AndreaBozzo/ceres-open-data-index huggingface dataset:
ROSAT Bright Survey (Schwope et al. 2000)

The ROSAT Bright Survey (RBS) is an identification program of the more than 2000 X-ray sources at high galactic latitude (absolute latitude b &gt; 30 degrees) with a count rate of more than 0.2 ct/s detected during the ROSAT All-Sky Survey (Voges et al. 1999, A&amp;A, 349, 389). The RBS identification program is more than 99.5% complete. A sub-sample of 931 sources with a count rate of more than 0.2 ct/s in the hard spectral band from 0.5 to 2.0 keV is 100% identified. The total survey area comprises 20391 square degrees at a flux limit of 2.4 x 10&lt;sup&gt;-12&lt;/sup&gt; erg/s/cm&lt;sup&gt;2&lt;/sup&gt; in the 0.5 to 2.0 keV band. About 1500 sources of the complete sample were identified by correlating the RBS with the SIMBAD and NED databases. The remaining ~500 sources were identified by low-resolution optical spectroscopy and CCD imaging utilizing various telescopes. The RBS Catalog contains optical and X-ray information for each source, including the most massive complete sample of X-ray selected AGN ever assembled, with a total of 669 members, and a well-populated X-ray selected sample of 302 clusters of galaxies with redshifts of up to 0.52. Three X-ray sources in the RBS remain without optical counterparts, RBS 378, RBS 1223, and RBS 1556. While the first is a possible X-ray transient, the latter two sources are isolated neutron star candidates (Motch et al. 1999, A&amp;A, 351, 177; Schwope et al. 1999, 341, L51). As noted elsewhere, this electronic version of the RBS Catalog has a small number of additions/corrections compared to the published version. This database was created by the HEASARC in August 2000 based on a machine-readable table supplied to the HEASARC by Axel Schwope in April 2000. Note that this table is an expanded version of Table 2 in the published paper and contains the following additional parameters: HR2 (hardness_ratio_2), and the Galactic hydrogen column density (nh_21cm). This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 5 3689 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 Global Gravity measurement and covers the time 2015-01-29T04:35:43.000 to 2015-01-29T08:15:13.500.

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Organization: National Aeronautics and Space Administration
Dixon Master List of Radio Sources (Version 43)

This database table is the Dixon Master List of Radio Sources (Version 43, dated November 1981) which contains flux densities for known radio sources detected at a variety of frequencies. The Master List of Radio Sources was prepared by combining about thirty catalogs of radio sources that were available as of that date into a common format. Notice that this is a list of observations, not of individual sources, and that an entry in this table corresponds to an observation of a radio source at a particular frequency from a particular source catalog: also, no attempt was made by the author to use the same name for the same source, e.g., the source 3C 273 appears more than a dozen times under a variety of names such as PKS 1226+02, NRAO400, CTA 53, etc. This database table was recreated at the HEASARC in June 2005 after it was discovered that the positions had been incorrectly precessed. The original input table used for both the previous and current HEASARC Dixon tables was the 43rd version of the Master List, dated November 1981. It was obtained from the Colorado node of the Astrophysics Data System (ADS), the now-defunct HTTP link &lt;adswww.colorado.edu/catalogs/rad_msl43.html&gt;, and apparently was provided by D. E. Harris on or after 1991. Notice that the version of this table that is currently available at CDS (&lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/2A"&gt;https://cdsarc.cds.unistra.fr/ftp/cats/VII/2A&lt;/a&gt;) is, according to Andernach (1989, Bull. Inf. Centre Donnees Stellaires, 37, 139), the 42nd edition (dated 1976) and has only 79493 entries compared to 84510 entries in the HEASARC table. 49 duplicate entries were removed from the HEASARC table in June 2019. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
WISE All-Sky Known Solar System Object Possible Association List

