AndreaBozzo/ceres-open-data-index huggingface dataset:
Rosetta Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

Heliocentric trajectories for Rosetta 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.

Tags: ephemeris
Organization: National Aeronautics and Space Administration
SDO/EVE Data Products at LASP/U.Colo

The EVE (Extreme Ultraviolet Variability Experiment)\nPrincipal Investigator site at U. Colorado's Laboratory for Atmospheric\nand Space Physics (LASP) archives, and provides multiple access paths \nto, a variety of SDO(Solar Dynamics Observatory)/EVE digital and \ndisplay solar images, as well as to tools for selecting and analyzing\ndata.  Data include Ka band and S band irradiances, and spectra, at various\ncalibration levels and at product-dependent time resolutions ranging\nbetween 0.25s and 1 min.

Tags: irradiance, spectrum
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 ROSETTA EXTENSION 1 1334 V1.0

This is a Rosetta Radio Science data set, collected during the ROSETTA EXTENSION 1 phase 2016-01-01 to 2016-04-05. It is a Global Gravity measurement at the comet 67P and covers the time 2016-01-12T01:07:20.000 to 2016-01-12T05:13:24.000.

Tags: __
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 5 3827 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2015-01-01 to 2016-12-31. It is a Occultation measurement and covers the time 2015-09-19T15:00:39 to 2015-09-21T12:16:39.500.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT 3 OSIWAC 3 RDR MTP020 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 2015-08-25T23:25:00.000 to 2015-09-22T23:24:59.000.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/EVE Level 4 Version 8 Data

The Laboratory for Atmospheric and Space Physics in Boulder, Colorado created Level 4 data files for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for maintaining access to all EVE products.\n\nThe level 4 spectra products consist of a model spectrum at a 1-minute cadence, with each product containing 1,440 spectra covering one UTC day. The model spectra are derived from the ESP quadrant diode irradiance and the isothermal plasma temperature from the GOES X-ray channel ratios. These measurements drive a model with components for quiet sun, active region, and flare spectrum contributions. A similar technique was used for TIMED-SEE and SORCE XPS level 4 products that utilized XPS soft x-ray measurements that are analogous to the ESP quadrant diode measurements.

Tags: irradiance, spectrum
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 2 EXT2-MTP030 EDR V3.0

This CODMAC level 2 data set contains uncalibrated image data in DN unit, 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 V3.0 supersedes previous deliveries of the same dataset with the following changes since the last version: Lien corrected dataset after the July and October 2018 PSA/PDS external peer reviews. Updated documentation and ancillary files, added document on bandpass filter. Updated SCIENCE_USER_GUIDE_V03.PDF to include one section about FAQ and one section about image data quality. Added shutter backtravel and readout issues to image quality map. Updated DATA_QUALITY_ID keyword in image header. Improved handling of images with missing packets.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/EVE Level 3 Version 8 Mission-Long Data

EVE level 3 data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. For a high-level introduction to the EVE instrumentation please visit:\nhttps://lasp.colorado.edu/home/eve/science/instrument/\n\nLevel 3 products are defined to contain daily averages beginning on 2010, day 120, April 30. This version change includes updated long-term degradation corrections for MEGS-B and ESP. A small dark adjustment was applied to MEG-B and large degradation changes were applied based on SDO EVE sounding rocket measurements. The MEGS-P (Lyman-alpha) diode processing has been updated to replace the Kalman filter with a Fourier transform filter, and the calibration has been updated to match SORCE SOLSTICE version 17.\n\nThe mission length merged datasets are provided at three sampling sizes for user convenience; specifically, native level 2 sampling (0.02nm), 1 angstrom, and 1 nm. The optical resolution is about 0.1 nm, so the 0.02nm spectra contain 5 samples per resolution element.

Tags: irradiance, spectrum
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSINAC 4 ESC2-MTP016 RDR-STR-REFL V1.0

This CODMAC level 4 data set contains solar stray light corrected, radiometric calibrated and geometric distortion corrected (resampled) image data in in reflectance units (normalized and thus without unit), acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft during the COMET ESCORT 2 mission phase, covering the period from 2015-05-05T23:25:00.000 to 2015-06-02T23:24:59.000. 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
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 7 4156 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2019-01-01 to 2020-12-31. It is a Occultation measurement and covers the time 2020-11-25T14:14:44.200 to 2020-11-25T14:36:52.500.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI Continuum, 720-Second Data

The HMI continuum data refers to map of the continuum intensity of the solar spectrum in the region of the Fe I absorption line at 6173 Å on the surface of the sun.\n\nHMI samples the Fe I absorption line at 6173.3 Å at six points. Assuming that the "pure" solar Fe I line profile is a Gaussian, and the HMI filter filter transmission profiles are delta functions, the first and second Fourier coefficients of the of the Fe I line can be calculated and an estimate of the Doppler Velocity can be made. An estimate (proxy) for the continuum intensity Ic is obtained by "reconstructing" the solar line from the estimates of the Doppler shift λo, the linewidth σ, and the linedepth Id. More details can be found at http://jsoc.stanford.edu/relevant_papers/observables.pdf.\n

Tags: imageintensity
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 3 3281 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 2012-05-08T07:26:07.000 to 2012-05-08T09:25:54.500.

