Spacecraft Spin Plane

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 3 3398 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2010-01-01 to 2012-12-31. It is a Global Gravity measurement and covers the time 2012-09-10T04:55:39.000 to 2012-09-10T07:35:09.500.

Tags: __
Organization: National Aeronautics and Space Administration
Parker Solar Probe, FIELDS Radio Frequency Spectrometer, RFS, Low Frequency Receiver, LFR, Spectra, Level 2 (L2), 7 s and 56 s Data

PSP FIELDS Radio Frequency Spectrometer, RFS, Low Frequency Reciever, LFR, Data:\n\nThe RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1]. For a full description of the FIELDS experiment, see reference [2]. For a description of the RFS, see reference [3].\n\nThe RFS produces auto and cross spectral data products in two frequency ranges, the Low Frequency Reciever range and the High Frequency Receiver range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR high-resolution spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.\n\nThe Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the Polyphase Filter Bank, PFB, and the Fast Fourier Transform, FFT, spectral processing as described in reference [3]. Corrections for base capacitance and antenna effective length have not been applied. These corrections will be applied in Level 3 RFS data. Therefore, the units for all spectral quantities are given in V^2/Hz.\n\nThe time resolution of the RFS data vary with instrument mode. During encounter, which is when PSP is within 0.25 astronomical units, AU, of the Sun, the cadence for RFS HFR and LFR spectra is typically about 7 s. During cruise mode, which is the default mode for operations outside of 0.25 AU, the cadence for HFR and LFR spectra is about 56 s.\n\nReferences:\n\n* 1) Fox, N.J., Velli, M.C., Bale, S.D., et al., Space Sci Rev (2016), 204:7, DOI:10.1007/s11214-015-0211-6\n* 2) Bale, S.D., Goetz, K., Harvey, P.R., et al., Space Sci Rev (2016), 204:49, DOI:10.1007/s11214-016-0244-5\n* 3) Pulupa, M., Bale, S.D., Bonnell, J.W., et al., JGR Space Physics (2017), 122, 2836-2854, DOI:10.1002/2016JA023345

Tags: instrumentstatus, spectrum, waves-passive
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 3 0895 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 3 phase 2015-07-01 to 2015-10-21. It is a Global Gravity measurement at the comet 67P and covers the time 2015-07-13T21:14:45.000 to 2015-07-14T04:39:07.500.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 2 0772 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 2 phase 2015-03-11 to 2015-06-30. It is a Global Gravity measurement at the comet 67P and covers the time 2015-05-13T09:30:20.000 to 2015-05-13T12:09:24.000.

Tags: __
Organization: National Aeronautics and Space Administration
Ulysses Dust Detection System Data

This data set contains information collected by the Ulysses Cosmic Dust instrument on the dust environment in interplanetary space within the inner solar system, between Jupiter and the Sun, and at high polar latitudes of the Sun. Both interplanetary and interstellar dust particles have been detected. This information is collected with a dust impact experiment, from which may be inferred direction of motion, mass, velocity and charge (see ULYDINST.CAT). The data presented in this dataset include instrumental readouts, inferred metadata, calibration information and a calendar of events.

Tags: dust
Organization: National Aeronautics and Space Administration
Circumpolar Arctic Vegetation, Geobotanical, Physiographic Maps, 1982-2003

This data set provides the spatial distributions of vegetation types, geobotanical characteristics, and physiographic features for the circumpolar Arctic tundra biome for the period 1982-2003. Specific attributes include dominant vegetation, bioclimate subzones, floristic subprovinces, landscape types, lake coverage, Arctic treeline, elevation, and substrate chemistry data. Vegetation indices, trends, and biomass estimate products for the circumpolar Arctic through 2010 are also provided.

Tags: earth-science-atmospheric-temperature-atmosphere-surface-temperature-air-temperature, earth-science-ecosystems-biosphere-terrestrial-ecosystems-forests, earth-science-landscape-land-surface-landscape-patterns, earth-science-topography-land-surface-terrain-elevation, earth-science-vegetation-biosphere-biomass, earth-science-vegetation-biosphere-vegetation-cover, earth-science-vegetation-biosphere-vegetation-species
Organization: National Aeronautics and Space Administration
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 10 s Data

Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.\n\nThe public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).\n\nRefer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.\n\nThe PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:\n\nAcknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).\n\nCitation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 10 s Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/6b2f-mx69

Tags: energeticparticles, ephemeris
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 2 0734 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 2 phase 2015-03-11 to 2015-06-30. It is a Global Gravity measurement at the comet 67P and covers the time 2015-04-27T12:33:05.000 to 2015-04-27T19:58:06.500.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 PRELANDING 0213 V1.0

This is a Rosetta Radio Science data set, collected during the PRELANDING phase 2014-01-21 to 2014-11-18. It is a Global Gravity measurement at the comet 67P and covers the time 2014-08-17T00:07:05.000 to 2014-08-17T06:45:08.500.