NASA's Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) mapped the sky at 3.4, 4.6, 12, and 22 μm (W1, W2, W3, W4) in 2010 with an angular resolution of 6.1", 6.4", 6.5", & 12.0" in the four bands. WISE achieved 5σ point source sensitivities better than 0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodiacal background.\n\nThe All-Sky Release includes all data taken during the WISE full cryogenic mission phase, 7 January 2010 to 6 August 2010, that were processed with improved calibrations and reduction algorithms. Release data products include an Atlas of 18,240 match-filtered, calibrated and coadded image sets, a Source Catalog containing positional and photometric information for over 563 million objects detected on the WISE images, and an Explanatory Supplement that is a guide to the format, content, characteristics and cautionary notes for the WISE All-Sky Release products.\n\nThe Known Solar System Object Possible Associations List is a compendium of asteroids, comets, planets or planetary satellites, with orbits known at the time of WISE second-pass data processing, that were predicted to be within the field-of-view at the time of individual WISE exposures. Individual objects were observed multiple times, so may have multiple entries in the list. When the predicted position of a solar system object is in proximity to a detection in the WISE single-exposures, the WISE source position and brightness information are also provided. \n\nThe WISE All-Sky Data Release Single-exposure Source Working Database contains positions and brightness information, uncertainties, time of observation and assorted quality flags for 9,479,433,101 "sources" detected on the individual WISE 7.7s (W1 and W2) and 8.8s (W3 and W4) Single-exposure images. Because WISE scanned every point on the sky multiple times, the Single-exposure Database contains multiple, independent measurements of objects on the sky.\n\nEntries in the Single-exposure Source Table include detections of real astrophysical objects, as well as spurious detections of low SNR noise excursions, transient events such as hot pixels, charged particle strikes and satellite streaks, and image artifacts light from bright sources including the moon. Many of the unreliable detections are flagged in the Single-exposure Table, but they have not been filtered out as they were for the Source Catalog. Therefore, the Table must be used with caution. Users are strongly encouraged to read the Cautionary Notes before using the Table.

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Organization: National Aeronautics and Space Administration
Panchromatic Hubble Andromeda Treasury ConeSearch

The Panchromatic Hubble Andromeda Treasury is a Hubble Space Telescope Multi-cycle program to map roughly a third of M31's star forming disk, using 6 filters covering from the ultraviolet through the near infrared. With HST's resolution and sensitivity, the disk of M31 will be resolved into more than 100 million stars, enabling a wide range of scientific endeavors.\nThe PHAT observations are grouped into 23 "bricks", each listed under a different proposal ID. Each brick consists of a 3x6 array of pointings, producing complete coverage in the UV, optical, and NIR. Each brick is observed as two 3x3 "half bricks", with observations taken ~6 months apart. In the first observing season, a 3x3 half brick of WFC3 pointings is completed in primary, while parallel observations produce a highly overlapping 3x3 tile of ACS observations in the adjacent half brick. After 6 months, the telescope can be rotated by 180 degrees from the original orientation, such that the primary WFC3 pointings cover the area that was tiled by ACS in the first season, and vice versa. Each pointing is observed for 2 orbits, using the 2 WFC3 cameras for one orbit each.\nFilters: F275W+F336W (WFC3/UVIS), F475W+F814W (ACS/WFC), F110W+F160W (WFC3/IR)\nDepth: UVIS data reach a magnitude limit of ~25 in F275W and F336W. ACS data reach maximum depths of ~28 magnitudes in F475W and ~27 magnitudes in F814W in the uncrowded outer disk. In these same regions, WFC3/IR data reach maximum depths of ~26.5 and ~25.5 in F110W and F160W, respectively. However, the depth is crowding limited in the optical and NIR, and thus is a strong function of radius. As a result, photometry in the inner bulge fields is far shallower.\n\nAll available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.

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Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 7 3996 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 2019-04-17T19:45:00.000 to 2019-04-17T21:30:00.000.

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Organization: National Aeronautics and Space Administration
IRAM 30-m Single-Dish Telescope Observation Log

This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850 m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550 m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there since September 30, 2009. The observation log for the the six-antenna interferometer on the Plateau de Bure in France is also available as the HEASARC database table &lt;a href="/W3Browse/ground-based/irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;, and the observation log for NOEMA (the NOrthern Extended Millimeter Array), the successor to the Plateau de Bure observatory, is available as the HEASARC database table &lt;a href="/W3Browse/ground-based/iramnoelog.html"&gt;IRAMNOELOG&lt;/a&gt;. For more information on IRAM, see &lt;a href="http://www.iram-institute.org/"&gt;the IRAM home page&lt;/a&gt;. This table was originally ingested by the HEASARC in January 2011. It is based on the CDS table B/iram/, files 30m.dat and 30m_pi.dat. It was last updated in September 2020, based on an updated version of these tables which were also obtained from the CDS. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ARECIBO VENUS RADIO TELESCOPE RESAMPLED 12.6 CM RADAR V1.0

The Arecibo 12.6 cm radar data set for Venus consists of scaled radar backscatter cross section images generated from data obtained in 1983 and 1988. The images are in raster format (one image per record, with no embedded labels). The original images are in 16-bit, unsigned integer, most-significant-byte-first format. Since the volume of the entire set of 16-bit images would have exceeded the capacity of the CD-ROM, some of the images have been scaled to 8-bit versions. Specifically, the entire set of 1988 images are in the scaled 8-bit format, while all the 1983 images are in the original 16-bit format. Both the 16-bit and the 8-bit images were provided by Don Campbell, Cornell University.