Tags: __
Organization: National Aeronautics and Space Administration
MARS EXPRESS SUN MRS 1/2/3 EXTENDED MISSION 5 3769 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2015-01-01 to 2016-12-31. It is a Solar Conjunction measurement and covers the time 2015-06-16T14:33:00 to 2015-06-16T17:44:00.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER SW RPCLAP 3CR4A CALIB2 V1.0

This data set containsCALIBRATED data from Rosetta RPC-LAP, acquired during the CRUISE 4-1mission phase where the primary target was the SOLAR WIND. It containsinstrument outputs in volts and amperes, calibrated and corrected forinstrument offsets.

Tags: __
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 4 3513 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2013-01-01 to 2014-12-31. It is a Global Gravity measurement and covers the time 2013-02-11T08:47:02.000 to 2013-02-11T10:48:00.500.

Tags: __
Organization: National Aeronautics and Space Administration
GO UVS TABULAR DATA FROM THE SL9-G IMPACT WITH JUPITER V1.0

The UltraViolet Spectrometer (UVS) on the Galileo spacecraft took unique data of Comet Shoemaker-Levy/9's impact with Jupiter. A preliminary analysis of this data is presented in this submission to the Planetary Data System (PDS). It consists of four small tables with detached labels and documentation.

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

Heliocentric trajectories for Sakigake 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.

Tags: ephemeris
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3                                     EXTENDED MISSION 9 4411 V1.0

This is a Mars Express                                     Radio Science data set, collected                                     during the extended mission phase                                     2023-01-01 to 2026-12-31.                                     It is a Occultation                                     measurement and covers the time                                     2024-02-22T00:49:15.500 to                                     2024-02-22T01:11:22.800.

Tags: __
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 8 4205 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2021-01-01 to 2022-12-31. It is a Occultation measurement and covers the time 2021-04-04T10:04:30.549 to 2021-04-04T10:54:32.349.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI line-of-sight Dopplergram, 720-Second Data

Dopplergrams are maps of solar surface velocity. The HMI (Camera 2) instrument takes 72 filtergrams to construct a single dopplergram. Six filtergrams are taken in six positions across the nominal 6173.3 Å spectral line; each filtergram is taken in two polarization states (right circularly polarized (RCP), or Stokes I-V, and left circularly polarized (LCP), or I+V). Assuming that the absorption line is a Gaussian and that the HMI filter transmission profiles are delta functions, the Fourier coefficients can be calculated and are then used to estimate the line-of-sight magnetic field strength B.

Tags: dopplergram
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 3 3306 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 2012-12-16T03:49:16.000 to 2012-12-16T05:42:05.500.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI Linedepth, 720-Second Data

The HMI Linedepth refers to the difference in intensity between the "true" continuum and intensity at the core of the the Fe I absorption line at 6173.3 Å on the surface of the sun. \n\nHMI samples the Fe I absorption line at 6173.3 Å at six points. Assuming that the "pure" solar Fe I line profile is a Gaussian, and the HMI filter filter transmission profiles are delta functions, the first and second Fourier coefficients of the of the Fe I line can be calculated and an estimate of the Doppler Velocity can be made. An estimate (proxy) for the continuum intensity Ic is obtained by "reconstructing" the solar line from the estimates of the Doppler shift λo, the linewidth σ, and the linedepth Id. More details can be found at http://jsoc.stanford.edu/relevant_papers/observables.pdf.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
CH1-ORB MOON M3 4 L2 REFLECTANCE  NEAR-IR SPECTRAL IMGS V1.0

This dataset contains pixel located,  reflectance-calibrated, near-IR spectral image data acquired from  November 2008 through August 2009 by the Moon Mineralogy Mapper  instrument during the Chandrayaan-1 mission to the Moon.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI Linedepth, 45-Second Data

The HMI Linedepth refers to the difference in intensity between the "true" continuum and intensity at the core of the the Fe I absorption line at 6173.3 Å on the surface of the sun. \n\nHMI samples the Fe I absorption line at 6173.3 Å at six points. Assuming that the "pure" solar Fe I line profile is a Gaussian, and the HMI filter filter transmission profiles are delta functions, the first and second Fourier coefficients of the of the Fe I line can be calculated and an estimate of the Doppler Velocity can be made. An estimate (proxy) for the continuum intensity Ic is obtained by "reconstructing" the solar line from the estimates of the Doppler shift λo, the linewidth σ, and the linedepth Id. More details can be found at http://jsoc.stanford.edu/relevant_papers/observables.pdf.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
SDO/HMI Data Products at JSOC/Stanford U.

