- ID:
- ivo://nasa.heasarc/aavsovsx
- Title:
- AAVSO International Variable Star Index
- Short Name:
- AAVSOVSX
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; <a href="http://www.aavso.org/vsx">http://www.aavso.org/vsx</a>). It consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included. This table was created by the HEASARC based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/vsx">CDS catalog B/vsx</a>. The CDS updates it regularly, and this HEASARC version is accordingly updated within a week of such updates. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/abell
- Title:
- Abell Clusters
- Short Name:
- Abell
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ABELL database contains information from a catalog of clusters of galaxies, each having at least 30 members within the magnitude range m3 to m3+2 (m3 is the magnitude of the third brightest cluster member) and each with a nominal redshift less than 0.2. The database contains the revised Northern Abell catalog, the Southern Abell catalog, and the Supplementary Southern Abell catalog; the catalogs are published as tables 3, 4 and 5 of Abell, Corwin & Orowin (1989). This database table was created by J. Osborne of Leicester from the STADAT SCAR file abelb.dat. The original SCAR version was created by Diana Parsons on 12 March 1990. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/abellzcat
- Title:
- Abell Clusters Measured Redshifts Catalog
- Short Name:
- ABELLZCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The all-sky ACO (Abell, Corwin and Olowin 1989, ApJS, 70, 1) Catalog of 4073 rich clusters of galaxies and 1175 southern poor or distant S-clusters has been searched for published redshifts. Data for 1059 of them were found and classified into various quality classes, e.g. to reduce the problem of foreground contamination of redshifts. Taking the ACO selection criteria for redshifts, a total of 992 entries remain, 21 percent more than ACO. Redshifts for rich clusters are now virtually complete out to a redshift z of 0.05 in the north and of 0.04 in the south. In the north, the magnitude-redshift (m_10 - z) relation agrees with that of Kalinkov et al. (1985, Astr. Nachr., 306, 283). For the southern rich clusters, minor adjustments to the m_10 - z relation of ACO are suggested, while for the S-clusters the redshifts are about 30 percent lower than estimated. This table was created by the HEASARC in May 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/165A">CDS Catalog VII/165A</a> file catalog.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/actmadcows
- Title:
- ACT Massive and Distant Clusters of WISE Survey (MaDCoWS) Candidates Catalog
- Short Name:
- ACTMADCOWS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Galaxy clusters are an important tool for cosmology, and their detection and characterization are key goals for current and future surveys. Using data from the Wide-field Infrared Survey Explorer (WISE), the Massive and Distant Clusters of WISE Survey (MaDCoWS) located 2839 significant galaxy overdensities at redshifts 0.7 <= z <= 1.5, which included extensive follow-up imaging from the Spitzer Space Telescope to determine cluster richnesses. Concurrently, the Atacama Cosmology Telescope (ACT) has produced large area millimeter-wave maps in three frequency bands along with a large catalog of Sunyaev-Zel'dovich (SZ)-selected clusters as part of its Data Release 5 (DR5). The authors aimed to verify and characterize MaDCoWS clusters using measurements of, or limits on, their thermal SZ effect signatures. They also used these detections to establish the scaling relation between SZ mass and the MaDCoWS-defined richness. Using the maps and cluster catalog from DR5, the authors explore the scaling between SZ mass and cluster richness. They do this by comparing cataloged detections and extracting individual and stacked SZ signals from the MaDCoWS cluster locations. The authors use complementary radio survey data from the Very Large Array, submillimeter data from Herschel, and ACT 224GHz data to assess the impact of contaminating sources on the SZ signals from both ACT and MaDCoWS clusters. They use a hierarchical Bayesian model to fit the mass-richness scaling relation, allowing for clusters to be drawn from two populations: one, a Gaussian centered on the mass-richness relation, and the other, a Gaussian centered on zero SZ signal. This study found that MaDCoWS clusters have submillimeter contamination that is consistent with a gray-body spectrum, while the ACT clusters are consistent with no submillimeter emission on average. Additionally, the intrinsic radio intensities of ACT clusters are lower than those of MaDCoWS clusters, even when the ACT clusters are restricted to the same redshift range as the MaDCoWS clusters. The authors found the best-fit ACT SZ mass versus MaDCoWS richness scaling relation has a slope of p1=1.84<sub>-0.14</sub><sup>+0.15</sup>, where the slope is defined as M ~lambda<sub>15</sub><sup>p1</sup> and lambda<sub>15</sub> is the richness. They also found that the ACT SZ signals for a significant fraction (~57%) of the MaDCoWS sample can statistically be described as being drawn from a noise-like distribution, indicating that the candidates are possibly dominated by low-mass and unvirialized systems that are below the mass limit of the ACT sample. Further, the authors noted that a large portion of the optically confirmed ACT clusters located in the same volume of the sky as MaDCoWS were not selected by MaDCoWS, indicating that the MaDCoWS sample is not complete with respect to SZ selection. Finally, the authors found that the radio loud fraction of MaDCoWS clusters increases with richness, while they found no evidence that the submillimeter emission of the MaDCoWS clusters evolved with richness. The authors concluded that the original MaDCoWS selection function is not well defined and, as such, reiterated the MaDCoWS collaboration's recommendation that the sample is suited for probing cluster and galaxy evolution, but not cosmological analyses. They found a best-fit mass-richness relation slope that agrees with the published MaDCoWS preliminary results. Additionally, they concluded that, while the approximate level of infill of the ACT and MaDCoWS cluster SZ signals (1-2%) is subdominant to other sources of uncertainty for current generation experiments, characterizing and removing this bias will be critical for next-generation experiments hoping to constrain cluster masses at the sub-percent level. This table was created by the HEASARC in April 2022 based upon the link provided by the LAMBDA archive: <a href="https://lambda.gsfc.nasa.gov/product/act/actpol_madcows_cl_catalog_get.html">https://lambda.gsfc.nasa.gov/product/act/actpol_madcows_cl_catalog_get.html</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/aegisx
- Title:
- AEGIS-X Chandra Extended Groth Strip X-Ray Point Source Catalog
- Short Name:
- AEGISX
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the X-ray sources detected in the AEGIS-X survey, a series of deep Chandra ACIS-I observations of the Extended Groth Strip (EGS). The survey comprises pointings at eight separate positions, each with nominal exposure of 200 ks, covering a total area of approximately 0.67 deg<sup>2</sup> in a strip of length 2 degrees. In their paper, the authors describe in detail an updated version of the data reduction and point-source-detection algorithms used to analyze these data. A total of 1325 band-merged sources have been found to a Poisson probability limit of 4 x 10<sup>-6</sup>, with limiting fluxes of 5.3 x 10<sup>-17</sup> erg cm<sup>-2</sup> s<sup>-1</sup> in the soft (0.5 - 2 keV) band and 3.8 x 10<sup>-16</sup> erg cm<sup>-2</sup> s<sup>-1</sup> in the hard (2 - 10 keV) band. They present simulations verifying the validity of their source-detection procedure and showing a very small, <1.5%, contamination rate from spurious sources. Optical/NIR counterparts have been identified from the DEEP2, CFHTLS, and Spitzer/Infrared Array Camera (IRAC) surveys of the same region. Using a likelihood ratio method, they find optical counterparts for 76% of their sources, complete to R<sub>AB</sub> = 24.1, and, of the 66% of the sources that have IRAC coverage, 94% have a counterpart to a limit of 0.9 uJy at 3.6 um (m<sub>AB</sub> = 23.8). After accounting for (small) positional offsets in the eight Chandra fields, the astrometric accuracy of Chandra positions is found to be 0.8 arcseconds rms; however, this number depends both on the off-axis angle and the number of detected counts for a given source. This table was created by the HEASARC in February 2009 based on the electronic versions of Tables 9, 10 and 11 from the paper which were obtained from the Astrophysical Journal web site. It is also available from the CDS at <a href="https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/180/102">https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/180/102</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/aegisxdcxo
- Title:
- AEGIS-X Deep Survey Chandra X-Ray Point Source Catalog
- Short Name:
- AEGISXDCXO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table is based on the results of deep Chandra imaging of the central region of the Extended Groth Strip, the AEGIS-X Deep (AEGIS-XD) survey. When combined with previous Chandra observations of a wider area of the strip, AEGIS-X Wide (AEGIS-XW), these provide data to a nominal exposure depth of 800ks in the three central ACIS-I fields, a region of approximately 0.29 deg<sup>2</sup>. This is currently the third deepest X-ray survey in existence; a factor ~2-3 shallower than the Chandra Deep Fields (CDFs), but over an area ~3 times greater than each CDF. This table contains a catalog of 937 point sources detected in the deep Chandra observations, along with identifications of the X-ray sources from deep ground-based, Spitzer, GALEX, and Hubble Space Telescope imaging. Using a likelihood ratio analysis, the authors associate multiband counterparts for 929/937 of their X-ray sources, with an estimated 95% reliability,making the identification completeness approximately 94% in a statistical sense. Reliable spectroscopic redshifts for 353 of the X-ray sources are available predominantly from Keck (DEEP2/3) and MMT Hectospec, so the current spectroscopic completeness is ~38%. For the remainder of the X-ray sources, the authors compute photometric redshifts based on multiband photometry in up to 35 bands from the UV to mid-IR. Particular attention is given to the fact that the vast majority of the X-ray sources are active galactic nuclei and require hybrid templates. The photometric redshifts have a mean accuracy sigma = 0.04 and an outlier fraction of approximately 5%, reaching sigma = 0.03 with less than 4% outliers in the area covered by CANDELS. The new AEGIS-XD Chandra data were taken at three nominal pointing positions, which the authors have designated AEGIS-1, AEGIS-2, and AEGIS-3. These observations were all taken in the time period 2007 December 11 to 2009 June 26 using the ACIS-I instrument. The centers of the 3 AEGIS fields correspond fairly closely to those of the EGS-3, EGS-4, and EGS-5 fields of Laird et al. (2009, ApJS, 180, 102). The Rainbow Cosmological Surveys Database (<a href="http://rainbowx.fis.ucm.es/Rainbow_Database/Home.html">http://rainbowx.fis.ucm.es/Rainbow_Database/Home.html</a>; see Section 4 of the reference paper for more details) contains many multiwavelength photometric datasets giving information on optical and infrared sources in these fields. The characteristics of these datasets are given in Table 7 of the reference paper. This table was created by the HEASARC in February 2016 based on the CDS catalog J/ApJS/220/10 files table11.dat, table12.dat, table13.dat, table14.dat and table15.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/akaribsc
- Title:
- AKARI/FIS All-Sky Survey Bright Source Catalog, Version 1
- Short Name:
- AKARIBSC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The AKARI Infrared Astronomical Satellite observed the whole sky in the far-infrared (50-180 microns or um) and the mid-infrared (9 and 18 um) between May 2006 and August 2007 (Murakami et al. 2007PASJ...59S.369M) in six infrared bands between 9 um and 180 um. The AKARI/FIS All-Sky Survey Bright Source Catalogue, Version 1.0 provides positions and fluxes for 427,071 point sources observed with the Far Infrared Surveyor (FIS) instrument in the 4 far-infrared wavelengths centered at 65, 90, 140 and 160 um; the table below provides a summary of the FIS filter characteristics: <pre> Filter: N60 WIDE-S WIDE-L N160 Center(um): 65 90 140 160 Range(um): 50-80 60-110 110-180 140-180 Pixel("): 26.8 26.8 44.2 44.2 </pre> The users of the catalog are requested to carefully read the release note at <a href="http://www.ir.isas.jaxa.jp/AKARI/Observation/">http://www.ir.isas.jaxa.jp/AKARI/Observation/</a> before critical discussions of the data. Any questions and comments are appreciated at the ISAS Helpdesk (iris_help@ir.isas.jaxa.jp). Please acknowledge the usage of the AKARI data (details at <a href="http://www.ir.isas.jaxa.jp/AKARI/Publications/guideline.html">http://www.ir.isas.jaxa.jp/AKARI/Publications/guideline.html</a>). This table was created by the HEASARC in May 2010 based on CDS catalog II/298 file fis.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/akaripsc
