AndreaBozzo/ceres-open-data-index huggingface dataset:
eROSITA eFEDS Hard X-Ray (2.3-5.0 keV) Source Catalog

The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory combines a large field of view and collecting area in the energy range ~0.2 to ~8.0 keV with the capability to perform uniform scanning observations of large sky areas. SRG/eROSITA performed scanning observations of the ~140 square degrees eROSITA Final Equatorial Depth Survey (eFEDS) field as part of its performance verification phase. The observing time was chosen to slightly exceed the depth of equatorial fields after the completion of the eROSITA all-sky survey. The authors present a catalog of detected X-ray sources in the eFEDS field providing source positions and extent information, as well as fluxes in multiple energy bands and document a suite of tools and procedures developed for eROSITA data processing and analysis, validated and optimized by the eFEDS work. A multi-stage source detection procedure was optimized and calibrated by performing realistic simulations of the eROSITA eFEDS observations. The authors cross-matched the eROSITA eFEDS source catalog with previous XMM-ATLAS observations, confirming excellent agreement of the eROSITA and XMM-ATLAS source fluxes. This table presents the hard band sample of 246 sources detected in the energy range 2.3-5.0 keV above a detection likelihood of 10. These sources were detected in three bands (0.2-0.6, 0.6-2.3, and 2.3-5keV) with detect_likelihood &gt;=5 and extent_likelihood = 0 (i.e. point sources). The linked &lt;a href="/W3Browse/erosita/efedsmain.html"&gt;EFEDSMAIN&lt;/a&gt; table presents the primary catalog of 27910 X-ray sources, including 542 with significant spatial extent, detected in the 0.2-2.3 keV energy range with detection likelihoods &gt;=6 , corresponding to a (point source) flux limit of ~6.5 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s in the 0.5-2.0 keV energy band (80% completeness). A supplementary catalog contains 4774 low-significance source candidates with detection likelihoods between 5 and 6. The dedicated data analysis software package, calibration database, and calibrated data products are described in an appendix. Additional information for the eROSITA early data release observations is available at the &lt;a href="https://erosita.mpe.mpg.de/edr/"&gt;eROSITA-DE EDR website&lt;/a&gt;. This database table was originally ingested by the HEASARC in August 2022 and is based upon the &quot;eROSITA/eFEDS hard catalogue&quot; file downloaded from the eROSITA-DE Early Data Release &lt;a href="https://erosita.mpe.mpg.de/edr/eROSITAObservations/Catalogues/"&gt;catalogs web page&lt;/a&gt;. It was revised in June 2024 in order to rename the right ascension, declination, and their related positional uncertainty parameters to match the parameter naming convention used in other eROSITA catalogs. In some cases, the HEASARC has altered the original field names, as per HEASARC conventions, and provides the original field names in square brackets. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ULY JUP SCE DOPPLER HI-RES DATA

The Ulysses spacecraft was occulted by                                      the Io Plasma Torus (IPT) during its                                      Jupiter encounter on 8 February 1992.                                      The Ulysses dual-frequency radio                                      subsystem used by the Ulysses Solar                                      Corona Experiment (SCE) was utilized                                      to measure the electron content                                      (column density) of the IPT. In the                                      nominal mode for radio-sounding                                      observations, both downlinks                                      (S-band: f_s = 2.3 GHz X-band:                                      f_x = 8.4 GHz) are phase coherent with                                      the uplink (S-band: f_u = 2.1 GHz).                                      The dual-frequency radio-sounding                                      technique exploits the dispersive                                      nature of ionized media on the                                      propagation of the two downlinks. The                                      tiny Doppler shift due to plasma                                      moving in and out of the ray path is                                      greater at S-band than at the higher                                      frequency X-band.

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Organization: National Aeronautics and Space Administration
Spitzer Extragalactic First Look Survey WIYN/Hydra Line Strength and Equivalent Width Catalog

The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared. \n\nThis catalog presents line strength and equivalent width measurements from the WIYN/Hydra spectra described in Marleau et al. (2007).

