AndreaBozzo/ceres-open-data-index huggingface dataset:
Far Ultraviolet Explorer (FUSE) Observation Log

NASA&#39;s FUSE (Far Ultraviolet Spectroscopic Explorer) spacecraft provided spectra in the far-ultraviolet portion of the electromagnetic spectrum (the wavelength range from 905 - 1180 Angstroms, or 90.5 - 118 nm), with a high spectral resolution of about 20000 (one wavelength point each 5 pm). FUSE was funded by NASA as part of its Origins program, and was developed in collaboration with the space agencies of Canada and France. It was operated for NASA by the Johns Hopkins University. FUSE was launched into orbit aboard a Delta II rocket on June 24, 1999 for a nominal mission of three years of operations. This table contains the FUSE Observation Log up to May 8, 2007, as archived at CDS in summer 2007. FUSE was formally decommissioned on October 18, 2007, following the failure of the last control wheel on the spacecraft in July 2007. More information about the FUSE Project can be found at NASA&#39;s Optical and Ultraviolet Archive (MAST) at &lt;a href="http://archive.stsci.edu/"&gt;http://archive.stsci.edu/&lt;/a&gt; and at the Johns Hopkins FUSE web site at &lt;a href="http://fuse.pha.jhu.edu/"&gt;http://fuse.pha.jhu.edu/&lt;/a&gt;. This database table was updated by the HEASARC in March 2009, superceding the previous versions of May 2007, May 2004, March 2005, and April 2006. It is primarily based on the CDS table &lt;B/fuse&gt;, specifically, the files fuse.dat, refs.dat and proposal.dat, but also contains additional information on proposal titles and bibliographic codes obtained from the MAST FUSE Archive. The HEASARC plans to update the bibliographic metadata for this table on a monthly basis as and when new information from the latter source becomes available. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Rosette Molecular Cloud Chandra X-Ray Point Source Catalog

The authors of this study have explored the young stellar populations in the Rosette Molecular Cloud (RMC) region with high spatial resolution X-ray images from the Chandra X-ray Observatory, which are effective in locating weak-lined T Tauri stars as well as disk-bearing young stars. A total of 395 X-ray point sources are detected, 299 of which (76%) have an optical or near-infrared (NIR) counterpart identified from deep FLAMINGOS images. From X-ray and mass sensitivity limits, the authors infer a total population of ~1700 young stars in the survey region. Based on smoothed stellar surface density maps, they investigate the spatial distribution of the X-ray sources and define three distinctive structures and substructures within them. Structures B and C are associated with previously known embedded IR clusters, while structure A is a new X-ray-identified unobscured cluster. A high-mass protostar RMCX 89 = IRAS 06306+0437 and its associated sparse cluster are studied. The different subregions are not coeval but do not show a simple spatial-age pattern. Disk fractions vary between subregions and are generally &lt;~ 20% of the total stellar population inferred from the X-ray survey. The data are consistent with speculations that triggered star formation around the H II region is present in the RMC, but do not support a simple sequential triggering process through the cloud interior. While a significant fraction of young stars are located in a distributed population throughout the RMC region, it is not clear if they originated in clustered environments. This HEASARC table contains the 348 primary sources listed in Table 1 of the reference paper, as well as the 47 tentative sources listed in Table 2 (the latter having a likelihood &gt; 10&lt;sup&gt;-3&lt;/sup&gt; of being a spurious background fluctuation based on Poisson statistics), to make a total of 395 X-ray sources. The information on optical and infrared counterparts to these X-ray sources which was provided in Table 4 of the reference paper has also been included herein. In order to allow users to clearly identify these 2 samples, the HEASARC has created a parameter source_sample which is set to &#39;P&#39; for the Table 1 primary sources and to &#39;T&#39; for the Table 2 tentative sources. This HEASARC table also contains the X-ray spectroscopic information derived for 158 sources which have photometric significance (the snr parameter) &gt;= 2.0 which was presented in Table 3 of the reference paper. All spectral fits used the &quot;wabs(apec)&quot; model in XSPEC and assumed 0.3 * Z_Sun abundances. The quoted emission measures and X-ray luminosities assume a distance to the Rosette molecular cloud of 1.4 kpc. This table was created by the HEASARC in July 2009 based on the merger of electronic versions of tables 1, 2, 3 and 4 from the above reference which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 PRELANDING 0288 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 2014-09-11T17:24:29.000 to 2014-09-12T01:05:11.000.