The HMI-AIA (Helioseismic and Magnetic Imager -\nAtmospheric Imaging Assembly) JSOC (Joint Science Operations Center) \nat Stanford University archives, and provides multiple access paths \nto, a variety of SDO(Solar Dynamics Observatory)/HMI digital and \ndisplay solar images and movies.  Included are dopplergrams (maps \nof solar surface velocity), continuum filtergrams (broad-wavelength \nphotographs of the solar photosphere), and both line-of-sight and \nvector magnetograms (maps of the photospheric magnetic field).\n

Tags: dopplergram, imageintensity, magnetogram
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 3 ESC1-MTP013 RDR V3.0

This CODMAC level 3 data set contains radiometric calibrated image data in W/m^2/sr/nm, acquired by the OSIRIS Wide Angle Camera on the Rosetta spacecraft during the COMET ESCORT 1 mission phase, covering the period from 2015-02-10T23:25:00.000 to 2015-03-10T23:24:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V3.0 supersedes previous deliveries of the same dataset with the following changes since the last version: Lien corrected dataset after the July and October 2018 PSA/PDS external peer reviews. Updated documentation and ancillary files, added document on bandpass filter. Updated SCIENCE_USER_GUIDE_V03.PDF to include one section about FAQ and one section about image data quality. Added shutter backtravel and readout issues to image quality map. Updated DATA_QUALITY_ID keyword in image header. Improved handling of images with missing packets. Included FITs files. Browse products changed to the same size as the original image.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER CHECK GIADA 2 RVM1 RENDEZMANOEUVRE1 V1.0

Payload Checkout 13 (PC13) was the final Cruise Phase Checkout of several payload checkouts performed with the Rosetta Payload. Since PC13 was scheduled as the final Cruise Phase Checkout, a number of additional payload operations were also executed to close out pending and essential requirements, and/or configure instruments for the upcoming Deep Space Hibernation Phase. Given the importance of this final checkout all Rosetta payload, except Osiris, took part in this scenario The Payload Checkout 13 ran for 9 consecutive days starting on the 1st December 2010 until the 9th December 2010. An RSI passive checkout was also completed on 14th December 2010. The Scenario was covered by dedicated NNO and DSN. During PC13 GIADA performs only a passive test (GD01) similar to the previous Passive Payload Checkouts. This passive test (GD01), which includes standard procedures and full functional verification, was executed by switching on Main and Redundant I/Fs in sequence and executing similar procedures for the two cases. The data reported in this data set have been converted from ADC counts to engineering values. The quality of the Housekeeping and Calibration data is good. Scientific data are due to noise, as no grain event is expected during this mission phase. These data must be only considered to evaluate GIADA behaviour and not as real scientific data. Data reported by GDS and IS are due to noise as no dust event is expected during this mission phase. MBS frequency changes, once normalised for frequency vs. temperature dependence, if present, are due to deposition of contaminants existing in the S/C environment. Housekeeping and Calibration data from all GIADA sub-systems are useful to evaluate instrument health and behaviour when compared with similar data acquired during other mission phases.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI Linewidth, 720-Second Data

The linewidth observable refers to the FWHM of the (assumed) Gaussian absorption line profile for the 6173.3 Å line on the surface of the sun.\n\nHMI samples the Fe I absorption line at 6173.3 Å at six points. Assuming that the "pure" solar Fe I line profile is a Gaussian, and the HMI filter filter transmission profiles are delta functions, the first and second Fourier coefficients of the of the Fe I line can be calculated and an estimate of the Doppler Velocity can be made. An estimate (proxy) for the continuum intensity Ic is obtained by "reconstructing" the solar line from the estimates of the Doppler shift λo, the linewidth σ, and the linedepth Id. More details can be found at http://jsoc.stanford.edu/relevant_papers/observables.pdf.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3                                     EXTENDED MISSION 9 4437 V1.0

This is a Mars Express                                     Radio Science data set, collected                                     during the extended mission phase                                     2023-01-01 to 2026-12-31.                                     It is a Occultation                                     measurement and covers the time                                     2024-03-20T02:22:01.100 to                                     2024-03-20T02:44:09.200.

Tags: __
Organization: National Aeronautics and Space Administration