- Title:
- AKARI/IRC All-Sky Survey Point Source Catalog, Version 1
- Short Name:
- AKARIPSC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The AKARI Infrared Astronomical Satellite observed the whole sky in the far-infrared (50-180 microns or um) and the mid-infrared (9 and 18 um) between May 2006 and August 2007 (Murakami et al. 2007PASJ...59S.369M) in six infrared bands between 9 um and 180 um. The AKARI/IRC Point Source Catalogue, Version 1.0 provides positions and fluxes for 870,973 sources observed with the InfraRed Camera (IRC): 844,649 sources in the S9W filter, and 194,551 sources in the L18W filter; the table below provides a summary of the IRC filter characteristics: <pre> Filter: S9W L18W Center(µm): 9 18 Width(µm): 4.10 9.97 Range(µm): 6.7-11.6 13.9-25.6 Pixel("): 9.4x9.4 10.4x9.4 Limit(mJy): 50 120 [at 5{sigma}] </pre> The users of the catalog are requested to carefully read the release note at <a href="http://www.ir.isas.jaxa.jp/AKARI/Observation/">http://www.ir.isas.jaxa.jp/AKARI/Observation/</a> before critical discussions of the data. Any questions and comments are appreciated at ISAS Helpdesk (iris_help@ir.isas.jaxa.jp) Please acknowledge the usage of the AKARI data (details at <a href="http://www.ir.isas.jaxa.jp/AKARI/Publications/guideline.html">http://www.ir.isas.jaxa.jp/AKARI/Publications/guideline.html</a>). This table was created by the HEASARC in May 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/297">CDS catalog II/297</a> file irc.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/wsrt20anep
- Title:
- AKARI NEP WSRT 20-cm Source Catalog
- Short Name:
- WSRT20ANEP
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Westerbork Radio Synthesis Telescope (WSRT) has been used in 2004 to make a deep radio survey of an ~1.7 degree<sup>2</sup> field coinciding with the AKARI north ecliptic pole (NEP) deep field. The WSRT survey consisted of 10 pointings, mosaiced with enough overlap to maintain a similar sensitivity across the central region that reached as low as 21 microJanskies/beam (µJy/beam) at 1.4 GHz. The observations, data reduction and source count analysis are presented in the reference paper, along with a description of the overall scientific objectives. A catalog containing 462 sources detected with a resolution of 17.0 arcsecs by 15.5 arcsecs is presented. The differential source counts calculated from the WSRT data have been compared with those from the shallow VLA-NEP survey of Kollgaard et al. (1994, ApJS, 93, 145), and show a pronounced excess for sources fainter than ~1 mJy, consistent with the presence of a population of star-forming galaxies at sub-mJy flux levels. The AKARI NEP deep field is the focus of a major observing campaign conducted across the entire spectral region. The combination of these data sets, along with the deep nature of the radio observations will allow unique studies of a large range of topics including the redshift evolution of the luminosity function of radio sources, the clustering environment of radio galaxies, the nature of obscured radio-loud active galactic nuclei, and the radio/far-infrared correlation for distant galaxies. This catalog provides the basic data set for a future series of paper dealing with source identifications, morphologies, and the associated properties of the identified radio sources. This table was created by the HEASARC in March 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/517/A54">CDS catalog J/A+A/517/A54</a> file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/aknepdfcxo
- Title:
- Akari North Ecliptic Pole Deep Field Chandra X-Ray Point Source Catalog
- Short Name:
- AKNEPDFCXO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from the 300-ks Chandra survey in the AKARI North Ecliptic Pole (NEP) deep field. This field has a unique set of 9-band infrared photometry covering 2-24 micron from the AKARI Infrared Camera, including mid-infrared (MIR) bands not covered by Spitzer. The survey is one of the deepest ever achieved at ~15 micron, and is by far the widest among those with similar depths in the MIR. This makes this field unique for the MIR-selection of AGN at z ~1. The authors have designed a source detection procedure, which performs joint Maximum Likelihood PSF fits on all of their 15 mosaicked Chandra pointings covering an area of 0.34 square degrees. The procedure has been highly optimized and tested by simulations. A point source catalog with photometry and Bayesian-based 90%-confidence upper limits in the 0.5-7, 0.5-2, 2-7, 2-4, and 4-7 keV bands has been produced. The catalog contains 457 X-ray sources and the spurious fraction is estimated to be ~1.7%. Sensitivity and 90%-confidence upper flux limits maps in all bands are provided as well. In their study, the authors searched for optical MIR counterparts in the central 0.25 square degrees, where deep Subaru Suprime-Cam multi-band images exist. Among the 377 X-ray sources detected therein, ~80% have optical counterparts and ~60% also have AKARI mid-IR counterparts. The authors cross-matched their X-ray sources with MIR-selected AGN from Hanami et al. (2012, PASJ, 64, 70). Around 30% of all AGN that have MID-IR SEDs purely explainable by AGN activity are strong Compton-thick AGN candidates. The source catalog contained in this table uses an internal threshold of ML = 9.5 which corresponds to ML<sub>empir</sub> ~12 (see Sect. 4.3.3 of the reference paper for more details). In total, 457 sources are detected, of which 377 objects fall in the deep Subaru imaging region (shown in Figure 1 of the reference paper). This catalog is designed to identify X-ray emitting objects in the Chandra/AKARI NEP deep field. Together with the optimized cross-identification procedure, the clear advantage of the catalog is the very high reliability, while the catalog sacrifices completeness for objects with low counts (see Figure 9 in the paper). Only ~1.7% of the objects listed in the source catalog are expected to be spurious source detections. The two sources that have an ML-threshold in the 0.5-7 keV band below 9.5 originate from a 0.5-7 keV single-band source detection run. To quote similar ML values for all objects, the authors list the total 0.5-7 keV ML values from the joint 3-energy band source detection run. The listed counts, count rates, fluxes, and the corresponding uncertainties in the 0.5-7 keV band are taken from the single-band detection run. Considering the uncertainty in the astrometric calibration, all sources should be considered as possible X-ray counterparts that are within a radius of r<sub>match</sub> = sqrt(sigma<sub>total</sub><sup>2</sup>+sigma<sub>astro</sub><sup>2</sup>), with sigma<sub>total</sub> = 5 * sqrt(sigma<sub>sys</sub><sup>2</sup>+sigma<sub>stat</sub><sup>2</sup>) and sigma<sub>sys</sub> = 0.1 arcseconds and sigma<sub>astro</sub> = 0.2 arcseconds (astrometric uncertainty). The authors also created a low-probability source catalog (not contained in this present HEASARC table): they caution that, due to the significant number of spurious sources in the low-probability catalog, it should NOT be used to select X-ray sources or to increase the sample size of X-ray-selected objects. It can be of interest if the scientific goal requires one to EXCLUDE potential X-ray emitting objects from a sample with a high completeness, since, using this strategy, one accepts those objects that are excluded are not associated with an X-ray-emitting object. The low-probability source catalog (available at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/J_MNRAS/446/911/">http://cdsarc.u-strasbg.fr/ftp/cats/J_MNRAS/446/911/</a> as the files lowpscat.dat.gz and lowpscat.fits) has a lower maximum likelihood threshold than the main source catalog (an internal threshold of ML = 5, corresponding to ML<sub>empir</sub> ~9.5). This catalog contains 626 detected sources, of which 506 are located within the deep Subaru imaging region. Based on their simulated data, the authors conclude that 19% of all the low-probability source catalog entries are false detections. Considering only the deep Subaru imaging area the spurious source fraction drops to 15%. When using information from this catalog, please cite the reference paper: Krumpe et al. (2015, MNRAS, 446, 911). This table was created by the HEASARC in August 2015 based on CDS table J/MNRAS/446/911 files mainscat.dat, the main source catalog. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pigssboofd
- Title:
- Allen Telescope Array Pi GHz Sky Survey (PiGSS) Boo Field Source Catalog
- Short Name:
- PIGSSBOOFD
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Pi GHz Sky Survey (PiGSS) is a key project of the Allen Telescope Array (ATA). PiGSS is a 3.1 GHz survey of radio continuum emission in the extragalactic sky with an emphasis on synoptic observations that measure the static and time-variable properties of the sky. During the 2.5 year campaign, PiGSS will twice observe ~250,000 radio sources in the 10,000 deg<sup>2</sup> region of the sky with b > 30 degrees to an rms sensitivity of ~1 mJy. Additionally, sub-regions of the sky will be observed multiple times to characterize variability on timescales of days to years. Presented here are the results from observations of a 10 deg<sup>2</sup> region in the Bootes constellation overlapping the NOAO Deep Wide Field Survey field. The PiGSS image was constructed from 75 daily observations distributed over a 4 month period and has an rms flux density between 200 and 250 microJy. This represents a deeper image by a factor of 4-8 than the authors will achieve over the entire 10,000 deg<sup>2</sup>. In this table, they provide flux densities, source sizes, and spectral indices for the 425 sources detected in the image. They identify ~100 new flat-spectrum radio sources, and project that, when completed, PiGSS will identify 104 flat-spectrum sources. In their paper the authors identify one source that is a possible transient radio source. This survey provides new limits on faint radio transients and variables with characteristic durations of months. This table was created by the HEASARC in March 2011 based on electronic versions of Tables 2 and 4 from the reference paper which were obtained from the ApJ web site. The HEASARC changed the sign of the values of the last parameter in Table 4 (herein called spectral_index_3_error) from negative to positive. In March 2013, after receiving a clarification from Steve Croft, the HEASARC corrected the names of the 4 parameters describing the source sizes (to reflect the fact that they were diameters nor radii) to major_axis, minor_axis, fit_major_axis and fit_minor_axis. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pigsselcnf
- Title:
- Allen Telescope Array Pi GHz Sky Survey (PiGSS) Deep Fields Source Catalog
- Short Name:
- PIGSSELCNF
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from a total of 459 repeated 3.1-GHz radio continuum observations (of which 379 were used in a search for transient sources) of the ELAIS-N1, Coma, Lockman Hole, and NOAO Deep Wide Field Survey (NDWFS) fields as part of the Allen Telescope Array (ATA) Pi GHz Sky Survey (PiGSS). The observations were taken in 2 simultaneous 100-MHz wide bands centered at 3.04 and 3.14 GHz approximately once per day between 2009 May and 2011 April. Each image covers 11.8 square degrees and has 100" FWHM resolution. Deep images for each of the four fields have rms noise between 180 and 310 microJy (uJy), and the corresponding catalogs contain ~200 sources in each field. Typically 40-50 of these sources are detected in each single-epoch image. This represents one of the shortest cadence, largest area, multi-epoch surveys undertaken at these frequencies. The authors compared the catalogs generated from the combined images to those from individual epochs, and from monthly averages, as well as to legacy surveys. They undertook a search for transients, with particular emphasis on excluding false positive sources,but find no confirmed transients, defined here as sources that can be shown to have varied by at least a factor of 10. However, the authors found one source that brightened in a single-epoch image to at least six times the upper limit from the corresponding deep image. They also found a source associated with a z = 0.6 quasar which appears to have brightened by a factor ~3 in one of their deep images, when compared to catalogs from legacy surveys. The authors place new upper limits on the number of transients brighter than 10 mJy: fewer than 0.08 transients deg<sup>-2</sup> with characteristic timescales of months to years; fewer than 0.02 deg<sup>-2</sup> with timescales of months; and fewer than 0.009 deg<sup>-2</sup> with timescales of days. In this study, the authors accepted only as real sources those that are independently detected in both frequencies in at least one epoch (with a position matching tolerance of 50", corresponding to a false match probability of <2%). Their threshold of ~ 4.2 sigma for detection in a single image corresponds to a threshold of ~ 5.9 sigma in the dual-image catalog. They generated catalogs for the deep fields, consisting only of sources detected at both frequencies, and these are contained in the present HEASARC table. Notice that the authors previously published a list of 425 radio sources in the NDWFS field in the constellation of Bootes in an earlier paper (Bower et al 2010, ApJ, 725, 1792, available as the HEASARC database table PIGSSBOOFD). In the 2013 paper, they have performed a partial re-analysis of these data to conform with the updated analysis techniques used on the other three fields. This table was created by the HEASARC in March 2013 based on electronic versions of Tables 2, 3, 4 and 5 (source lists for each of the 4 fields, ELAIS N1, Lockman, Coma, and NDWFS, respectively) from the reference paper which were obtained from the ApJ web site. The HEASARC has created a new parameter called field_name which identifies in which table/field the source can be found. Thus, to select only sources in the Lockman Hole field, the user should select field_name= 'Lockman'. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atats