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Organization: National Aeronautics and Space Administration
ROSATAll-SkySurvey:Giants&Supergiants

The ROSAT All-Sky Survey Catalogue of Optically Bright Late-Type Giant and Supergiant Stars contains X-ray data for all late-type (spectral types of A through M, inclusive) giants and supergiants (luminosity classes of I through III-IV, inclusive) listed in the Bright Star Catalogue (BSC) that have been detected in the ROSAT All-Sky Survey. The RASS giants and supergiants catalog contains 450 entries of X-ray emitting, evolved late-type stars, which corresponds to an average detection rate of 11.7 percent. For each star, the ROSAT PSPC count rate, the hardness ratio, the apparent X-ray flux (calculated using an individual energy-conversion-factor based on the hardness ratio), and the ratio of X-ray to bolometric flux are given. The full details of the data selection, the source detection criteria, etc., are given in the paper by Huensch, Schmitt and Voges (1998, A&amp;AS, 127, 251) describing this catalog; essentially for a star to be identified as an X-ray source, the X-ray source had to have at least a 99.9 percent existence probability, corresponding to a likelihood of greater than or equal to 7, and lie within 90 arcseconds of the optical position. Given the number of sky locations examined and the total number of RASS sources, it is expected that of order 27.4 of the 450 claimed associations in this catalog will be chance coincidences. This database was created at the HEASARC in July 1998 based on the ADC/&lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+AS/127/251"&gt;CDS Catalog J/A+AS/127/251&lt;/a&gt;. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
NGC 2244/Rosette Nebula Chandra X-Ray Point Source Catalog

This table contains the point source catalog based on the first high spatial resolution X-ray study of NGC 2244, the 2 Myr old stellar cluster in the Rosette Nebula, using Chandra. Over 900 X-ray sources are detected within 20 arcminutes of the cluster central position (J2000.0 RA and Dec of 6 31 59.9, +4 55 36); 77% of these X-ray sources have optical or FLAMINGOS NIR stellar counterparts and are mostly previously uncataloged young cluster members. The X-ray-selected population is estimated to be nearly complete between 0.5 and 3 M&lt;sub&gt;solar&lt;/sub&gt;. A number of further results emerge from the analysis: (1) The X-ray luminosity function (XLF) and the associated K-band LF indicate a normal Salpeter IMF for NGC 2244. This is inconsistent with the top-heavy IMF reported from earlier optical studies that lacked a good census of &lt; 4 M&lt;sub&gt;solar&lt;/sub&gt; stars. By comparing the NGC 2244 and Orion Nebula Cluster XLFs, the authors estimate a total population of ~2000 stars in NGC 2244. (2) The spatial distribution of X-ray stars is strongly concentrated around the central O5 star, HD 46150. The other early O star, HD 46223, has few companions. The cluster&#39;s stellar radial density profile shows two distinctive structures: a power-law cusp around HD 46150 that extends to ~0.7 pc, surrounded by an isothermal sphere extending out to 4 pc with core radius 1.2 pc. This double structure, combined with the absence of mass segregation, indicates that this 2 Myr old cluster is not in dynamical equilibrium. (3) The fraction of X-ray-selected cluster members with K-band excesses caused by inner protoplanetary disks is 6%, slightly lower than the 10% disk fraction estimated from the FLAMINGOS study based on the NIR-selected sample. (4) X-ray luminosities for 24 stars earlier than B4 confirm the long-standing log (L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt;) ~ -7 relation. The Rosette OB X-ray spectra are soft and consistent with the standard model of small-scale shocks in the inner wind of a single massive star. This table was created by the HEASARC in July 2008 based on electronic versions of Tables 2, 3, 4, 5 and 6 of the reference paper which were obtained from the electronic ApJ web site. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 PRELANDING 0298 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 2014-09-16T17:05:04.000 to 2014-09-16T23:25:10.500.