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Organization: National Aeronautics and Space Administration
Merged Catalog of Reflection Nebulae

Several catalogs of reflection nebulae have been merged to create a uniform catalog of 913 objects. It contains revised coordinates, cross-identifications of nebulae and stars, as well as identifications with IRAS point sources. The HEASARC has endeavored to render all identifications of the nebulae in the various catalogs according to the styles recommended by the Dictionary of Nomenclature of Celestial Objects. This table was created by the HEASARC in October 2012 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/399/141"&gt;CDS Catalog J/A+A/399/141&lt;/a&gt; file table1.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 4 PRL-MTP001 RDR V2.0

This CODMAC level 4 data set contains radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm, acquired by the OSIRIS Wide Angle Camera on the Rosetta spacecraft during the PRELANDING mission phase, covering the period from 2014-01-20T10:00:00.000 to 2014-05-07T12:47:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V2.0 supersedes previous deliveries of the same dataset with the following changes since the last version: Lien corrected dataset after October 2018 PSA/PDS external peer review. 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.

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Organization: National Aeronautics and Space Administration
ROSAT XUV Pointed Phase

We present a catalogue of XUV sources from observations by the Wide Field Camera (WFC) on ROSAT during the pointed phase. The ROSAT WFC is a telescope sensitive in the extreme UV range (17-210eV) which observes in parallel with the ROSAT X-Ray Telescope (XRT). The 5916 pointed observations processed are from the calibration and verification phase in June 1990 and from the period 9 Feb. 1991 to 15 July 1994. The catalogue contains 1022 independent source detections which correspond to 328 individual sources, many of which have been observed repeatedly. Each observation was done with one of four filters S1, S2, P1 and P2. Of the 328 sources 113 are new sources (they are not listed in the &quot;2RE&quot; catalogue) and 274 have been identified with optical counterparts. The catalogue contains coordinates, observed count rates, normalized source count rates and the proposed optical counterpart with its spectral class. 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 COMET ESCORT 4 1270 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 4 phase 2015-10-22 to 2015-12-31. It is a Global Gravity measurement at the comet 67P and covers the time 2015-12-20T01:36:25.000 to 2015-12-20T06:43:34.000.

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Organization: National Aeronautics and Space Administration
Australia Telescope Compact Array AKARI Deep Field South 20-cm Source Catalog

The results of a deep radio survey at a wavelength of 20 cm are reported for a region containing the AKARI Deep Field South (ADF-S) near the South Ecliptic Pole (SEP), using the Australia Telescope Compact Array (ATCA). The survey (hereafter referred to as the ATCA-ADFS survey) has 1-sigma detection limits ranging from 18.7 to 50 microJansky per beam (&micro;Jy/beam, over an area of ~1.1 deg&lt;sup&gt;2&lt;/sup&gt;, and ~2.5 deg&lt;sup&gt;2&lt;/sup&gt; to lower sensitivity. The observations, data reduction and source count analysis are presented in the paper, along with a description of the overall scientific objectives, and a catalog containing 530 radio sources detected with a resolution of 6.2 x 4.9 arcseconds (contained herein). The AKARI Deep Field South survey was primarily made in the far-infrared at wavelengths of 65, 90, 140, 160 micron (&micro;m) over a 12 deg&lt;sup&gt;2&lt;/sup&gt; area with the AKARI Far-Infrared Surveyor (FIS) instrument, with shallower mid-infrared coverage at 9 and 18 um using the AKARI Infrared Camera (IRC) instrument. In addition to the wide survey, deeper mid-infrared pointed observations, using the IRC, covering ~0.8 deg&lt;sup&gt;2&lt;/sup&gt; and reaching 5-sigma sensitivities of 16, 16, 74, 132, 280 and 580 uJy at 3.2, 4.6, 7, 11, 15 and 24 um, respectively, were also carried out. The radio observations were collected over a 13 day period in 2007 July using the ATCA operated at 1.344 and 1.432 GHz. The total integration time for the 2007 observations was 120 hours. The 2007 data were augmented with a further deep observation made in 2008 December over five nights towards a single pointing position at the ADF-S, which lay just off center of the larger ATCA-ADFS field reported here. This added a further 50 h of integration time. The data were processed in exactly the same way as that from the 2007 observing sessions. Note that in the terminology of the authors, a radio component is described as a region of radio emission represented by a Gaussian shaped object in the map. Close radio doubles are represented by two Gaussians and are deemed to consist of two components, which make up a single source. A selection of radio sources with multiple components is shown in Fig. 3 of the reference paper. This table was created by the HEASARC in November 2013 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/427/1830"&gt;CDS Catalog J/MNRAS/427/1830&lt;/a&gt; file table2.dat. 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 COMET ESCORT 2 0868 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 2 phase 2015-03-11 to 2015-06-30. It is a Global Gravity measurement at the comet 67P and covers the time 2015-06-30T10:12:15.000 to 2015-06-30T11:37:47.000.