- Title:
- Allen Telescope Array Twenty-cm Survey (ATATS) Source Catalog
- Short Name:
- ATATS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the source catalog from the Allen Telescope Array Twenty-centimeter Survey (ATATS), a multi-epoch (12 visits), 690 deg<sup>2</sup> radio image and catalog at 1.4 GHz. The survey is designed to detect rare, very bright transients as well as to verify the capabilities of the ATA to form large mosaics. The combined image using data from all 12 ATATS epochs has an rms noise sigma = 3.94 mJy beam<sup>-1</sup> and a dynamic range of 180, with a circular beam of 150 arcseconds FWHM. It contains 4408 sources to a limiting sensitivity of 5 sigma = 20 mJy beam<sup>-1</sup>. The authors compare the catalog generated from this 12-epoch combined image to the NRAO VLA Sky Survey (NVSS), a legacy survey at the same frequency, and find that they can measure source positions to better than ~ 20 arcseconds. For sources above the ATATS completeness limit, the median flux density is 97% of the median value for matched NVSS sources, indicative of an accurate overall flux calibration. The authors examine the effects of source confusion due to the effects of differing resolution between the ATATS and NVSS on their ability to compare flux densities. They detect no transients at flux densities greater than 40 mJy in comparison with NVSS and place a 2 sigma upper limit of 0.004 deg<sup>-2</sup> on the transient rate for such sources. These results suggest that the >~ 1 Jy transients reported by Matsumara et al. (2009, AJ, 138, 787) may not be true transients, but rather variable sources at their flux density threshold. This table was created by the HEASARC in September 2010 based on the electronic version of Table 2 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/rassasaspv
- Title:
- All-Sky Automatic Survey (ASAS) Photometry of ROSAT All-Sky Survey Sources
- Short Name:
- RASSASASPV
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Photometric data from the All-Sky Automatic Survey (ASAS) - South (Declination less than 29 degrees) Survey have been used for the identification of bright stars located near the sources from the ROSAT All Sky Survey Bright Source Catalog (RASSBSC). In total, 6,028 stars brighter than 12.5 magnitude in the I- or the V-bands have been selected and analyzed for periodicity. Altogether, 2,302 variable stars have been found with periods ranging from 0.137 days to 193 days. Most of these stars have X-ray emission of coronal origin, but there are a few cataclysmic binaries and early type stars with colliding winds. Whenever it was possible, the authors collected data available in the literature so as to verify the periods and to classify variable objects. The catalog includes 1,936 stars (1,233 new) considered to be variable due to presence of spots (rotationally variable), 127 detached eclipsing binary stars (33 new), 124 contact binaries (11 new), 96 eclipsing stars with deformed components (19 new), 13 ellipsoidal variables (4 new), 5 miscellaneous variables and one pulsating RR Lyr type star (blended with an eclipsing binary). More than 70% of the new variable stars have amplitudes smaller than 0.1 magnitudes, but for the star ASAS 063656-0521.0 the authors have found the largest known amplitude of brightness variations due to the presence of spots (up to Delta V = 0.8 magnitudes). This table was created by the HEASARC in May 2018, based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/AcA/62/67">CDS Catalog J/AcA/62/67</a> files catalog.dat and remarks.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/euvexrtcat
- Title:
- All-Sky Catalog of Faint EUV Sources
- Short Name:
- EUV/Faint
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The All-Sky Catalog of Faint Extreme-Ultraviolet (EUV) Sources is a list of 534 objects detected jointly in the Extreme Ultraviolet Explorer (EUVE) (100 Angstrom (AA) band) All-Sky Survey and in the ROSAT X-ray Telescope (XRT) (0.25 keV band) All-Sky Survey. The joint selection criterion within a 1.5 arcminute positional tolerance permitted the use of a low count rate threshold in each survey. This low threshold was roughly 60% of the threshold used in the previous EUVE all-sky surveys, and 166 of the objects listed in this table were new EUV sources, appearing neither in the Second EUVE Source Catalog nor in the ROSAT Wide Field Camera Second Catalog. Preliminary identifications are offered for 105 of the 166 sources not previously reported in any EUV catalog: by far the most numerous (81) of the identifications are late-type (F-M) stars, while 18 are other stellar types, only 5 are white dwarfs, and none are extragalactic. The paucity of WDs and extragalactic objects may be explained by a strong horizon effect wherein interstellar absorption strongly limits the effective new-source search volume, and, thereby, selectively favors low-luminosity nearby sources over more luminous but distant objects. Notice that, with the adopted 1.5 arcminute acceptance criterion, about 50 spurious detections are expected. This Browse table was created in July 2003 based on CDS table IX/35/faint.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/qorgcat
- Title:
- All-Sky Optical Catalog of Radio/X-Ray Sources
- Short Name:
- QuasarOrg
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels >40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at <a href="http://quasars.org/qorg-data.htm">http://quasars.org/qorg-data.htm</a> Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result. This table was created by the HEASARC in November 2004 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/427/387">CDS Catalog J/A+A/427/387</a> file master.dat.gz. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/aegis20id
- Title:
- All-Wavelength Extended Groth Strip Int. Survey (AEGIS) 20-cm Fully Id-ed Sample
- Short Name:
- AEGIS20ID
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Infrared 3.6 - 8.0 micron (µm) images of the Extended Groth Strip (EGS) yield plausible counterpart identifications for all but one of 510 radio sources in the AEGIS20 S(1.4 GHz) > 50 microJansky (µJy) sample (Ivison et al. 2007, ApJ, 660, L77, available at the HEASARC as the AEGIS20 database table). This is the first such deep sample that has been effectively 100% identified. Achieving the same identification rate at R band would require observations reaching R<sub>AB</sub> > 27. Spectroscopic redshifts are available for 46% of the sample and photometric redshifts for an additional 47%. Almost all of the sources with 3.6-um AB magnitudes brighter than 19 have spectroscopic redshifts z < 1.1, while fainter objects predominantly have photometric redshifts with 1 <~ z <~ 3. Unlike more powerful radio sources that are hosted by galaxies having large stellar masses within a relatively narrow range, the AEGIS20 counterparts have stellar masses spanning more than a factor of 10 at z ~ 1. The sources are roughly 10% - 15% starbursts at z <~ 0.5 and 20%-25% active galactic nuclei mostly at z > 1, with the remainder of uncertain nature. Throughout this study, magnitudes are in the AB system, and the notation [w] means the AB magnitude at wavelength w in um. Source distances are based on standard Lambda-CDM cosmology with H<sub>0</sub> = 71 km s<sup>-1</sup> Mpc<sup>-1</sup> and Omega<sub>M</sub> = 0.27. Practical calculation of luminosity distances was based on the program ANGSIX (Kayser et al. 1997, A&A, 318, 680). This table was created by the HEASARC in July 2013 based on the electronic versions of Tables 1, 3, 4, and 5 from the reference paper which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/aegis20
- Title:
- All-Wavelength Extended Groth Strip Int. Survey (AEGIS) VLA 20-cm Source Catalog
- Short Name:
- AEGIS20
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from AEGIS20, a radio survey of the Extended Groth Strip (EGS) conducted with the Very Large Array (VLA) at a frequency of 1.4 GHz. The resulting catalog contains 1122 emitters (HEASARC Note: The abstract of the original reference paper said 1123, but as noted by Willner et al. (2012, ApJ, 756, 72: footnote 10, one entry ('EGS20 J142303.7+532224.5') was listed twice in the original catalog), and it is sensitive to ultraluminous (10<sup>12</sup> solar luminosities) starbursts to z <= 1.3, well matched to the redshift range of the DEEP2 spectroscopic survey in this region. The authors use stacking techniques to explore the microJansky-level emission from a variety of galaxy populations selected via conventional criteria - Lyman break galaxies (LBGs), distant red galaxies (DRGs), UV-selected galaxies, and extremely red objects (EROs) - determining their properties as a function of color, magnitude, and redshift and their extinction-free contributions to the history of star formation. This study confirms the familiar pattern that the star formation rate (SFR) density, increases by at least a factor of ~ 5 from z = 0 to 1, although the authors note highly discrepant UV- and radio-based SFR estimates. Their radio-based SFRs become more difficult to interpret at z > 1 where correcting for contamination by radio-loud active galactic nuclei (AGNs) comes at the price of rejecting luminous starbursts. While stacking radio images is a useful technique, accurate radio-based SFRs for z >> 1 galaxies require precise redshifts and extraordinarily high fidelity radio data to identify and remove accretion-related emission. Data were obtained at 1.4 GHz during 2003 to 2005 with the VLA in its B configuration, acquiring seven 3.125 MHz channels every 5 s at each of four intermediate frequencies. Data were obtained at six positions, spaced by 15 arcminutes, concentrating in the northern half of the EGS because of the proximity of 3C 295 (a 23 Jy source at 1.4 GHz). Around 18 hours of data were acquired for each of the field positions. Calibrated visibilities and associated weights were used to generate mosaics of 37 x 512<sup>2</sup> x 0.8 arcsec<sup>2</sup> pixel images to quilt the VLA's primary beam in each EGS field position. CLEAN boxes were placed tightly around all sources, and a series of IMAGR and CALIB tasks were run, clipping the UV data after subtracting CLEAN components generated by the third iteration of IMAGR. The central images from each of the pointings were then knitted together using FLATN, ignoring data beyond the primary beam's half-power point, to produce a large mosaic. The synthesized beam is circular, with a FWHM of ~ 3.8 arcseconds. To define a sample of radio sources, the authors searched signal-to-noise ratio (S/N) images using the SAD detection algorithm, emulating the technique described by Biggs & Ivison (2006, MNRAS, 371, 963). Sources with >= 4-sigma peaks were fitted with two-dimensional Gaussians using JMFIT, and those with >- 5-sigma peaks that survived were fitted in total intensity. Sources with sizes equal to or smaller than the restoring beam were considered unresolved. No correction is made for bandwidth smearing in the catalog; this is a small effect (~ 5%) given the mosaicking strategy and the use of the B configuration. 38, 79, 171, 496, and 1123 sources are detected with 1.4 GHz flux densities >= 2000, >= 800, >= 320, >= 130 and >= 50 microJansky (uJy) [including the duplicate source mentioned above], where the 5-sigma detection limits at 130 and 50 uJy cover 0.73 and 0.04 deg<sup>2</sup>, respectively. Confusion is not an issue; the source density on an arcmin<sup>2</sup> scale is < 0.01 beam<sup>-1</sup>. This table was created by the HEASARC in July 2013 based on an electronic versions of the catalog described in the reference paper which was obtained as a FITS file from the first author's web site at <a href="http://www.roe.ac.uk/~rji/aegis20/">http://www.roe.ac.uk/~rji/aegis20/</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/allwiseagn