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Organization: National Aeronautics and Space Administration
NEW HORIZONS  SDC PLUTO CRUISE  CALIBRATED V2.0

This data set contains Calibrated data taken by the New Horizons  Student Dust Counter  instrument during the  pluto cruise  mission phase. This is VERSION 2.0 of this data set.   SDC collected science data intermittently during the hibernation  years following the Jupiter encounter, designated as the PLUTOCRUISE  phase. There were also Annual Checkouts (ACOs), STIM calibrations,  Noise calibrations, and an anomaly in November, 2007.   SDC's main science data collection periods were during hibernation.  During ACOs, science data are taken intermittently but the user must  be careful in analyzing these data since there is usually more  activity on the spacecraft during hibernation. STIM and Noise refer  to scheduled calibrations and are done with a regular cadence of one  per year after the Jupiter encounter; they occurred sporadically in  the early years of the mission.   Note that some SDC data files have the same stop and start time and  a zero exposure time. The reason for this is that the start and  stop time for SDC data files are the event times for the first and  last events in the files, so for files that contain a single event,  these two values are the same.   The changes in Version 2.0 were re-running of the ancillary data  in the data product, updated geometry from newer SPICE kernels,  minor editing of the documentation, catalogs, etc., and resolution  of liens from the December, 2014 review, plus those from the May,  2016 review of the Pluto Encounter data sets.   New observations added with this version (V2.0) include ongoing  cruise observations from August, 2014 through January, 2015.

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Organization: National Aeronautics and Space Administration
NuSTAR As-Flown Timeline

The NUAFTL database table records the As-Flown Timeline for the Nuclear Spectroscopic Telescope Array (NuSTAR) hard X-ray observatory. NuSTAR observes the sky in the high energy X-ray (3 - 79 keV) region of the electromagnetic spectrum using focusing optics. The as-flown timeline provides a summary of what NuSTAR has observed and is updated automatically when each observation is completed. This HEASARC database table is updated automatically within a day or so of updates to the referenced URL. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
AMMR Air and Brightness Temperature Data, Wakasa Bay, Version 1

The Wakasa Bay Field Campaign was conducted to validate rainfall algorithms developed for the Advanced Microwave Scanning Radiometer - Earth Observing System (AMSR-E).

Tags: earth-science-atmospheric-temperature-atmosphere-surface-temperature-air-temperature, earth-science-microwave-spectral-engineering-brightness-temperature
Organization: National Aeronautics and Space Administration
TD1 Stellar Ultraviolet Fluxes Catalog