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Organization: National Aeronautics and Space Administration
NGC 2516 Cluster XMM-Newton X-Ray Point Source Catalog

This table contains the results from a deep X-ray survey of the young (~ 140 Myr), rich open cluster NGC 2516 obtained with the EPIC camera on board the XMM-Newton satellite. By combining the data from six observations, a high sensitivity, greater than a factor of 5 with respect to recent Chandra observations, has been achieved. Kaplan-Meier estimators of the cumulative X-ray luminosity distribution, statistically corrected for non-member contaminants, were built by the authors and compared to those of the nearly coeval Pleiades cluster. 431 X-ray sources were detected, and 234 of them have as optical counterparts cluster stars spanning the entire NGC 2516 main sequence. On the basis of X-ray emission and optical photometry, 20 new candidate members of the cluster have been identified; at the same time there are 49 X-ray sources without known optical or infrared counterpart. The X-ray luminosities of cluster stars span the range log L&lt;sub&gt;x&lt;/sub&gt; (erg s&lt;sup&gt;-1&lt;/sup&gt;) = 28.4 - 30.8. The representative coronal temperatures span the 0.3 - 0.6 keV (3.5 - 8 MK) range for the cool component and 1.0 - 2.0 keV (12 - 23 MK) for the hot one; similar values were found in other young open clusters like the Pleiades, IC 2391, and Blanco 1. While no significant differences were found in their X-ray spectra, NGC 2516 solar-type stars are definitely less luminous in X-rays than their nearly coeval Pleiades counterparts. The comparison with a previous ROSAT survey reveals the lack of variability amplitudes larger than a factor of 2 in solar-type cluster stars in a ~ 11 yr time scale, and thus activity cycles like in the Sun are probably absent or have a different period and amplitude in young stars. NGC 2516 has been observed several times with XMM-Newton during the first two years of satellite operations for calibration purposes. The observations used in this analysis span a period of 19 months with exposure times between 10 and 20 ks. All of these observations have been performed with the thick filter. In the combined EPIC datasets the authors detected 431 X-ray sources with a significance level greater than 5.0 sigma, which should lead statistically to at most one spurious source in the field of view. This table was created by the HEASARC in May 2007 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/450/993"&gt;CDS catalog J/A+A/450/993&lt;/a&gt; files tablea1.dat and tableb1.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 4 PRL-MTP007 RDR V2.0

This CODMAC level 4 data set contains radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm, acquired by the OSIRIS Wide Angle Camera on the Rosetta spacecraft during the PRELANDING mission phase, covering the period from 2014-09-02T10:00:00.000 to 2014-09-23T09:59:59.000. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V2.0 supersedes previous deliveries of the same dataset with the following changes since the last version: Lien corrected dataset after October 2018 PSA/PDS external peer review. 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.

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Organization: National Aeronautics and Space Administration
IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog

This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/246"&gt;CDS Catalog II/246&lt;/a&gt;) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively. This table was created by the HEASARC in October 2011 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/362/1065"&gt;CDS Catalog J/MNRAS/362/1065&lt;/a&gt; files table1.dat, table2.dat and table3.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 4 3587 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 2013-06-13T00:14:04.000 to 2013-06-13T02:59:30.500.