- Title:
- AllWISE Catalog of Mid-IR AGNs
- Short Name:
- ALLWISEAGN
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains an all-sky sample of ~1.4 million active galactic nuclei (AGNs) meeting a two-color infrared photometric selection criterion for AGNs as applied to sources from the Wide-field Infrared Survey Explorer final catalog release (AllWISE). The authors assess the spatial distribution and optical properties of their sample and find that the results are consistent with expectations for AGNs. These sources have a mean density of ~38 AGNs per square degree on the sky, and their apparent magnitude distribution peaks at g ~ 20, extending to objects as faint as g ~ 26. The authors test the AGN selection criterion against a large sample of optically identified stars and determine the "leakage" (that is, the probability that a star detected in an optical survey will be misidentified as a quasi-stellar object (QSO) in their sample) rate to be <= 4.0 x 10<sup>-5</sup>. They conclude that their sample contains almost no optically identified stars (<= 0.041%), making this sample highly promising for future celestial reference frame work as it significantly increases the number of all-sky, compact extragalactic objects. The authors further compare their sample to catalogs of known AGNs/QSOs and find a completeness value of >= 84% (that is, the probability of correctly identifying a known AGN/QSO is at least 84%) for AGNs brighter than a limiting magnitude of R <= 19. This sample includes approximately 1.1 million previously uncataloged AGNs. The WISE survey is an all-sky mid-IR survey at 3.4, 4.6, 12, and 22 microns (W1, W2, W3, and W4, respectively) conducted between 2010 January 7 and August 6, during the cryogenic mission phase, and first made available to the public on 2011 April 14. WISE has angular resolutions of 6.1, 6.4, 6.5, and 12.0 arcseconds in its four bands, respectively. The AllWISE data release, which was used for this work, incorporates data from the WISE Full Cryogenic, 3-Band Cryo, and NEOWISE Post-Cryo survey (Mainzer et al. 2014, ApJ, 792, 30) phases, which were co-added to achieve a depth of coverage ~0.4 mag deeper than previous data releases. AllWISE contains the positions, apparent motions, magnitudes, and point-spread function (PSF)-profile fit information for almost 748 million objects. Astrometric calibration of sources in the WISE catalog was done by correlation with bright stars from the 2MASS point source catalog, and the astrometric accuracy for sources in the AllWISE release was further improved by taking into account the proper motions of these reference stars, taken from the fourth USNO CCD Astrograph Catalog (UCAC4, Zacharias et al. 2013, AJ, 145, 44). A comparison with ICRF sources shows that AllWISE Catalog sources in the brightness range of 8 < W1 < 12 mag have positional accuracies to within 50 mas, and half of these sources have positional accuracies to within 20 mas. For more details on the WISE mission, see Wright et al. (2010, AJ, 140, 1868). The authors took all sources from the AllWISE catalog following Equations (3) and (4) from Mateos et al. (2012, MNRAS, 426, 3271) and they require that all of their sources have S/N >= 5 in the first three bands, as recommended in Mateos et al. (2012); as a further constraint, they limit their results to those with cc_flags = "0000," meaning that the sources are unaffected by known artifacts such as diffraction spikes, persistence, halos, or optical ghosts. In order to characterize the optical properties of their sample, the authors cross-matched it to SDSS-DR12, which is the final data release of SDSS-III (Eisenstein et al. 2011, AJ, 142, 72), within a radial tolerance of R < 1", obtaining 424,366 matches. To determine the fraction of false positive positional matches (that is, incorrectly correlating an object in their sample with a different SDSS object due to random positional agreement), they performed the same match on a scrambled version of their sample coordinates, determining that less than 1% of other cross-matches are false positive positional matches between the two catalogs. The authors also cross-matched their sample sources with he second release of the Large Quasar Astrometric Catalog (LQAC-2; Souchay et al. 2012, A&A, 537, A99), which contains 187,504 quasars, including radio-selected quasars from the ICRF2, optically selected quasars from SDSS, and infrared-selected quasars from 2MASS, and thus represents a robust sample of quasars over a wide range of wavelengths. They find that 93,403 quasars from LQAC-2 have clean detections. The majority of non-detections are due to sources in LQAC-2 that are too faint, having R >~ 19. This table was created by the HEASARC in January 2016 based on the machine-readable version of Table 1 from the reference paper which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/nwayawgros
- Title:
- AllWISE Counterparts and Gaia Matches to ROSAT/2RXS X-Ray Sources
- Short Name:
- NWAYAWGROS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the 132,254 AllWISE counterparts and/or Gaia matches to 106,573 X-ray sources detected in the ROSAT 2RXS survey with Galactic latitude |b| > 15 degrees. These are the brightest X-ray sources in the sky, but their position uncertainties and the sparse multi-wavelength coverage until now rendered the identification of their counterparts a demanding task with uncertain results. New all-sky multi-wavelength surveys of sufficient depth, like AllWISE and Gaia, and a new Bayesian statistics-based algorithm, NWAY, allow us, for the first time, to provide reliable counterpart associations. NWAY extends previous distance- and sky density-based association methods and, using one or more priors (e.g. colors, magnitudes), weights the probability that sources from two or more catalogs are simultaneously associated on the basis of their observable characteristics. Here, counterparts have been determined using a Wide-field Infrared Survey Explorer (WISE) color-magnitude prior. A reference sample of 4,524 XMM/Chandra and Swift X-ray sources demonstrates a reliability of 94.7 per cent for 2RXS sources. Combining the results of this work and of the matching of XMM-Newton Slew Survey, Version 2 (XMMSL2) sources also reported in this study (the results of the latter are available as the HEASARC's database table NWAYAWGXMM) with Chandra-COSMOS data, the authors propose a new separation between stars and AGN in the X-ray/WISE flux-magnitude plane, that is valid over six orders of magnitude. The authors also release the NWAY code and its user manual. NWAY was extensively tested with XMM-COSMOS data. Using two different sets of priors, the authors find an agreement of 96 per cent and 99 per cent with published Likelihood Ratio methods. Their results were achieved faster and without any follow-up visual inspection. With the advent of deep and wide area surveys in X-rays (e.g. SRG/eROSITA, Athena/WFI) and radio (ASKAP/EMU, LOFAR, APERTIF, etc.), NWAY will provide a powerful and reliable counterpart identification tool. For all the available options, see the NWAY manual at <a href="https://github.com/JohannesBuchner/nway/raw/master/doc/nway-manual.pdf">https://github.com/JohannesBuchner/nway/raw/master/doc/nway-manual.pdf</a>. This table was created by the HEASARC in February 2018 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/473/4937">CDS catalog J/MNRAS/473/4937</a> file 2rxswg.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/nwayawgxmm
- Title:
- AllWISE Counterparts and Gaia Matches to XMM-Newton Slew Survey (v2.0) Sources
- Short Name:
- NWAYAWGXMM
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the 19,141 AllWISE counterparts and/or Gaia matches to 17,665 X-ray sources detected in the XMM-Newton Slew Survey, Version 2 (hereafter XMMSL2, currently available at the HEASARC as the XMMSLEWCLN table) list of 'Clean' sources that lie at Galactic latitude |b| > 15 degrees. These are among the brightest X-ray sources in the sky, but their position uncertainties and the sparse multi-wavelength coverage until now have rendered the identification of their counterparts a demanding task with uncertain results. New all-sky multi-wavelength surveys of sufficient depth, like AllWISE and Gaia, and a new Bayesian statistics-based algorithm, NWAY, allow us, for the first time, to provide reliable counterpart associations. NWAY extends previous distance- and sky density-based association methods and, using one or more priors (e.g. colors, magnitudes), weights the probability that sources from two or more catalogs are simultaneously associated on the basis of their observable characteristics. Here, counterparts have been determined using a Wide-field Infrared Survey Explorer (WISE) color-magnitude prior. A reference sample of 4,524 XMM/Chandra and Swift X-ray sources demonstrates a reliability of 97.4 per cent for XMMSL2 sources. Combining the results of this work and of the matching of ROSAT All-Sky Survey 2RXS sources also reported in this study (the results of the latter are available as the HEASARC's database table NWAYAWGROS) with Chandra-COSMOS data, the authors propose a new separation between stars and AGN in the X-ray/WISE flux-magnitude plane, that is valid over six orders of magnitude. The authors also release the NWAY code and its user manual. NWAY was extensively tested with XMM-COSMOS data. Using two different sets of priors, the authors find an agreement of 96 per cent and 99 per cent with published Likelihood Ratio methods. Their results were achieved faster and without any follow-up visual inspection. With the advent of deep and wide area surveys in X-rays (e.g. SRG/eROSITA, Athena/WFI) and radio (ASKAP/EMU, LOFAR, APERTIF, etc.), NWAY will provide a powerful and reliable counterpart identification tool. For all the available options, see the NWAY manual at <a href="https://github.com/JohannesBuchner/nway/raw/master/doc/nway-manual.pdf">https://github.com/JohannesBuchner/nway/raw/master/doc/nway-manual.pdf</a>. This table was created by the HEASARC in February 2018 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/473/4937">CDS catalog J/MNRAS/473/4937</a> file xmmslew2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/alfperxmm
- Title:
- Alpha Per Open Cluster XMM-Newton X-Ray Source Catalog
- Short Name:
- ALFPERXMM
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from the analysis of an archival XMM-Newton observation of part of the Alpha Persei open cluster. The authors detected 102 X-ray sources in the energy band from 0.3 to 8.0 keV, of which 39 of them are associated with the cluster as evidenced by their appropriate magnitudes and colors from Two Micron All Sky Survey (2MASS) photometry. In the reference paper, the authors extend the X-ray luminosity distribution (XLD) of the Alpha Persei cluster for M dwarfs, to add to the XLD found for hotter dwarfs from spatially extensive surveys of the whole cluster by ROSAT. Some of the hotter stars are identified as a background, possible slightly older group of stars at a distance of approximately 500 pc. Alpha Per is a young open cluster, found to be 50 Myr old from its upper main sequence turnoff morphology (Meynet et al. 1993, A&AS, 98, 477). More recently, Stauffer et al. (1999, ApJ, 527, 219) have found an age of 90 Myr from the low mass lithium depletion boundary. In addition to being relatively nearby (170 pc; Randich et al. 1996, A&A, 305, 785), the Alpha Per cluster is also lightly reddened (E(B - V ) = 0.09 mag; Meynet et al. 1993), making the data interpretation relatively robust. A fraction of the Alpha Per cluster was observed by XMM-Newton as part of the Mission Scientist Guaranteed Time (Pallavicini et al., 2004, MmSAI, 75, 434). A 60-ks observation was obtained on 2000 September 5 using the EPIC MOS and PN cameras on board XMM-Newton with a pointing centered at RA: 3<sup>h</sup> 26<sup>m</sup> 16<sup>s</sup> and Dec: 48<sup>o</sup> 50<sup>m</sup> 29<sup>s</sup> (J2000.0). This table was created by the HEASARC in June 2014 based on CDS Catalog J/AJ/145/143 files table1.dat and table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/amigps16gh
- Title:
- AMI Galactic Plane Survey 16-GHz Source Catalog
- Short Name:
- AMIGPS16GH