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Organization: National Aeronautics and Space Administration
GingaBackgroundLightcurves&Spectra

The GINGABGD database table contains a summary of the contents of the Ginga pointed observations of (nominally empty) background fields. This table has been produced from the raw Ginga LAC First Reduction Files (FRFs), and contains information of the individual pointings in addition to FITS spectra and light curves, HDS and FITS data cubes and the plots produced during the pipeline processing. These products can be used with either the Ginga data analysis software or the &lt;a href="/docs/xanadu/xanadu.html"&gt;XANADU software suite&lt;/a&gt;. This archive (database and all the associated products) is a copy of the GINGABGD data products held at the Leicester Data Archive Service (&lt;a href="http://ledas-www.star.le.ac.uk/"&gt;http://ledas-www.star.le.ac.uk/&lt;/a&gt;). It was delivered to the HEASARC as part of archive exchange between data centers to facilitate the data transfer across the Atlantic. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Planck Sunyaev-Zeldovich Cluster MMF3 List

The Planck Sunyaev-Zeldovich Cluster catalogs contain a list of galaxy clusters detected through the Sunyaev-Zel'dovich effect (SZ) and consist of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such clusters. This version of the SZ catalogs, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010.\n\nThree pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalog is constructed as the union of the catalogs from the three detection methods. The individual catalogs are provided for the expert user in order to assess the consistency of the pipelines. The union catalogue contains the coordinates and the signal-to-noise ratio of the detections and a summary of the external validation information, including external identification of a cluster and its redshift if it is available.

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Organization: National Aeronautics and Space Administration
RR-1 and RR-3 mouse liver transcriptomics with and without ERCC control RNA spike-ins

Proper interpretation of RNA sequencing data requires an understanding of assay sensitivity and sources of variability. To this end, the External RNA Control Consortium (ERCC) developed a standard set of 92 poly-adenylated RNA transcripts that are orthogonal to mammalian RNA that can be added to RNA extracts before library generation and sequencing. The presence of these RNA standards at known ratios improves interpretation of RNA sequencing datasets. To test the utility of the ERCC RNA controls, total RNA extracted from mouse livers from the Rodent Research 1 (flight, ground control, basal control and vivarium control groups) and Rodent Research 3 (flight, ground control and basal control groups) missions were sequenced with and without the ERCC control RNA (RR-3 liver samples without ERCC control have been sequenced previously and the dataset is released in the GLDS-137). To allow comparison within and between groups, ERCC Mix 1 or Mix 2 were added to half of the samples from each group, respectively.

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Organization: National Aeronautics and Space Administration
HEAO 1 A2 Piccinotti Catalog

The HEAO 1 A-2 experiment&#39;s operations began on day 224 of 1977 (12 August 1977) and ended on day 739 of 1977 (9 January 1979). The A-2 experiment performed two independent, low-background, high-sensitivity surveys of the entire sky 6 months apart, the first scan during days 248 to 437 of 1977 (5 September 1977 - 13 March 1978) and the second scan during days 73 to 254 of 1978 (14 March 1978 - 11 September 1978). The authors analyzed the A-2 data in order to obtain a complete flux-limited sample of extragalactic X-ray sources. The region between galactic latitudes of -20 and +20 degrees was excluded to minimize contamination from galactic sources. A circle of 6 degrees radius around the Large Magellanic Cloud sources was also excluded to prevent confusion problems. Therefore, there remained 65.5% of the sky (8.23 steradians) covered by this survey. The lowest statistical significance for the existence of the sources included in this catalog is 5 sigma, as required by the maximum likelihood methods used by the authors to determine the log N - log S parameters. Taking into account this statistical significance requirement, the authors estimated the completeness level of the first and second scans to be 1.25 and 1.8 R15 ct/s, respectively. 1 R15 ct/s is approximately 2.17 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s in the 2-10 keV energy band for a power-law spectrum with a photon index of 1.65. This catalog contains data for 68 non-galactic sources (61 extragalactic and 7 unidentified sources) which were listed in Table 1 of the published catalog. The identified sources fall into several categories, including narrow emission line galaxies, broad emission line galaxies, BL Lacertae objects, and clusters of galaxies. This table was last revised by the HEASARC in November 2004 when 2 sources (H1257-042 and H1325-020) which had for some reason been omitted from the previous HEASARC version (the provenance of which is somewhat uncertain) were added back in to the table. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Globular Cluster Systems of Galaxies Catalog

This table contains a catalog of 422 galaxies with published measurements of their globular cluster (GC) populations. Of these, 248 are E galaxies, 93 are S0 galaxies, and 81 are spirals or irregulars. Among various correlations of the total number of GCs with other global galaxy properties, the authors find that the number of globular clusters N&lt;sub&gt;GC&lt;/sub&gt; correlates well though nonlinearly with the dynamical mass of the galaxy bulge M&lt;sub&gt;dyn&lt;/sub&gt; = 4 sigma _e_&lt;sup&gt;2&lt;/sup&gt; R&lt;sub&gt;e&lt;/sub&gt;/G, where sigma&lt;sub&gt;e&lt;/sub&gt; is the central velocity dispersion and R&lt;sub&gt;e&lt;/sub&gt; the effective radius of the galaxy light profile. In their paper, the authors also present updated versions of the GC specific frequency S&lt;sub&gt;N&lt;/sub&gt; and specific mass S&lt;sub&gt;M&lt;/sub&gt; versus host galaxy luminosity and baryonic mass. These graphs exhibit the previously known U-shape: highest S&lt;sub&gt;N&lt;/sub&gt; or S&lt;sub&gt;M&lt;/sub&gt; values occur for either dwarfs or supergiants, but in the mid-range of galaxy size (10&lt;sup&gt;9&lt;/sup&gt; - 10&lt;sup&gt;10&lt;/sup&gt; L&lt;sub&gt;sun&lt;/sub&gt;) the GC numbers fall along a well-defined baseline value of S&lt;sub&gt;N&lt;/sub&gt; ~= 1 or S&lt;sub&gt;M&lt;/sub&gt; = 0.1, similar among all galaxy types. Along with other recent discussions, the authors suggest that this trend may represent the effects of feedback, which systematically inhibited early star formation at either very low or very high galaxy mass, but which had its minimum effect for intermediate masses. Their results strongly reinforce recent proposals that GC formation efficiency appears to be most nearly proportional to the galaxy halo mass M&lt;sub&gt;halo&lt;/sub&gt;. The mean &quot;absolute&quot; efficiency ratio for GC formation that the authors derive from the catalog data is M&lt;sub&gt;GCS&lt;/sub&gt;/M&lt;sub&gt;halo&lt;/sub&gt; = 6 x 10&lt;sup&gt;-5&lt;/sup&gt;. They suggest that the galaxy-to-galaxy scatter around this mean value may arise in part because of differences in the relative timing of GC formation versus field-star formation. Finally, they find that an excellent empirical predictor of total GC population for galaxies of all luminosities is N&lt;sub&gt;GC&lt;/sub&gt; ~ (R&lt;sub&gt;e&lt;/sub&gt; sigma&lt;sub&gt;e&lt;/sub&gt;)&lt;sup&gt;1.3&lt;/sup&gt;, a result consistent with fundamental plane scaling relations. This table was created by the HEASARC in February 2014 based on an electronic version of Table 1 from the reference paper which was obtained from the ApJ web site. A duplicate entry for NGC 4417 was removed in June 2019. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Upper Sco XMM-Newton X-Ray Point Source Catalog

The authors studied the X-ray emission from young stars by analyzing the deep (a ~53 ks exposure centered at a J2000.0 RA and Dec of 16 14 00.0, -23 00 00 and a ~43 ks exposure at 15 56 25.0, -23 37 47) XMM-Newton observations of two regions of the Upper Scorpius (USco) subgroup of the Scorpius-Centaurus (Sco-Cen) association which is estimated to have an age of 5 Myr. Portions of the USco association were observed in the optical with the CTIO Curtis Schmidt telescope and the Danish 1.54m telescope. This table contains all the X-ray sources detected in the two XMM-Newton observations, as well as their near-IR counterparts from the 2MASS and DENIS catalogs, and their optical counterparts from the CTIO and Danish 1.54 m observations. Based on the near-infrared and optical photometry, 22 Upper Scorpius photometric members have been identified among the 224 detected X-ray sources. This table was created by the HEASARC in March 2007 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/459/199"&gt;CDS catalog J/A+A/459/199&lt;/a&gt; files tabled1.dat and table2.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
VG1 J/S/SS PWS EDITED SPECTRUM ANALYZER FULL RES V1.0

This data set includes nearly all measurements collected from the     spectrum analyzer component of the Plasma Wave Spectrometer (PWS)     onboard Voyager 1 for the entire mission.  Some noise lines during the     planetary encounters have been edited from the data set.  Each sweep of     the PWS spectrum analyzer records spectral densities in 16 frequency     channels from 50 Hz to 10 kHz.  The values in this data set are given     as instrument data numbers.  Instructions for producing calibrated     values are provided.  An example C-language program which reads this     data set and produces calibrated values is also provided.

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Organization: National Aeronautics and Space Administration