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

Heliocentric trajectories for Parker Solar Probe in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinates\n\nThe 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.\n\nThe 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:\n\n+---------------------------------------------------------------------+\n| Method Name  | FPA Longitude Definition                             |\n|---------------------------------------------------------------------|\n| B1950.0      | the actual FPA at 22:09 UT on December 31, 1949      |\n| J2000.0      | the smoothed FPA at 12:00 UT on January 1, 2000      |\n| True of Date | the actual FPA at 00:00 UT on the date of interest   |\n| Mean of Date | the smoothed FPA at 00:00 UT on the date of interest |\n+---------------------------------------------------------------------+\n\nThe heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method.\n\nMore 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.\n\nCitation: Szabo, A. (2020). Parker Solar Probe Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/41s1-hx58

Tags: ephemeris
Organization: National Aeronautics and Space Administration
VG1 SAT MAG RESAMPLED KRONOGRAPHIC (L1)                                      COORDS 48.0SEC V1.0

This data set includes calibrated    magnetic field data acquired by the Voyager 1 Low Field Magnetometer    (LFM) during the Saturn encounter. Coverage begins in the solar wind    inbound to Saturn and continues past the last outbound bowshock crossing.    The data are in Kronographic (L1) coordinates and have been averaged from    the 9.6 second summary rate to a 48 second sample rate. All magnetic field    measurements are given in nanoTesla (nT). The magnetic field data    are calibrated (see the calibration description included in the    Voyager 1 Magnetometer instrument catalog file for details).  This    data set supersedes VG1-S-MAG-4-48.0SEC.

Tags: __
Organization: National Aeronautics and Space Administration
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 5 min Data

Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.\n\nThe public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).\n\nRefer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.\n\nThe PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:\n\nAcknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).\n\nCitation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 5 min Data [Data set]. NASA Space Physics Data Facility.

Tags: energeticparticles, ephemeris
Organization: National Aeronautics and Space Administration
TIMED SEE Level 4 XPS Modeled Solar Irradiance Data

The SEE XPS Level 4 data are derived from the XPS Level 1 data products. The XPS Level 4 processing algorithm uses reference CHIANTI spectral models to generate a higher spectral resolution (0.1 nm) estimate of the solar XUV irradiance by scaling the model reference spectra to match the XPS photometer currents (signal). The CHIANTI Quiet Sun (QS) spectrum and Active Region (AR) spectrum are used with a scaling of the AR spectrum to match the minimum signal on each day, and then a CHIANTI isothermal flare spectrum is scaled to match the signal above the daily minimum signal. The flare temperature is determined from the ratio of the GOES XRS 0.1-0.8 nm irradiance to the GOES XRS 0.05-0.4 nm irradiance. These scaling factors, flare temperature, and resulting model spectrum in the 0-40 nm range in 0.1 nm intervals are in the XPS Level 4 data product for every measurement made by XPS photometer #1 or #2 (0.1-7 nm band).\n\nA SEE XPS Level 4 data product is produced for each UT day, and these daily products are also merged into three different full mission data files:\n\n    daily averages (24-hour)\n    orbit averages (3-min about every 97 min)\n    1-minute averages (but with only about 3% duty cycle)\n\nThe XPS Level 4 result in 0.1 nm intervals is also compressed into 1-nm intervals for use in the SEE Level 3 and Level 3A data products.\n\nOn-orbit instrument characterization is an ongoing effort, and the SEE team checks photometer degradation using redundant channels and underflight calibration rockets whose payload includes TIMED SEE prototype instruments.\n\nThe accuracy of the XPS Level 1 irradiance is 12%-26%, photometer dependent. There is additional uncertainty for applying the spectral model for the XPS Level 4 irradiances, and this estimated accuracy is 30% for the integrated XUV irradiance. The spectral distribution in the XPS Level 4 is from the CHIANTI model and not from direct measurements from XPS, a set of broadband photometers. The spectral distribution above 27 nm has been validated with the TIMED SEE EGS (27-190 nm, 0.4 nm resolution) measurements, so there is good confidence in the spectral distribution shortward of 27 nm.

Tags: irradiance-timed, see, sun
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 4 ESC1-MTP011 RDR-INFLDSTR 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 W/m^2/sr/nm,  acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft  during the COMET ESCORT 1 mission phase, covering the period  from 2014-12-19T23:25:00.000 to 2015-01-13T23:24:59.000. 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
ROSETTA-ORBITER 67P OSINAC 4 EXT1-MTP025 RDR-REFLECT V1.0

This CODMAC level 4 data set contains 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 ROSETTA EXTENSION 1 mission phase, covering the period from 2016-01-12T23:25:00.000 to 2016-02-09T23:24:59.000. 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 October 2018 PSA/PDS external peer review.

Tags: __
Organization: National Aeronautics and Space Administration