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Arcminute Microkelvin Imager (AMI) Galactic Plane Survey is a large-area survey of the outer Galactic plane to provide arcminute resolution (approximately 3 arcminutes) images at milli-Jansky (mJy) sensitivity in the centimeter-wave band. This table contains results from the first data release of the survey, consisting of 868 deg<sup>2</sup> of the Galactic plane, covering the area above 40 degrees Declination (corresponding to 76 to 170 degrees Galactic Longitude) between Galactic Latitudes of -5 to +5 degrees at a central frequency of 15.75 GHz (1.9 cm). The noise level in the survey is <~ 3mJy/beam away from bright sources. This table contains the source catalog of 3503 radio sources detected with peak flux densities at or greater than 5 sigma. In their paper, the authors describe in detail the drift-scan observations which have been used to construct the maps, including the techniques used for observing, mapping and source extraction, and summarize the properties of the finalized data sets. These observations constitute the most sensitive Galactic plane survey of large extent at centimeter-wave frequencies greater than 1.4 GHz. This table was originally ingested by the HEASARC in March 2013 based on the CDS Catalog J/MNRAS/429/3330 file catdr1.dat. It was updated in September 2013 using the latest data file from the CDS, which provided positions with improved precision. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ansuvpscat
- Title:
- ANS Ultraviolet Photometry Catalog of Point Sources
- Short Name:
- ANSUVPSCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- All reliable observations of point sources with the ultraviolet photometer onboard the Astronomical Netherlands Satellite (ANS) operating between the October 1974 and April 1976 are presented. Extended objects, non-detected objects, and objects at the edges of the instrument's field of view have been omitted. The catalog contains 3573 objects, mostly stars (the total ANS UV database contained 4800 observed positions). The ANS satellite observed in five UV channels centered around 150, 180, 220, 250 and 330 nm (1500, 1800, 2200, 2500 and 3300 Angstroms). The characteristics of the ANS UV photometric bands are: <pre> Band designation 15N 15W 18 22 25 33 ------------------------------------------------------------------------- Central wavelength (nm) 154.5 154.9 179.9 220.0 249.3 329.4 Bandwidth (nm) 5.0 14.9 14.9 20.0 15.0 10.1 </pre> The reported magnitudes were obtained from mean count rates converted to fluxes using the ANS absolute calibration of Wesselius et al. (1980A&A....85..221W). In addition to the ultraviolet magnitudes, the catalog contains positions taken from the satellite pointing, spectral types, and UBV data from other sources as well as comments on duplicity, variability, and miscellaneous notes concerning individual objects. Within the ANS photometric system, the UV magnitudes of different objects are comparable down to a level of 0.5-1.0%. Several studies on the intercomparison of all ANS data, and on the comparison of the ANS data with stellar models, with other UV satellites, and with the expected UV fluxes on the basis of ground-based information alone suggest that the ANS photometric system is well-established, and has, in particular, a linear dynamic range of at least a factor of 20,000. In these two respects, repeatability and dynamic range, the ANS UV instrument far exceeded all other UV missions then extant, e.g., TD-S2/68, OAO-WEP, and IUE. Of course, ANS had a much poorer spectral resolution, about 15 nm (150 Angstroms), than the other instruments. This table was created by the HEASARC in September 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/97">CDS Catalog II/97</a> file ans.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/arcquincxo
- Title:
- Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog
- Short Name:
- ARCQUINCXO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster. This table was created by the HEASARC in July 2007 based on CDS Catalog J/MNRAS/371/38 file table1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/acceptcat
- Title:
- Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog
- Short Name:
- ACCEPTCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K<sub>0</sub> + K<sub>100</sub> (r/100 kpc)<sup>alpha</sup>, where K<sub>0</sub> quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K<sub>0</sub> distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K<sub>0</sub> ~ 30 - 50 keV cm<sup>2</sup> and population peaks at K<sub>0</sub> ~ 15 keV cm<sup>2</sup> and K<sub>0</sub> ~ 150 keV cm<sup>2</sup>. The effects of point-spread function smearing and angular resolution on best-fit K<sub>0</sub> values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K<sub>0</sub> is also considered, and they find no indication that K<sub>0</sub> is significantly impacted by either. All data and results associated with this work are publicly available via the project web site <a href="http://www.pa.msu.edu/astro/MC2/accept/">http://www.pa.msu.edu/astro/MC2/accept/</a>. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August. This table was created by the HEASARC in January 2012 based on CDS Catalog J/ApJS/182/12 files table1.dat and table5.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ariel5
- Title:
- Ariel V All-Sky Monitor
- Short Name:
- ARIEL5
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The All Sky Monitor was one of six X-ray instruments on the Ariel 5 satellite. The satellite was launched into a low inclination (2.8 degrees), nearly circular orbit (altitude ~520 km) on 15 October 1974. Ariel 5 was actively pointed so that objects of interest could be observed by the four instruments aligned along its spin axis. The ASM was mounted 90 degrees from the spin axis; the satellite had a spin period of 6 seconds. The ASM operated from October 18, 1974 to March 10, 1980. The ASM instrument, built by the Lab for High Energy Astrophysics at NASA- Goddard Space Flight Center, provided continuous coverage of the entire sky, except for a 20 degree band straddling the satellite's equator. The ASM was intended to act as an early detection system for transients, and to monitor the variability of bright ( > 0.2 Crab) galactic sources. The instrument consisted of a pair of X-ray pinhole cameras, each covering opposite halves of the sky, with gas-filled imaging proportional counters. Position determination of sources was accomplished through position-sensitive anode wires and satellite rotation. Each camera had a 1-cm<sup>2</sup> aperture. Overall telemetry constraints limited the duty cycle for any given source to 1 percent. With the low telemetry rate provided for this instrument (1 bit/s), temporal and spectral information were sacrificed for the sake of all-sky coverage. Hence, spectral information was limited to a single 3 - 6 keV bandpass, and temporal resolution was limited to the satellite orbital period, ~100 minutes. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascaegclus
- Title:
- ASCA Elliptical Galaxies and Galaxy Clusters Catalog
- Short Name:
- ASCAEGCLUS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L<sub>X</sub> ~ kT<sup>alpha</sup>, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT > 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R<sub>1500</sub> (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M<sub>gas</sub> ~ T<sup>(2.33+/-0.07)</sup> from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h<sub>50</sub> km s<sup>-1</sup> Mpc<sup>-1</sup> and q<sub>0</sub> to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: <pre> Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm<sup>2</sup>) NGC 5018 9.8 x 10<sup>14</sup> GHO 1322+3114 1.3 x 10<sup>13</sup> J1888.16CL 5.9 x 10<sup>14</sup> CL 0317+1521 4.5 x 10<sup>14</sup> MS 1512.4+3647 1.0 x 10<sup>12</sup> PRG 38 6.9 x 10<sup>14</sup> SCGG 205 6.9 x 10<sup>14</sup> RGH 101 9.1 x 10<sup>14</sup> 3C 184 8.5 x 10<sup>14</sup> RX J1756.5+6512 1.6 x 10<sup>13</sup> 3C 324 5.4 x 10<sup>14</sup> PDCS 01 2.8 x 10<sup>14</sup> MS 0147.8-3941 5.0 x 10<sup>14</sup> </pre> This table was created by the HEASARC in December 2011 based on CDA Catalog J/PASJ/56/965 files table3.dat, table4.dat, table5.dat, table6.dat and table7.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascagps
- Title:
- ASCA Galactic Plane Survey of Faint X-Ray Sources
- Short Name:
- ASCAGPS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Sugizaki et al. (2001) have published a study of faint X-ray sources that were resolved in the ASCA Galactic Plane Survey and their contribution to the galactic ridge X-ray emission, and the present database contains their list of discrete sources. The X-ray emission from the central region of the Galactic plane, |l|<~45 degrees and |b|<~0.4 degrees, was studied in the 0.7 to 10 keV energy band with a spatial resolution of ~3' with the Advanced Satellite for Cosmology and Astrophysics (ASCA) observatory. The authors developed a new analysis method for the ASCA data to resolve discrete sources from the extended Galactic ridge X-ray emission (GRXE). Using the ASCA Gas Imaging Spectrometers (GISs), they successfully resolved 163 discrete sources with X-ray fluxes down to 10^-12.5^ergs/cm^2/s and determined the intensity variations of the GRXE as a function of the Galactic longitude with a spatial resolution of about 1 degree. This database was created by the HEASARC in December 2001 based on the ADC/CDS Catalog J/ApJS/134/77/table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascagis
- Title:
- ASCA GIS Source Catalog (AMSS-I + AMSS-II)
- Short Name:
- ASCAGIS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This is the complete X-ray source catalog of the ASCA Medium Sensitivity Survey, AMSS, or the Gas Imaging Spectrometer (GIS) catalog project. It has been constructed from data for fields covering Galactic latitudes |b| > 10 degrees which were obtained with the GIS instrument onboard the ASCA satellite between 1993 May and 1996 December (part I) and between 1997 January and 2000 May (part II). Part I of this catalog (AMSS-I) utilizes 368 combined fields, and contains 1343 sources (including target sources) with detection significance above 5 sigma in at least one of the 3 survey bands of 0.7-7.0, 2-10, or 0.7-2.0 keV, while AMSS-II uses 306 fields, and contains a total of 1190 sources, using the same criteria. The AMSS-I and AMSS-II catalogs together contain 2533 sources from an area of 278 square degrees and provide a unique database of X-ray sources in the flux range of 10^-13 to 10^-11 erg cm^-2 s^-1 (0.7-10 keV). The published paper contains a summary of the statistical properties of a complete X-ray sample consisting of 1969 serendipitous sources selected from AMSS-I and AMSS-II. For each source, the ASCA source name, position, 90% error radius, count rates (both observed and as corrected for Galactic absorption) in the 3 energy bands, detection signifances and fluxes in the 3 energy bands, and hardness ratio and associated error are provided. This version of the Browse ASCAGIS table containing the combined AMSS-I and AMSS-II source lists was created by the HEASARC in February 2006 based on the CDS version of the AMSS-I source list (CDS catalog J/ApJS/133/1) and the electronic ApJS version of the AMSS-II source list. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascalss
- Title:
- ASCA Large Sky Survey
- Short Name:
- ASCALSS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ASCA Large Sky Survey (LSS) was the first wide-area unbiased survey with the ASCA satellite in the 0.7 - 10 keV band around the North Galactic Pole region covering a continuous area of 7 square degrees. To make the best use of ASCA's capabilities, the authors developed a new source detection method in which the complicated detector responses were fully taken into account. Applying this method to the entire LSS data independently in the total (0.7 - 7 keV), hard (2 - 10 keV), and soft (0.7 - 2 keV) bands, they detected 107 sources altogether, with sensitivity limits of 6 x 10<sup>-14</sup> (0.7 - 7 keV), 1 x 10<sup>-13</sup> (2 - 10 keV), and 2 x 10<sup>-14</sup> ergs/s/cm<sup>2</sup> (0.7 - 2 keV), respectively. The complete list of detected sources is presented in this table. The detection criteria that needed to be satisfied were: (i) the significance of the summed count rate of the GIS and the SIS should exceed 4.5, and (ii) the significance of either the GIS or the SIS should also exceed 3.5. This database was created by the HEASARC in December 2001 based on the ADC/CDS Catalog J/ApJ/518/656. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascamaster
- Title:
- ASCA Master Catalog
- Short Name:
- ASCA
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ASCAMASTER table contains data on all ASCA observations that were ever in any of the following states: 'Accepted', 'Scheduled Long-Term', 'Scheduled Short-Term', 'Processed', and 'Archived'. The final status of an observation is given by the parameter Status. Specific dates that affect the status of an observation are listed as the parameters scheduled_date, observed_date, processed_date, archived_date, and cycle. Notice that, if one or more of the date parameters are empty for a given observation, this means that that those particular processes have not occurred: e.g., if observed_date is empty, this means that the planned observation was not observed. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascaprspec
- Title:
- ASCAProposalInfo&Abstracts
- Short Name:
- ASCAPRSPEC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ASCAPRSPEC table was created for the purpose of providing a complete, accurate, and easily accessible tracking of ASCA proposal information. This is a service provided by NASA HEASARC .