The Belgian/UK Ultraviolet Sky Survey Telescope (S2/68) in the ESRO TD1 satellite carried out a controlled scan of the entire sky. It measured the absolute ultraviolet flux distribution between 2740A and 1350A of point sources down to 10th visual magnitude for unreddened early B stars. The S2/68 experiment has been described by Boksenberg et al. (1973MNRAS.163..291B), and the absolute calibration by Humphries et al. (1976A&amp;A....49..389H). The TD1 Catalog of Stellar Ultraviolet Fluxes represents results from the sky-scan experiment on the TD1 satellite of the European Space Research Organization (ESRO), now part of ESA. It lists the absolute fluxes, in four passbands, for 31,215 stars: &lt;pre&gt; Passband Center: 274.0nm 236.5nm 196.5nm 156.5nm Effective Width: 31.0nm 33.0nm 33.0nm 33.0nm &lt;/pre&gt; The stars have been selected subject to the constraint that the signal-to-noise ratio should be at least 10.0 in any one of the four passbands. Null values of a flux field and an error field indicate there are no valid data for the star. This usually arises with close pairs of stars whose spectra overlap. Five standard flux error values are greater than 99.99, and were too large for the format of the flux field in the original table. Thus, the flux error values which were greater than 99.99 are given as 99.99. Many of the fainter stars of spectral type later than A5 do not have significant signals in all of the spectrophotometric channels (particularly the 1565A channel). Consequently, after the removal of the background, they can randomly give rise to small negative values of flux. Those negative values were not suppressed, but are given together with their error, as they can be significant when considered as part of a statistical sample. Although the sky coverage is essentially complete, the catalog does not contain the fluxes for all stars that fall within the limit of the sensitivity of the instrument. If any star expected to be present is missing, then its signal is probably blended with that of a nearby star, in which case the data have been discarded. The original contents of the HEASARC&#39;s TD1 database table came from a magnetic tape sent to NASA/Goddard Space Flight Center by Dr. G.I. Thompson of the Royal Observatory in Edinburgh, Scotland. The HEASARC recreated this database table in August 2005, based on the &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/59B"&gt;CDS Catalog II/59B&lt;/a&gt; file catalog.dat.gz, in an effort to modernize its parameter names and documentation, as well as to add Galactic coordinates. The data in the CDS version originally came from &quot;Selected Astronomical Catalogs&quot; Vol. 1 CD-ROM released by the NASA Astronomical Data Center (ADC) in 1991. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Updated AGILE Catalog of Bright Gamma-Ray Sources and Variability

This table contains some of the results from a variability study of a sample of bright gamma-ray (30 MeV - 50 GeV) sources. This sample is an extension of the first AGILE catalog of gamma-ray sources (1AGL), obtained using the complete set of AGILE observations in pointing mode performed during a 2.3 year period from July 9, 2007 until October 30, 2009. The dataset of AGILE pointed observations covers a long time interval and its gamma-ray data archive is useful for monitoring studies of medium-to-high brightness gamma-ray sources. In the analysis reported here, the authors used data obtained with an improved event filter that covers a wider field of view, on a much larger (about 27.5 months) dataset, integrating data on observation block (OB) time scales, which mostly range from a few days to thirty days. The data processing resulted in a better characterized source list than 1AGL was, and includes 54 sources, 7 of which are new high galactic latitude (|b_II_|&gt;= 5 degrees) sources, 8 are new sources on the galactic plane, and 20 sources are from the previous catalogue with revised positions. Eight 1AGL sources (2 high-latitude and 6 on the galactic plane) were not detected in the final processing either because of low OB exposure and/or due to their position in complex galactic regions. The reference paper reports the results in a catalog of all the detections obtained in each single OB, including the variability results for each of these sources. In particular, the authors found that 12 sources out of 42 or 11 out of 53 are variable, depending on the variability index used, where 42 and 53 are the number of sources for which these indices could be calculated. Seven of the 11 variable sources are blazars, the others are the Crab pulsar+nebula, LS I +61 303, Cyg X-3, and 1AGLR J2021+4030. This HEASARC table contains 54 AGILE-detected sources and the main parameters of their maximum significance (defined by sqrt(TS)) detections: for each source, the name, coordinates, the sqrt(TS) value as a measure of the detection significance, the E &gt; 100 MeV flux, the four variability indices described in Section 5 of the reference paper, the number of detections, the confirmed counterparts and source class, if any, and other possible associations ordered according to the angular distance from the AGL source are given. These data are listed in Table 5a of the reference paper. This HEASARC table does not contain the list of fluxes for these sources as measured in all of the relevant individual OBs (Table 5b in the reference paper). This latter is obtainable from the CDS: &lt;a href="http://cdsarc.u-strasbg.fr/ftp/cats/J_A+A/558/A137/table5b.dat"&gt;http://cdsarc.u-strasbg.fr/ftp/cats/J_A+A/558/A137/table5b.dat&lt;/a&gt;. This table was created by the HEASARC in December 2013 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/558/A137"&gt;CDS catalog J/A+A/558/A137&lt;/a&gt; file table5a.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
GO E PWS RESAMP SUMMARY EARTH 1 SPECTRUM ANALYZER 60S V1.0

This data set includes 1-minute averages of the electric and magnetic    wave spectra obtained during the period that the Galileo plasma wave    receiver was operated during the first flyby of Earth.  The parameter    provided for the electric field spectrum is the electric field spectral    density in units of V^2/m^2/Hz. The magnetic field spectrum is provided    in units of magnetic field spectral density, nT^2/Hz.