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Organization: National Aeronautics and Space Administration
SAGE MIPS 70 micron Full List

The Spitzer Space Telescope Survey of the Large Magellanic Cloud Legacy Project Surveying the Agents of a Galaxy's Evolution (SAGE) traces the life cycle of observable matter that drives the evolution of a galaxy's appearance. SAGE has revealed over 6 million sources including ~150,000 evolved stars, ~50,000 young stellar objects and the diffuse interstellar medium with column densities > 1.2×1021 cm -2. The data will provide fundamental insights into the physical processes of the interstellar medium, the formation of new stars and the injection of mass by evolved stars and their relationships on the galaxy-wide scale of the Large Magellanic Cloud.\n\nTo be included in a Catalog, each source has to meet a number of criteria. The source had to be nearly point like with a correlation value 0.89. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. There are a small number of sources with 24 um magnitudes between 4 and 8 which have unusually low uncertainties (i.e., high S/N). The origin of these sources is under investigation and seems to be related to edge effects in the AORs. In the meantime, these sources were removed from the 24 um catalogs. Finally, all sources had to have signal-to-noise values >5. The final catalogs likely have a few remaining unreliable sources, but we estimate this to be at the less than 1% error.\n\nThe Full Lists contain ALL the sources extracted from the mosaics, thus a user should be aware that it contains spurious sources. The full list may be useful to search for the potential counterparts to known sources.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P VIRTIS 2 PRELANDING MTP007 V1.0

This release contains the digital numbers (DN) contained in the telemetry (TM) packages of the VIRTIS instrument on board of the spacecraft Rosetta. This volume contains data at the vicinity of comet 67P, from the PRELANDING MTP007 phase, which occurred from 2014-09-02 to 2014-09-23

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 4 1161 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 4 phase 2015-10-22 to 2015-12-31. It is a Global Gravity measurement at the comet 67P and covers the time 2015-11-07T05:28:29.500 to 2015-11-07T12:29:04.000.

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Organization: National Aeronautics and Space Administration
7C(G) 151-MHz Northern Galactic Plane Survey Catalog

Results from a survey of the northern Galactic plane (at Declination &gt;= 30&lt;sup&gt;o&lt;/sup&gt; at 151 MHz made with the Cambridge Low Frequency Synthesis Telescope (CLFST) are presented in this table. This survey was designated the 7C(G) - i.e. the Galactic portion of the then-ongoing 7C surveys. The 7C(G) covers the regions 80&lt;sup&gt;o&lt;/sup&gt; &lt; l &lt; 104&lt;sup&gt;o&lt;/sup&gt; and 126&lt;sup&gt;o&lt;/sup&gt; &lt; l &lt; 180&lt;sup&gt;o&lt;/sup&gt;, for |b| &lt;= 5.5&lt;sup&gt;o&lt;/sup&gt;, and has some coverage to |b| ~ 9&lt;sup&gt;o&lt;/sup&gt;, with a resolution of ~70 x70 cosec{delta} arcsec&lt;sup&gt;2&lt;/sup&gt; (RA x Dec). The observations, data reduction and calibration of this survey are described in the reference paper, and the catalog of 6262 compact sources, with a completeness limit of ~ 0.25 Jy (250 mJy) over most of the survey region, is presented in this table. The catalog has an rms positional accuracy of better than 10 arcseconds, and the flux densities are tied to the scale of Roger, Bridle &amp; Costain (1973, AJ, 78, 1030) with an accuracy of better than 10 per cent. This table was created by the HEASARC in October 2010 based on CDS table J/MNRAS/294/607 file 7cg.dat. This is a service provided by NASA HEASARC .

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Organization: National Aeronautics and Space Administration
SAGE-SMC MIPS 70 micron Combined Epoch Full List

The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. \n\nTo be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.

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Organization: National Aeronautics and Space Administration