34. ASCA Proposals
- ID:
- ivo://nasa.heasarc/ascao
- Title:
- ASCA Proposals
- Short Name:
- ASCAO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ASCAO database contains the listing of accepted targets from all proposals submitted in repsonse to the ASCA Guest Observer (GO) Announcements of Opportunities (AOs), as well as the targets that were selected for the Performance Verification (PV) phase. The current version of ASCAO includes all accepted targets from AOs 1 through 8.5 inclusive. Notice that, since the accepted targets include Priority 3 ones of which only a fraction have or will actually be observed, some of the listed targets in this database will never have been observed. To obtain more detailed information about the status of particular targets, please consult either the Master ASCA database table (ASCAMASTER) or the ASCA Observing Log database table (ASCALOG). This database was last updated in August 2000 based on information provided by the ASCA Project. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ascasis
- Title:
- ASCA SIS Source Catalog
- Short Name:
- ASCASIS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This preliminary ASCA SIS Source Catalog contains a list of point sources detected by the Solid-state Imaging Spectrometers (SIS) on-board the ASCA Observatory. This catalog was generated by searching for point-like sources in all data available from the HEASARC's ASCA public archive (ASCAPUBLIC) as of 24 Oct 1996; and is populated by both target and serendipitous sources in the SIS field-of-view. For each catalogued source various information is available, which includes the celestial coordinates of the source, the count rate, the significance of detection, and the hardness ratio, total aperture counts, exposure time, and start time of the observation. In addition, a set of three GIF "thumbnail" images is available in the broad (0.5 - 12 keV), soft (2 < keV), and hard (> 2 keV) spectral bands centered on the apparent detection. These images are convenient for accessing the quality of the source detection. The current catalog is preliminary, the goal of the catalog authors being to make the SIS source list available as quickly as possible. To accomplish this, they took an incremental approach and placed their "work in progress" on-line, warts and all. They urge caution in using and citing these preliminary results, as they point out that the information is not, as yet, 100% reliable. This catalog was generated in January 1997 by Drs. Eric Gotthelf and Nicholas White and resulted from their search for point-like sources in all of the then-available SIS data files in the HEASARC's Public ASCA Data Archive as of 24 Oct 1996. The catalog is populated with both targeted and serendipitous sources that were present in the SIS field-of-view. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/asiagosn
- Title:
- Asiago Supernova Catalog (Dynamic Version)
- Short Name:
- ASIAGOSN
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the dynamic version of the Asiago Supernova Catalog. It supersedes the original 1999 version by Barbon et al. (1999A&AS..139..531B, Cat. II/227), and contains data about the supernovae observed since 1885 and their parent galaxies through a few days prior to the most recent update. In addition to the list of newly discovered SNe, the literature has been searched for new information on past SNe as well. The data for the parent galaxies have also been homogenized. This table was created by the HEASARC based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/sn">CDS Catalog B/sn</a>. The CDS updates it regularly, and this HEASARC version is accordingly updated within a week of such updates. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/acrs
- Title:
- Astrographic Catalog of Reference Stars
- Short Name:
- ACRS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- For a number of years there has been a great demand for a high-density catalog of accurate stellar positions and proper motions that maintains a consistent system of reference over the entire sky. The Smithsonian Astrophysical Observatory Star Catalog (SAO; SAO Staff 1966) has partially met those requirements, but its positions brought to current epochs now contain errors on the order of 1 second of arc, plus the proper motions in the SAO differ systematically with one another depending on their source catalogs. With the completion of the Second Cape Photographic Catalogue (CPC2; de Vegt et al. 1989), a photographic survey comparable in density to the AGK3 (Dieckvoss 1975) was finally available for the southern hemisphere. These two catalogs were used as a base and matched against the AGK2 (Schorr & Kohlschuetter 1951-58), Yale photographic zones (Yale Trans., Vols. 11-32), First Cape Photographic Catalogue (CPC1; Jackson & Stoy 1954, 55, 58; Stoy 1966), Sydney Southern Star Catalogue (King & Lomb 1983), Sydney Zone Catalogue -48 to -54 degrees (Eichhorn et al. 1983), 124 meridian circle catalogs, and catalogs of recent epochs, such as the Carlsberg Meridian Catalogue, La Palma (CAMC), USNO Zodiacal Zone Catalog (Douglass & Harrington 1990), and the Perth 83 Catalogue (Harwood [1990]) to obtain as many input positions as possible. All positions were then reduced to the system of the FK4 (Fricke & Kopff 1963) using a combination of the FK4, the FK4 Supplement as improved by H. Schwan of the Astronomisches Rechen-Institut in Heidelberg, and the International Reference Stars (IRS; Corbin 1991), then combined with the CPC2 and AGK3. The total number of input positions from which the ACRS was formed is 1,643,783. The original catalog is divided into two parts. Part 1 contains the stars having better observational histories and, therefore, more reliable positions and proper motions. This part constitutes 78 percent of the catalog; the mean errors of the proper motions are +/-0.47 arcsec per century and +/-0.46 arcsec per century in right ascension and declination, respectively. The stars in Part 2 have poor observational histories and consist mostly of objects for which only two catalog positions in one or both coordinates were available for computing the proper motions. Where accuracy is the primary consideration, only the stars in Part 1 should be used, while if the highest possible density is desired, the two parts should be combined. The ACRS was compiled at the U. S. Naval Observatory with the intention that it be used for new reductions of the Astrographic Catalogue (AC) plates. These plates are small in area (2 x 2 deg) and the IRS is not dense enough. Whereas the ACRS was compiled using the same techniques developed to produce the IRS, it became clear as the work progressed that the ACRS would have applications far beyond its original purpose. With accurate positions and proper motions rigorously reduced to both the FK4 and FK5 (Fricke et al. 1988) systems, it does more than simply replace the SAO. Rather, it provides the uniform system of reference stars that has been needed for many years by those who require densities greater than the IRS and with high accuracy over a wide range of epochs. It is intended that, as additional observations become available, stars will be migrated from Part 2 to Part 1, with the hope that eventually the ACRS will be complete in one part. Additional details concerning the compilation and properties of the ACRS can be found in Corbin & Urban (1989) except that the star counts and errors given here supersede the ones given in 1989. The HEASARC revised this database table in August, 2005, in order to add Galactic coordinates. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/actsouth
- Title:
- Atacama Cosmology Telescope (ACT) Extragalactic Southern Sources Catalog
- Short Name:
- ACTSOUTH
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ACTSOUTH catalog is a multi-frequency, multi-epoch catalog of extragalactic sources, based on 150, 220 and 280 GHz observations carried out in 2008, 2009 and 2010 using the Millimeter Bolometric Array Camera on the Atacama Cosmology Telescope. The catalog contains 695 sources, found in a sky area of ~600 square degrees. It is obtained by cross-matching sources found in 11 sub-catalogs, one for each season and frequency band. Also include are co-added data from ~150 and ~160 square degrees using 2 and 3 years of overlapping observations. The authors divide the sources into two populations, synchrotron and dusty emitters, based on their spectral behavior in the 150 - 220 GHz frequency range. They find 374 synchrotron sources and 321 dusty source candidates. Cross-matching with catalogs from radio to X-ray results in 264 synchrotron sources (71%) and 89 dusty sources (28%) with counterparts, suggesting that 232 dusty candidates are not in existing catalogs. This table was ingested by the HEASARC in November 2023 based upon the files downloaded from the LAMBDA archive at <a href="https://lambda.gsfc.nasa.gov/product/act/act_south_cat_get.html">https://lambda.gsfc.nasa.gov/product/act/act_south_cat_get.html</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/actszclust
- Title:
- Atacama Cosmology Telescope DR5 Sunyaev-Zeldovich Cluster Catalog
- Short Name:
- ACTSZCLUST
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The catalog of 4195 optically confirmed Sunyaev-Zel'dovich (SZ) selected galaxy clusters were detected with signal-to-noise > 4 in 13,211 deg<sup>2</sup> of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multi-frequency matched filter to 98- and 150-GHz maps constructed from ACT observations obtained from 2008-2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ-signal vs. mass scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M<sub>500c</sub> > 3.8 x 10<sup>14</sup>M<sub>sol</sub>, evaluated at z=0.5, for clusters detected at signal-to-noise ratio > 5 in maps filtered at an angular scale of 2.40. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ-signal mass-scaling relation, such as the Dark Energy Survey (4566 deg<sup>2</sup>), the Hyper Suprime-Cam Subaru Strategic Program (469 deg<sup>2</sup>), and the Kilo Degree Survey (825 deg<sup>2</sup>). This HEASARC database table was ingested in February 2021. It contains the ACT DR5 SZ cluster catalog obtained from the LAMDBA website (<a href="https://lambda.gsfc.nasa.gov/product/act/actpol_dr5_szcluster_catalog_info.cfm#catalog">https://lambda.gsfc.nasa.gov/product/act/actpol_dr5_szcluster_catalog_info.cfm#catalog</a>). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/actssrcat
- Title:
- Atacama Cosmology Telescope 2008 Southern Survey 148/218 GHz Source Catalog
- Short Name:
- ACTSSRCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a catalog of 191 extragalactic sources detected by the Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern survey. Flux densities span 14 -1700 mJy, and the authors use source spectral indices derived using ACT-only data to divide their sources into two subpopulations: 167 radio galaxies powered by central active galactic nuclei (AGN) and 24 dusty star-forming galaxies (DSFGs). They cross-identify 97% of their sources (166 of the AGN and 19 of the DSFGs) with those in currently available catalogs. When combined with flux densities from the Australia Telescope 20-GHz survey and follow-up observations with the Australia Telescope Compact Array, the synchrotron-dominated population is seen to exhibit a steepening of the slope of the spectral energy distribution from 20 to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated source population has a median spectral index, alpha<sub>148-218GHz</sub>, of 3.7<sup>+0.62</sup><sub>-0.86</sub>, and includes both local galaxies and sources with redshift around 6. Dusty sources with no counterpart in existing catalogs likely belong to a recently discovered subpopulation of DSFGs lensed by foreground galaxies or galaxy groups. The ACT experiment (Swetz et al., 2011, ApJS, 194, 41) is situated on the slopes of Cerro Toco in the Atacama Desert of Chile at an elevation of 5190m. ACT's latitude gives access to both the northern and southern celestial hemispheres. Observations occurred simultaneously in three frequency bands, at 148 GHz (2.0 mm), 218 GHz (1.4 mm) and 277 GHz (1.1 mm) with angular resolutions of roughly 1.4, 1.0 and 0.9 arcminutes, respectively. The ACT-detected source list contains 169 sources selected at 148 GHz with S/N > 5, spanning two decades in flux density, from 14 to 1700 mJy. The 218 GHz map independently yielded 133 sources with S/N > 5. The combination of these two independent source lists from which the present table was constructed gives a total count of 191 sources, with 110 galaxies detected with S/N > 5 at both frequencies. This table was created by the HEASARC in May 2015 based on CDS Catalog J/MNRAS/439/1556/ file table4.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/actegsrcat
- Title:
- Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog
- Short Name:
- ACTEGSRCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (>50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha<sub>5-20</sub> = -0.07 +/- 0.06, alpha<sub>20-148</sub> = -0.39 +/- 0.04, and alpha<sub>5-148</sub> = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C<sub>Sync</sub> = (2.8 +/- 0.3) x 10<sup>-6</sup> microKelvin<sup>2</sup>. This table was created by the HEASARC in January 2011 based on an electronic version of Table A1 from the paper (the Point Source Catalog) which was obtained from the LAMBDA website at <a href="http://lambda.gsfc.nasa.gov/product/suborbit/act_prod_table.cfm">http://lambda.gsfc.nasa.gov/product/suborbit/act_prod_table.cfm</a> This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/at20g1fgl
- Title:
- AT20G/Fermi 1FGL Source Catalog
- Short Name:
- AT20G1FGL
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The high-frequency radio sky, like the gamma-ray sky surveyed by the Fermi satellite, is dominated by flat-spectrum radio quasars and BL Lac objects at bright flux levels. To investigate the relationship between radio and gamma-ray emission in extragalactic sources, the authors have cross-matched the Australia Telescope 20-GHz survey catalog (AT20G: Murphy et al. 2010, MNRAS, 402, 2403, available as a HEASARC Browse table) with the Fermi-LAT 1-year Point Source Catalog (1FGL: Abdo et al. 2010, ApJS, 188, 405, also available as the HEASARC Browse table FERMILPSC). The 6.0 sr of sky covered by both catalogs (Declination < 0 degrees, |b| > 1.5 degrees) contains 5890 AT20G radio sources and 604 1FGL gamma-ray sources. The AT20G source positions are accurate to within ~1 arcsec and, after excluding known Galactic sources, 43% of Fermi 1FGL sources have an AT20G source within the 95% Fermi confidence ellipse. Monte Carlo tests imply that at least 95% of these matches are genuine associations. Only five gamma-ray sources (1% of the Fermi catalog) have more than one AT20G counterpart in the Fermi error box. The AT20G matches also generally support the active galactic nucleus (AGN) associations in the First LAT AGN Catalog. The authors find a trend of increasing gamma-ray flux density with 20 GHz radio flux density. The Fermi detection rate of AT20G sources is close to 100% for the brightest 20 GHz sources, decreasing to 20% at 1 Jy, and to roughly 1% at 100 mJy. Eight of the matched AT20G sources have no association listed in 1FGL and are presented here as potential gamma-ray AGNs for the first time. The authors also identify an alternative AGN counterpart to one 1FGL source. The percentage of Fermi sources with AT20G detections decreases toward the Galactic plane, suggesting that the 1FGL catalog contains at least 50 Galactic gamma-ray sources in the southern hemisphere that are yet to be identified. This table contains the complete list of all 233 Fermi-AT20G matches. This table was created by the HEASARC in August 2010 based on the electronic version of Table 4 obtained from the ApJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlasd2cpt
- Title:
- ATLargeAreaSurvey(ATLAS)CDF-S&ELAIS-S11.4-GHzDR2ComponentsCatalog
- Short Name:
- ATLASD2CPT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 microJy 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 'component' 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 'blob' 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 'source' 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 .