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Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MARSIS EXPERIMENT DATA RECORD EXT 4 V1.0

This dataset contains the                    scientific telemetry produced by the MARSIS                    instrument after editing for duplicated and                    corrupted packets, together with geometric                    information computed on ground to locate                    observations in space and time. Both subsurface                    and ionosphere sounding data are included in                    the dataset.

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Organization: National Aeronautics and Space Administration
AMPR BRIGHTNESS TEMPERATURE (TB) TOGA COARE

The Advanced Microwave Precipitation Radiometer (AMPR) data set was part of the atmospheric measurements collected during the intensive observation period of the Tropical Ocean Global Atmosphere-Coupled Ocean Atmosphere Response Experiment (TOGA COARE). AMPR brightness temperature data were collected at a combination of frequencies (10.7, 19.35, 37.1, and 85.5 GHz) and for the period Jan. 12, 1993 - Feb. 25, 1993. The TOGA COARE geographic domain pertinent to the AMPR data set was from the equator to 21 S latitude and 145 E - 161 E longitude.

Tags: earth-science-microwave-spectral-engineering-brightness-temperature
Organization: National Aeronautics and Space Administration
ATLargeAreaSurvey(ATLAS)CDF-S&ELAIS-S11.4-GHzDR2ComponentsCatalog

This table derives from the first of two papers describing the second data release (DR2) of the Australia Telescope Large Area Survey (ATLAS) at 1.4 GHz. This survey comprises deep wide-field observations in total intensity, linear polarization, and circular polarization over the Chandra Deep Field-South (CDF-S) and European Large Area Infrared Space Observatory Survey (ELAIS)-South 1 regions. DR2 improves upon the first data release by maintaining consistent data reductions across the two regions, including polarization analysis, and including differential number counts in total intensity and linear polarization. Typical DR2 sensitivities across the mosaicked multi-pointing images are 30 &micro;Jy per beam at approximately 12 arcseconds by 6 arcseconds resolution over a combined area of 6.4 square degrees. In their paper, the authors present detailed descriptions of their data reduction and analysis procedures, including corrections for instrumental effects such as positional variations in image sensitivity, bandwidth smearing with a non-circular beam, and polarization leakage, and application of the BLOBCAT source extractor. They present the DR2 images and catalogs of components (discrete regions of radio emission) and sources (groups of physically associated radio components), and describe new analytic methods to account for resolution bias and Eddington bias when constructing differential number counts of radio components. The authors use the term &#39;component&#39; to refer to an isolated region of emission that is best described by a single 2D elliptical Gaussian. Blended regions of contiguous emission may consist of multiple individual components. Following the terminology from Hales et al. (2012, MNRAS, 425, 979), a &#39;blob&#39; is an agglomerated island of pixels above an SNR cutoff, which may encapsulate a single component or a blended region of emission. In Section 6 of the reference paper, the authors use the term &#39;source&#39; to refer to single or multiple components belonging to the same astronomical object. This HEASARC table contains the ATLAS 1.4 GHz DR2 component catalog, a portion of which is displayed in Table A1 of the reference paper for guidance regarding its form and content. The catalog lists a total of 2,588 components in total intensity and linear polarization; no components were discovered in circular polarization. A list of the ATLAS 1.4 GHz DR2 sources, a portion of which is displayed in Table B1 of the reference paper for guidance regarding its form and content, is not included in this HEASARC table. This table was created by the HEASARC in October 2014 based on an electronic version of Table A1 from the reference paper which was obtained from the MNRAS web site. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration