AndreaBozzo/ceres-open-data-index huggingface dataset:
NEW HORIZONS      PEPSSI KEM2      RAW V1.0

This data set contains Raw data taken by the      New Horizons Pluto Energetic Particle Spectrometer Science Investigation      instrument during the KEM1 ENCOUNTER and KEM2 CRUISE mission      phases. This is VERSION 1.0 of this data set.      This version includes data acquired by the spacecraft between      08/14/2018 and 04/10/2023. It only includes data downlinked before      05/01/2023 and after 04/30/2023. Future datasets may include more data      acquired by the spacecraft after 08/13/2018 but downlinked after      04/30/2023.      This dataset contains observations from prior to, during, and after      the ASTEROID 486958 Arrokoth (2014 MU69) encounter.

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Organization: National Aeronautics and Space Administration
VLA Subaru/XMM-Newton Deep Field 1.4-GHz Sources Optical/Near-IR Counterparts

In Simpson et al. (2006, MNRAS, 372, 741, hereafter Paper I, available at the HEASARC as the &lt;a href="/W3Browse/radio-catalog/vlasxdf1p4.html"&gt;VLASXDF1P4&lt;/a&gt; table, the authors presented a catalog of 505 sources with 1.4-GHz peak radio flux densities greater than 100 uJy over a 0.81 deg&lt;sup&gt;2&lt;/sup&gt; region of the Subaru/XMM-Newton Deep Field (SXDF) and some of the properties of their optical counterparts. In this study (Simpson et al. 2012, MNRAS, 421, 3060, Paper III in the series) the authors present spectroscopic and 11-band photometric redshifts for galaxies in the 100-uJy Subaru/XMM-Newton Deep Field radio source sample. The authors find good agreement between their redshift distribution and that predicted by the Square Kilometre Array (SKA) Simulated Skies project. They find no correlation between K-band magnitude and radio flux, but show that sources with 1.4-GHz flux densities below ~ 1 mJy are fainter in the near-infrared than brighter radio sources at the same redshift, and they discuss in their paper the implications of this result for spectroscopically incomplete samples where the K-z relation has been used to estimate redshifts. The authors use the infrared-radio correlation to separate their sample into radio-loud and radio-quiet objects and show that only radio-loud hosts have spectral energy distributions consistent with predominantly old stellar populations, although the fraction of objects displaying such properties is a decreasing function of radio luminosity. Many of the spectra presented in this study were obtained as part of the European Southern Observatory (ESO) program P074.A-0333, undertaken using the Visible Multi-Object Spectrograph (VIMOS) instrument on UT3/Melipal. Several observational campaigns have obtained spectra of objects within the SXDF, and Paper II in this series (Vardoulaki et al. 2008, MNRAS, 387, 505) presented spectra for 28 of the brightest 37 radio sources, obtained from a variety of sources. The near-infrared data used here come from the third data release (DR3) of the UKIRT (United Kingdom Infrared telescope) Infrared Deep Sky Survey, while the optical data in the UDS come from the SXDF, which comprises five separate Suprime-Cam pointings. This table was created by the HEASARC in August 2013 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/421/3060"&gt;CDS Catalog J/MNRAS/421/3060&lt;/a&gt; file table1.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
NEW HORIZONS  ALICE PLUTO CRUISE  RAW V2.0

This data set contains Raw data taken by the New Horizons  Alice Ultraviolet Imaging Spectrograph  instrument during the  pluto cruise  mission phase. This is VERSION 2.0 of this data set.   ALICE Activities Overview at Annual CheckOuts (ACOs) during the  Pluto Cruise mission phase started with the standard WakeUp  sequence (memory/code checks, aperture door performance test,  pixelhack issue verification, 24 hours of decontamination and  three one hour dark observations) and finished with the standard  Button-Up sequence (code and parameter refresh). Other activities  (with targets as noted) were calibrations for flux (Spica,  rho-Leo, gamma-Grus, HD93521, Sun in Solar OCcultation Channel,  SOCC), flatfield (rho-Leo), airglow scattered light and SOCC  pointing calibrations (Spica, zeta-Pup), SOCC flat (Sun), dark sky  stares, spinning dark observations (in some cases the Sun strobes  through the slit), pointing and short wavelength calibration  (HD93521), InterPlanetary Medium (IPM) histograms and pixellist  observations, dual target tests (HD214680 : 8 Lac, HD214168 : 10  Lac), MEV Solar Wind (HEET) baseine observation, Pluto encounter  rehearsals, and instrument interference tests.   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 IPM  histogram scans in December, 2014, which failed.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 3 0870 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 2015-07-01T03:27:20.000 to 2015-07-01T04:55:17.000.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER MARS OSINAC 2 MARS EDR V2.0

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 MARS SWING-BY mission phase, covering the period  from 2006-07-29T00:00:00.000 to 2007-05-28T23:59:59.000. The prime target is planet Mars. This version V2.0 supersedes previous deliveries of the same dataset with the following changes since the last version: Reprocessed dataset after October 2018 PSA/PDS external peer review.

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Organization: National Aeronautics and Space Administration
MassiveYoungStar-FormingComplexStudyinIR&X-Rays:IR-ExcessSources

The Massive Young Star-Forming Complex Study in Infrared and X-rays (MYStIX) project provides a comparative study of 20 Galactic massive star-forming complexes with distances between 0.4 and 3.6 kpc. Probable stellar members in each target complex are identified using X-ray and/or infrared data via two pathways: (1) X-ray detections of young/massive stars with coronal activity/strong winds or (2) infrared excess (IRE) selection of young stellar objects (YSOs) with circumstellar disks and/or protostellar envelopes. In this particular study, the authors present the methodology for the second pathway using Spitzer/IRAC, 2MASS, and UKIRT imaging and photometry. Although IRE selection of YSOs is well-trodden territory, MYStIX presents unique challenges. The target complexes range from relatively nearby clouds in uncrowded fields located toward the outer Galaxy (e.g., NGC 2264, the Flame Nebula) to more distant, massive complexes situated along complicated, inner Galaxy sightlines (e.g., NGC 6357, M 17). The authors combine IR spectral energy distribution (SED) fitting with IR color cuts and spatial clustering analysis to identify IRE sources and to isolate probable YSO members in each MYStIX target field from the myriad types of contaminating sources that can resemble YSOs: extragalactic sources, evolved stars, nebular knots, and even unassociated foreground/background YSOs. Applying their methodology consistently across 18 of the target complexes, they produce the MYStIX IRE Source (MIRES) Catalog comprising 20,719 sources, including 8,686 probable stellar members of the MYStIX target complexes. They also classify the SEDs of 9,365 IR counterparts to MYStIX X-ray sources to assist the first pathway, the identification of X-ray-detected stellar members. The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26), provides a comprehensive, parallel study of 20 Galactic massive star-forming regions. The basic input data for the MIRES Catalog were near-IR (NIR) and mid-IR (MIR) photometric catalogs. The authors also used NIR and MIR images and mosaics for visualizing the point-source populations with respect to various nebular structures. They provide high-level descriptions of each input catalog in section 2 of the reference paper. This table contains the MYStIX IRE Source (MIRES) Catalog comprising IR data on 20,719 sources, including 8,686 probable stellar members of the MYStIX target complexes, viz., massive star-forming regions (MSFRs), which was given in Table 2 of the reference paper. It does not include the IR data of the above-mentioned 9,365 IR counterparts to MYStIX X-ray sources (the SED Classification of IR Counterparts to MYStIX X-ray sources (SCIM-X Catalog) that were listed in Table 7 of the reference paper. This table was created by the HEASARC in February 2014 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/31"&gt;CDS Catalog J/ApJS/209/31&lt;/a&gt; file table2.dat. 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 6 3882 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 2017-01-08T20:47:01 to 2017-01-08T21:32:00.

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Organization: National Aeronautics and Space Administration
SSA22 Field Chandra X-Ray Point Source Catalog

This table contains the main X-ray point-source catalog for a deep ~400-ks Chandra ACIS-I (Advanced CCD Imaging Spectrometer) exposure of the SSA22 field. The observations were centred on a z = 3.09 protocluster, which is populated by Lyman break galaxies (LBGs), Lyman-alpha emitters (LAEs) and extended Lyman-alpha-emitting blobs (LABs). The survey reached ultimate (3 count) sensitivity limits of ~5.7 x 10&lt;sup&gt;-17&lt;/sup&gt; and ~3.0 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the 0.5-2 and 2-8 keV bands, respectively (corresponding to L(2-10 keV) ~ 5.7 x 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and L(10-30 keV) ~ 2.0 x 10&lt;sup&gt;43&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; at z = 3.09, respectively, for an assumed photon index of Gamma = 1.4). These limits make SSA22 the fourth deepest extragalactic Chandra survey yet conducted, and the only one focused on a known high-redshift structure. In total, the authors detect 297 X-ray point sources and identify one obvious bright extended X-ray source (not included in the current table) over a ~330 arcmin&lt;sup&gt;2&lt;/sup&gt; region. In addition to the X-ray data, the authors provide all available optical spectroscopic redshifts and near-infrared and mid-infrared photometry available for their sources. The basic X-ray and infrared properties of their Chandra sources indicate a variety of source types, although absorbed active galactic nuclei (AGN) appear to dominate. In total, they have identified 12 X-ray sources (either via optical spectroscopic redshifts or LAE selection) at z = 3.06 - 3.12 that are likely to be associated with the SSA22 protocluster. These sources have X-ray and multiwavelength properties that suggest they are powered by AGN with 0.5 - 8 keV luminosities in the range of ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;45&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. The authors have analysed the AGN fraction of sources in the protocluster as a function of local LAE source density and find suggestive evidence for a correlation between AGN fraction and local LAE source density (at the ~96 per cent confidence level), implying that supermassive black hole growth at z ~3 is strongest in the highest density regions. This table was created by the HEASARC in February 2010 based on the electronic version of Table 2 from the reference paper which was obtained from the Monthly Notices web site. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
Chandra COSMOS (C-COSMOS) Survey X-Ray Point Source Catalog

The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.5 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS field (centered at RA, Dec of 10 hours , +02 degrees) with an effective exposure of ~ 160 ks, and an outer 0.4 deg&lt;sup&gt;2&lt;/sup&gt; area with an effective exposure of ~ 80 ks. The limiting source detection depths are 1.9 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; in the soft (0.5 - 2 keV) band, 7.3 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; in the hard (2 - 10 keV) band, and 5.7 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; in the full (0.5 - 10 keV) band. In this paper, the authors describe the strategy, design, and execution of the C-COSMOS survey, and present the catalog of 1761 point sources detected at a probability of being spurious of &lt; 2 x 10&lt;sup&gt;-5&lt;/sup&gt; (1655 in the full, 1340 in the soft, and 1017 in the hard bands). By using a grid of 36 heavily (~ 50%) overlapping pointing positions with the ACIS-I imager, a remarkably uniform (+/-12%) exposure across the inner 0.5 deg&lt;sup&gt;2&lt;/sup&gt; field was obtained, leading to a sharply defined lower flux limit. The widely different point-spread functions obtained in each exposure at each point in the field required a novel source detection method, because of the overlapping tiling strategy, which is described in a companion paper. This method produced reliable sources down to a 7-12 counts, as verified by the resulting log N-log S curve, with sub-arcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper. Supporting data products for this table (including images, event files, and exposure maps) are available at the &lt;a href="https://cosmos.astro.caltech.edu/page/xray/"&gt;COSMOS Survey website&lt;/a&gt; and at &lt;a href="https://irsa.ipac.caltech.edu/data/COSMOS/"&gt;IRSA&lt;/a&gt;. At the IRSA website, it is also possible to search a database that includes &quot;postage stamps&quot; of the X-ray data for each source, along with the multi-wavelength optical and infrared data, including the I-band, K-band, and Spitzer 3.6-micron (Band 1) images used in the Part III paper (Civano et al. 2012) to identify the sources. See also the related table &lt;a href="ccosmosoid.html"&gt;CCOSMOSOID&lt;/a&gt; for the optical and infrared identifications of the surveyed X-ray point sources. This table was created by the HEASARC in November 2009 based on an electronic version of the C-COSMOS Catalog which was obtained from the Astrophysical Journal web site. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 2002T7/CAL/CHECK ALICE 3 CVP1 V1.0

This data set contains CODMAC level 3 cometary, calibration, and instrument checkout data acquired by the Rosetta Orbiter ALICE UV Spectrometer during the first commissioning phase of the Rosetta mission, which occurred March 5, 2004 to June 6, 2004.

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Organization: National Aeronautics and Space Administration
GLIMPSE 360 Archive

GLIMPSE360 is a Warm Mission Spitzer Cycle 6 Exploration Science Program (PIDs 60020, 61070, 61071, 61072, 61073, 70072) that mapped 187 degrees of longitude of the Galactic plane that have not been mapped by previous Spitzer Galactic Plane surveys (GLIMPSE, GLIMPSEII, GALCEN, GLIMPSE3D, Vela Carina, SMOG and Cygnus-X). The specific Galactic longitudes covered by GLIMPSE360 are l=65◦-76◦, 82◦-102◦, and 109◦-265◦. The latitude range is about 2.8◦. The latitude center follows the Galactic warp. GLIMPSE360 completes the full circle of the Galactic plane.\n\nThe GLIMPSE360 Archive (GLM360A or the “Archive”) consists of point sources with less stringent selection critera than the Catalog. The information provided is in the same format as the Catalog. The Catalog is a subset of the Archive, but the entries for a particular source might not be the same due to additional nulling of magnitudes in the Catalog because of the more stringent requirements.

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Organization: National Aeronautics and Space Administration
20cm Radio Catalog

The 1.4-GHz Northern Sky Catalog - Version: 4 December 1991 This is the 20-cm Northern Sky Catalog of White, R. L. and Becker, R. H. (1992, Ap.J.Supp., in press) containing 30,239 sources detected from the Condon Greenbank images taken at 1.4 GHz over the declination range of -5 degrees to 82 degrees with a flux density limit of 100 mJy. This 20 cm catalog also contains the results of a cross-correlation with catalogs at 6 and 80 cm covering the northern sky between Dec=0 degrees and 70 degrees to give the spectral indices at three frequencies for about 20,000 sources. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 4 EXT3-MTP033 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 Wide Angle Camera on the Rosetta spacecraft during the ROSETTA EXTENSION 3 mission phase, covering the period from 2016-08-09T23:25:00.000 to 2016-09-02T06:39:59.000. 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.

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Organization: National Aeronautics and Space Administration
Wisconsin Ultraviolet Photo-Polarimeter Experiment

The Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE) was the spectropolarimetry component of the three ASTRO instruments that flew on Space Shuttle missions in December 1990 and March 1995. A halfwave spectropolarimeter provided medium resolution spectropolarimetry for research into the interstellar medium, hot stars, stars with circumstellar material, interacting binary stars, novae, solar system objects, and active galaxies. A Lyot analyzer obtained low resolution observations of faint targets, but due to calibration problems did not produce scientifically useful data. The WUPPE instrument provides a unique data set, one of the few providing polarimetric data in the ultraviolet portion of the spectrum.

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Organization: National Aeronautics and Space Administration
GLIMPSE 3D Catalog

GLIMPSE3D is the third in a series of large area projects to map selected regions of the Galactic plane using the Spitzer Space Telescope Infrared Array Camera (IRAC). GLIMPSEI1 covered the Galactic plane from |l| = 10◦ to 65◦ and |b| < 1◦; GLIMPSEII filled in the inner 20 degrees of the Galactic plane, |l| < 10◦, with vertical extensions up to ±1.5◦ for |l| =5◦to 2◦, and up to ±2◦ from |l| =2◦to 0◦. GLIMPSE3D adds vertical extensions, generally up to |b| < 3◦, but up to |b| < 4.2◦ in the center of the Galaxy. The goal of this coverage is to provide data to study the vertical stellar and interstellar\n\nThe GLIMPSE3D Archive (GLM3DA or the “Archive”) consists of point sources with a signal- to-noise > 5 in at least one band and less stringent selection critera than the Catalog. The photometric uncertainty is typically < 0.3 mag. The GLIMPSE3D Catalog is a subset of the Archive, but note that the entries for a particular source might not be the same due to additional nulling of magnitudes in the Catalog because of the more stringent requirements.

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Organization: National Aeronautics and Space Administration
Hi-GAL 500 micron Photometric Catalog

The Herschel infrared Galactic Plane Survey (Hi-GAL) covers the Galactic plane at five wavelengths from 70 to 500 microns. Hi-GAL DR1 is limited to the inner Milky Way in the longitude range +68d > l > -70d and latitude range 1d > b > -1d. The generation of the Hi-GAL photometric catalogs is discussed in detail in Molinari et al. (2016).

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Organization: National Aeronautics and Space Administration
Spitzer Deep Wide-Field Survey 3.6 micron Epoch 1 Catalog

The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 square degrees in the Boötes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit - for the first time - the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ~ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ~ 1.5.\n\nThe delivery consists of four band-matched catalogs for each of the four epochs and for the total SDWFS coadd data, a total of 20 catalogs. Vega magnitudes are reported for each IRAC band: 3.6, 4.5, 5.8, and 8 microns. Each source was measured three ways: 4 arcsec diameter aperture, 6 arcsec diameter aperture, and Kron radius aperture (MAG_AUTO in SExtractor). Source coordinates correspond to 2MASS catalog positions to within 0.2 arcsec. The tabulated uncertainties are twice the SExtractor (statistical only) uncertainties as an attempt to account for systematic uncertainties.

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Organization: National Aeronautics and Space Administration
FEPS Photometry Catalog

The Formation and Evolution of Planetary Systems (FEPS) Spitzer Legacy program was designed to char- acterize the evolution of circumstellar gas and dust around solar- type stars between ages of 3 Myr and 3 Gyr. To achieve these goals, FEPS obtained spectrophotometric observations with the Spitzer Space Telescope for a sample of 328 stars (see Meyer et al. 2006 for a description of the sample). The observing strategy was to measure the spectral energy distribution (SED) between wavelengths of 3.6 and 70 um with IRAC  and MIPS photometry, and between 8 and 35 um with low-resolution IRS spectra.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER SW RPCLAP 3RVM1 CALIB2 V1.0

This data set containsCALIBRATED data from Rosetta RPC-LAP, acquired during the RENDEZVOUSMANOEUVRE 1 mission phase where the primary target was the SOLAR WIND.It contains instrument outputs in volts and amperes, calibrated andcorrected for instrument offsets.

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Organization: National Aeronautics and Space Administration
Spitzer Wide-area InfraRed Extragalactic Survey ELAIS-S1 MIPS 160 micron Catalog

The Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), the largest Spitzer Legacy program, is a wide-area, imaging survey to trace the evolution of dusty, star-forming galaxies, evolved stellar populations, and AGN as a function of environment, from redshifts z~3 to the current epoch. SWIRE surveys 6 high-latitude fields, totaling ~50 sq. deg. in all 7 Spitzer bands: 3.6, 4.5, 5.8, and 8 microns with IRAC and 24, 70, and 160 microns with MIPS (Lonsdale et al. 2003). The SWIRE Legacy Extragalactic Source Catalogs will eventually contain in excess of 2 million IR-selected galaxies, from those dominated by the light of stellar populations detected primarily by IRAC, to starbursts, ultra-luminous infrared galaxies and AGN detected also by MIPS.

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Organization: National Aeronautics and Space Administration