- ID:
- ivo://nasa.heasarc/atlascscpt
- Title:
- AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog
- Short Name:
- ATLASCSCPT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg<sup>2</sup> field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component. This table was created by the HEASARC in August 2012 based on CDS Catalog J/AJ/132/2409 file table4.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlascsid
- Title:
- AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog
- Short Name:
- ATLASCSID
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg<sup>2</sup> field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component. his table was created by the HEASARC in August 2012 based on CDS Catalog J/AJ/132/2409 file table6.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlas5p5gh
- Title:
- AT Large Area Survey (ATLAS) E-CDF-S 5.5-GHz Components Catalog
- Short Name:
- ATLAS5P5GH
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Star-forming galaxies are thought to dominate the sub-mJy radio population, but recent work has shown that low-luminosity active galactic nuclei (AGNs) can still make a significant contribution to the faint radio source population. Spectral indices are an important tool for understanding the emission mechanism of the faint radio sources. The authors have observed the extended Chandra Deep Field South at 5.5 GHz using a mosaic of 42 pointings with the Australia Telescope Compact Array (ATCA). Their image reaches an almost uniform sensitivity of ~ 12 microJy (uJy) rms over 0.25 deg<sup>2</sup> with a restoring beam of 4.9 arcsec x 2.0 arcsec, making the ATLAS 5.5-GHz survey one of the deepest 6-cm surveys to date. This table contains the 5.5 GHz catalog of 142 source components corresponding to the 123 sources in this field: the source counts from this field are discussed in the reference paper. This table was created by the HEASARC in February 2013 based on the electronic version of Table 1 from the reference paper which was obtained from the MNRAS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlas2p3gh
- Title:
- ATLargeAreaSurvey(ATLAS)ELAIS-S1&CDF-S2.3-GHzSourceCatalog
- Short Name:
- ATLAS2P3GH
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope Large Area Survey (ATLAS) aims to image a 7 deg<sup>2</sup> region centered on the European Large Area ISO Survey - South 1 (ELAIS-S1) field and the Chandra Deep Field South (CDF-S) at 1.4 GHz with high sensitivity (up to sigma ~ 10 uJy) to study the evolution of star-forming galaxies (SFGs) and Active Galactic Nuclei (AGN) over a wide range of cosmic time. The main goal of the present work is to study the radio spectra of an unprecedentedly large sample of sources (~ 2000 observed, ~ 600 detected in both frequencies). This table contains the results from ancillary radio observations at a frequency of 2.3 GHz which were obtained with the Australia Telescope Compact Array (ATCA). It comprises the catalog of sources with measured 1.4 GHz to 2.3 GHz spectral indices (Table 2 in the reference paper), compiled in the framework of ATLAS. It comprises only such sources which have unambiguous detections at both 1.4 GHz and 2.3 GHz, so no upper or lower limits on the spectral index based on non-detections are included. The 2.3-GHz detection limit is 300 uJy (equivalent to 4.5 sigma in the ELAIS-S1 field and 4.0 sigma in the CDF-S). The authors compute spectral indices between 1.4 GHz and 2.3 GHz using matched-resolution images and investigate various properties of their source sample in their dependence on their spectral indices. The authors find the entire source sample to have a median spectral index of -0.74, in good agreement with both the canonical value of -0.7 for optically thin synchrotron radiation and other spectral index studies conducted by various groups. Regarding the radio spectral index Alpha as indicator for source type, they find only marginal correlations so that flat or inverted spectrum sources are usually powered by AGN and hence conclude that, at least for the faint population, the spectral index is not a strong discriminator. They investigate the z-Alpha relation for their source sample and find no such correlation between spectral index and redshift at all. The authors do find a significant correlation between redshift and radio to near-infrared flux ratio, making this a much stronger tracer of high-z radio sources. They also find no evidence for a dependence of the radio-IR correlation on spectral index. This table was created by the HEASARC in August 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/544/A38">CDS Catalog J/A+A/544/A38</a> file spix_pub.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlasescpt
- Title:
- AT Large Area Survey (ATLAS) ELAIS-S1/SWIRE 1.4-GHz Components Catalog
- Short Name:
- ATLASESCPT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from the Australia Telescope Large Area Survey (ATLAS), and consists of sensitive (1 sigma < 30 uJy) 1.4-GHz radio observations of a 3.9 deg<sup>2</sup> field centered on the European Large Area ISO Survey S1 (ELAIS-S1) region, largely coincident with infrared observations of the Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. In their paper, the authors describe the observations and calibration, source extraction, and cross-matching to infrared sources. A total of 1366 radio components are identified, corresponding to 1276 distinct radio sources, 1183 of which are matched with infrared sources in the companion table ATLASESID. The authors have discovered 31 radio sources with no infrared counterpart at all, adding to the class of Infrared-Faint Radio Sources. The radio observations where made on 27 separate days in 2004 and 2005 with the Australia Telescope Compact Array (ATCA) with a total net integration time of 231 hours. as described in detail in Section 2.1 and Tables 1 and 2 of the reference paper. The observations were made in a mosaic of 20 overlapping pointings, where pointings 1-12 have net integration times of 10.5 hours per pointing and pointings 13-24 have net integration times of 13.5 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1.34 and 1.43 GHz. After editing, the predicted noise level is 22 uJy in the center of the mosaic. Toward the image edges, the noise level increases due to primary beam attenuation. This table contains the list of 1366 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission which is best defined as a Gaussian. Close radio doubles are very likely to be best represented by two Gaussians and are therefore deemed to consist of two components. Single or multiple components are called a radio source if they are deemed to belong to the same object. This table was created by the HEASARC in August 2012 based on CDS Catalog J/AJ/135/1276 file table4.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlasesid
- Title:
- AT Large Area Survey (ATLAS) ELAIS-S1/SWIRE ID and Classification Catalog
- Short Name:
- ATLASESID
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from the Australia Telescope Large Area Survey (ATLAS), and consists of sensitive (1 sigma < 30 uJy) 1.4-GHz radio observations of a 3.9 deg<sup>2</sup> field centered on the European Large Area ISO Survey S1 (ELAIS-S1) region, largely coincident with infrared observations of the Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. In their paper, the authors describe the observations and calibration, source extraction, and cross-matching to infrared sources. A total of 1366 radio components are identified, corresponding to 1276 distinct radio sources, 1183 of which are matched with infrared sources in the present table. The authors have discovered 31 radio sources with no infrared counterpart at all, adding to the class of Infrared-Faint Radio Sources. The radio observations where made on 27 separate days in 2004 and 2005 with the Australia Telescope Compact Array (ATCA) with a total net integration time of 231 hours, as described in detail in Section 2.1 and Tables 1 and 2 of the reference paper. The observations were made in a mosaic of 20 overlapping pointings, where pointings 1-12 have net integration times of 10.5 hours per pointing and pointings 13-24 have net integration times of 13.5 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1.34 and 1.43 GHz. After editing, the predicted noise level is 22 uJy in the center of the mosaic. Toward the image edges, the noise level increases due to primary beam attenuation. This table contains the list of 1276 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 5 of the reference paper. The authors define a radio 'component' as a region of radio emission which is best defined as a Gaussian. Close radio doubles are very likely to be best represented by two Gaussians and are therefore deemed to consist of two components. Single or multiple components are called a radio source if they are deemed to belong to the same object. This table was created by the HEASARC in August 2012 based on CDS Catalog J/AJ/135/1276 file table5.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlasspecz
- Title:
- ATLargeAreaSurvey(ATLAS)SpectroscopicClasses&RedshiftsCatalog
- Short Name:
- ATLASSPECZ
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope Large Area Survey (ATLAS) has surveyed 7 square degrees of sky around the Chandra Deep Field South (CDF-S) and the European Large Area ISO Survey-South 1 (ELAIS-S1) fields at 1.4 GHz. ATLAS aims to reach a uniform sensitivity of 10 µJy (µJy) beam<sup>-1</sup> rms over the entire region with first data release currently reaching ~ 30 uJy beam<sup>-1</sup> rms. Here the authors present 466 new spectroscopic redshifts for radio sources in ATLAS as part of their optical follow-up program. Of the 466 radio sources with new spectroscopic redshifts, 142 have star-forming optical spectra, 282 show evidence for active galactic nuclei (AGN) in their optical spectra, 10 have stellar spectra and 32 have spectra revealing redshifts, but with insufficient features to classify. The authors compare their spectroscopic classifications with two mid-infrared diagnostics and find them to be in broad agreement. ATLAS is a pathfinder for the forthcoming Evolution Map of the Universe (EMU) survey and the data presented in this paper will be used to guide EMU's survey design and early science papers. This paper uses H<sub>0</sub> = 70 km s<sup>-1</sup> Mpc<sup>-1</sup>, Omega<sub>M</sub> = 0.3 and Omega<sub>Lambda</sub> = 0.7, and the web-based calculator of Wright (2006, PASP, 118, 1711) to estimate the distance-dependent physical parameters. This table was created by the HEASARC in March 2013 based on an electronic version of Table 2 from the reference paper which was obtained from the MNRAS web site. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/arxa
- Title:
- Atlas of Radio/X-Ray Associations (ARXA)
- Short Name:
- ARXA
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: <pre> Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. </pre> Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio & X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see <a href="http://quasars.org/qorg-data.htm">http://quasars.org/qorg-data.htm</a>). Questions or comments on ARXA may be directed to eric@flesch.org. See also: <pre> APM home page <a href="http://www.ast.cam.ac.uk/~apmcat">http://www.ast.cam.ac.uk/~apmcat</a> USNO-A home page <a href="http://www.nofs.navy.mil/">http://www.nofs.navy.mil/</a> NVSS home page <a href="http://www.cv.nrao.edu/nvss/">http://www.cv.nrao.edu/nvss/</a> FIRST home page <a href="http://sundog.stsci.edu/">http://sundog.stsci.edu/</a> SUMSS home page <a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html">http://www.astrop.physics.usyd.edu.au/SUMSS/index.html</a> XMM-Newton home page <a href="http://xmmssc-www.star.le.ac.uk">http://xmmssc-www.star.le.ac.uk</a> HRI & PSPC home page <a href="http://www.mpe.mpg.de/ROSAT/">http://www.mpe.mpg.de/ROSAT/</a> WGA home page <a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html">http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html</a> RASS-FSC home page <a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc">http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc</a> RASS-BSC home page <a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc">http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc</a> Chandra home page <a href="http://chandra.harvard.edu">http://chandra.harvard.edu</a> XAssist home page <a href="http://xassist.pha.jhu.edu/zope/xassist">http://xassist.pha.jhu.edu/zope/xassist</a> (XMMX & CXOX sources are from XAssist) </pre> If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This online catalog was created by the HEASARC in January 2010 based on a machine-readable table obtained from the author's ARXA web site at <a href="http://quasars.org/arxa.htm">http://quasars.org/arxa.htm</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atnfpulsar
- Title:
- ATNF Pulsar Catalog
- Short Name:
- ATNF
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope National Facility (ATNF) Pulsar Catalog is a catalog of known pulsars compiled by R.N. Manchester et al. and is descended from pulsar database used for the paper "Catalog of 558 Pulsars" by J.H. Taylor, R.N. Manchester and A.G. Lyne 1993, ApJS, 88, 529-568. The current catalog has been supplemented by inclusion of published data from more recent radio surveys, in particular, the Parkes Multibeam (PM) Pulsar Survey (Manchester et al. 2001, MNRAS, 328, 17-35) [available at the HEASARC as the PMPULSAR table] and the Swinburne Intermediate Latitude Pulsar Survey (Edwards et al. 2001, MNRAS, 326, 358-374), both made using the ATNF Parkes 64-m radio telescope. Binary parameters for known binary pulsars are also included as well as all available astrometric and spin parameter information for all pulsars. The catalog includes all published rotation-powered pulsars. Two separate small subsets of pulsars detected only at high energies are also included in the current table: the first group comprises X-ray and gamma-ray pulsars which are apparently powered by spin-down energy, but which have not been detected at radio wavelengths, while the second group contains anomalous X-ray pulsars (AXPs) and soft-gamma-ray repeaters (SGRs) for which coherent pulsations have been detected. Accretion-powered pulsars such as Her X-1 and the recently discovered X-ray millisecond pulsars such as SAX J1808.4-3658 are not included in this table, however. Many people have contributed to the compilation of the data contained in this catalog and the database that it was derived from. The authors particularly thank Andrew Lyne of the University of Manchester, Jodrell Bank Observatory, David Nice of Princeton University, and Russell Edwards, then at Swinburne University of Technology. The also acknowledge the efforts of Warwick University students Adam Goode and Steven Thomas who compiled and checked a recent version of the database. The original (summer 2003) database at the ATNF website was compiled with the invaluable assistance of Maryam Hobbs, while the ATNF web interface was designed and constructed by Albert Teoh, a Summer Vacation Scholar at the ATNF in 2002/2003. The authors would appreciate if anyone making use of this catalog in a publication acknowledges the source of their information by quoting the ATNF Pulsar Catalog website address of <a href="http://www.atnf.csiro.au/research/pulsar/psrcat/">http://www.atnf.csiro.au/research/pulsar/psrcat/</a> This database table was initially created by the HEASARC in January 2002. It was revised in March 2002, in June 2003, and again in January 2014. It is based on the table obtained from <a href="http://www.atnf.csiro.au/research/pulsar/psrcat/expert.html">http://www.atnf.csiro.au/research/pulsar/psrcat/expert.html</a>. <p> Changes to the catalog are logged at <a href="http://www.atnf.csiro.au/research/pulsar/psrcat/catalogueHistory.html">http://www.atnf.csiro.au/research/pulsar/psrcat/catalogueHistory.html</a>. <p> The HEASARC table will be updated on a weekly basis whenever the original ATNF database table is updated. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atcdfsss82
- Title:
- Australia Telescope Chandra Deep Field-South and SDSS Stripe 82 20-GHz Sources
- Short Name:
- ATCDFSSS82
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a source catalog, one of the first results from a deep, blind radio survey carried out at 20 GHz with the Australia Telescope Compact Array, with follow-up observations at 5.5, 9 and 18 GHz. The Australia Telescope 20GHz (AT20G) deep pilot survey covers a total area of 5 deg<sup>2</sup> in the Chandra Deep Field South and in Stripe 82 of the Sloan Digital Sky Survey. The authors estimate the survey to be 90% complete above 2.5 mJy. Of the 85 sources detected, 55% have steep spectra (spectral index alpha<sub>1.4</sub><sup>20</sup> < -0.5) and 45% have flat or inverted spectra (alpha<sub>1.4</sub><sup>20</sup> >= -0.5). The steep-spectrum sources tend to have single power-law spectra between 1.4 and 18 GHz, while the spectral indices of the flat- or inverted-spectrum sources tend to steepen with frequency. Among the 18 inverted-spectrum (alpha<sub>1.4</sub><sup>20</sup> >= 0.0) sources, 10 have clearly defined peaks in their spectra with alpha<sub>1.4</sub><sup>5.5</sup> > 0.15 and alpha<sub>9</sub><sup>18</sup> < -0.15. On a 3-yr time-scale, at least 10 sources varied by more than 15 percent at 20 GHz, showing that variability is still common at the low flux densities probed by the AT20G-Deep Pilot (AT20GDP) survey. The AT20G-Deep Pilot survey was carried out with he ATCA in 2009 July, shortly after the telescope was provided with a new wide-bandwidth correlator, the CABB. As a result of this upgrade to the telescope, the observing bandwidth was increased by a factor of 16, from 2x128 to 2x2048 MHz, in all bands (ranging from 1.1 to 105 GHz), greatly increasing the sensitivity of continuum observations. These observations were made in continuum mode using two 2048-MHz CABB bands centered at 19 and 21 GHz, with each 2048-MHz band divided into 2048 1-MHz channels. All four Stokes parameters were measured. This table was created by the HEASARC in August 2015 based on the union of CDS Catalog J/MNRAS/439/1212 files table2.dat (the 50 sources in the 3-hr field) and table3.dat (the 35 sources in the 21-hr field). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atcaadfs20
- Title:
- Australia Telescope Compact Array AKARI Deep Field South 20-cm Source Catalog
- Short Name:
- ATCAADFS20
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 (uJy/beam, over an area of ~1.1 deg<sup>2</sup>, and ~2.5 deg<sup>2</sup> 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 (um) over a 12 deg<sup>2</sup> 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<sup>2</sup> 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 CDS Catalog J/MNRAS/427/1830 file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atesp1p4gh
- Title:
- Australia Telescope ESO Slice Project 1.4-GHz Source Catalog
- Short Name:
- ATESP1P4GH
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&A, 325, 954) galaxy redshift survey. This 26-degree<sup>2</sup> region is centered at Declination -40 degrees, and ranges in RA from 22<sup>h</sup> 30<sup>m</sup> to 01<sup>h</sup> 15<sup>m</sup>. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper. This table was created by the HEASARC in November 2012 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/63">CDS Catalog VIII/63</a> file atesp.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/at2fglus
- Title:
- Australia Telescope 2FGL Unassociated Sources Radio Source Catalog
- Short Name:
- AT2FGLUS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors report results of the first phase of observations with the Australia Telescope Compact Array (ATCA) at 5 and 9 GHz of the fields around 411 gamma-ray sources having declinations less than +10 degrees which were detected by the Fermi Gamma-ray Space Telescope, but marked as unassociated in the 2nd Fermi Large-Area Telescope (2FGL) Catalog (available at the HEASARC as the FERMILPSC table). They have detected 424 radio sources with flux densities in the range from 2 mJy to 6 Jy in the fields of 283 gamma-ray sources within their gamma-ray position error ellipses (drawn to cover the area of 99 per cent probability of their localization). Of these, 146 objects were detected in both 5- and 9-GHz bands. The authors found 84 sources with spectral indices flatter than -0.5 in their sample. The majority of detected sources are weaker than 100 mJy and for this reason were not found in previous surveys. Approximately 1/3 of this sample, 128 objects, have the probability of being associated which is more than 10 times the probability of their being a background source found in the vicinity of the gamma-ray object by chance. This table contains the catalog of positions of these radio sources, estimates of their flux densities and their spectral indices, when available. This table was created by the HEASARC in July 2013 based on the electronic versions of Tables 1, 2 and 3 from the reference paper which were obtained from the MNRAS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/at20gharc
- Title:
- Australia Telescope 20-GHz (AT20G) High-Angular Resolution Catalog
- Short Name:
- AT20GHARC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the high-angular-resolution catalog for the Australia Telescope 20-GHz (AT20G) survey, using the high-angular-resolution 6-km antenna data at the baselines of ~4500 m of the Australia Telescope Compact Array (ATCA). The authors have used the data to produce the visibility catalog that separates the compact active galactic nuclei (AGNs) from the extended radio sources at the 0.15-arcsecond angular scale, corresponding to the linear size scale of 1 kpc at redshifts higher than 0.7. They find the radio population at 20 GHz to be dominated by compact AGNs constituting 77% of the total sources in the AT20G. In the paper, they introduce the visibility-spectra diagnostic plot, produced using the AT20G cross-matches with lower frequency radio surveys at 1 GHz [the NRAO VLA Sky Survey (NVSS: Condon et al. 1998, AJ, 115, 1693) and the Sydney University Molonglo Sky Survey (SUMSS: Mauch et al. 2003, MNRAS, 342, 1117)], that separates the 20-GHz population into distinct sub-populations of the compact AGNs, the compact steep-spectrum (CSS) sources, the extended AGN-powered sources and extended flat-spectrum sources. The extended flat-spectrum sources include a local thermal emitting population of high-latitude planetary nebulae and also gravitational lens and binary black hole candidates among the AGNs. The authors find a smooth transition in properties between the CSS sources and the AGN populations. The visibility catalog, together with the main AT20G survey, provides an estimate of angular size scales for sources in the AT20G and an estimate of the flux arising from central cores of extended radio sources. The identification of the compact AGNs in the AT20G survey provides high-quality calibrators for high-frequency radio telescope arrays and very large baseline interferometry observations. This table was created by the HEASARC in December 2013 based on machine-readable versions of Tables 2 and 3 from the reference paper which were obtained from the MNRAS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/at20g
- Title:
- Australia Telescope 20-GHz (AT20G) Survey Catalog
- Short Name:
- AT20G
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope 20-GHz Survey (AT20G) is a blind radio survey carried out at 20 GHz with the Australia Telescope Compact Array (ATCA) from 2004 to 2008, and covers the whole sky south of declination 0 degrees. The AT20G source catalogue presented here is an order of magnitude larger than any previous catalogue of high-frequency radio sources, and includes 5890 sources above a 20-GHz flux-density limit of 40 mJy. All AT20G sources have total intensity and polarisation measured at 20 GHz, and most sources south of declination -15 degrees also have near-simultaneous flux-density measurements at 5 and 8 GHz. A total of 1559 sources were detected in polarised total intensity at one or more of the three frequencies. The completeness of the AT20G source catalog is 91% above 100 mJy/beam and 79% above 50 mJy/beam in regions south of Declination -15 degrees. North of -15 degrees, some observations of sources between 14 and 20 hours in RA were lost due to bad weather and could not be repeated, so the catalog completeness is lower in this region. Each detected source was visually inspected as part of the authors' quality control processs, and so the reliability of the final catalog is essentially 100%. This table was created by the HEASARC in March 2010 based on the CDS Catalog J/MNRAS/402/2403/ file at20gcat.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/at20gbss
- Title:
- Australia Telescope 20-GHz Survey Bright Source Sample
- Short Name:
- AT20GBSS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope 20-GHz (AT20G) Survey is a blind survey of the whole southern sky at 20 GHz (with follow-up observations at 4.8 and 8.6 GHz) carried out with the Australia Telescope Compact Array from 2004 to 2007. The Bright Source Sample (BSS) is a complete flux-limited sub-sample of the AT20G Survey catalog comprising 320 extragalactic (|b| > 1.5 degrees) radio sources south of declination -15 degrees with 20-GHz flux densities S<sub>20GHz</sub> > 0.50 Jy (500 mJy). Of these sources, 218 have near simultaneous observations at 8 and 5 GHz. In the reference paper, the authors present an analysis of the radio spectral properties in total intensity and polarization, size, optical identifications and redshift distribution of the BSS sources. Optical identifications provided an estimation of redshift for 186 sources with median values of 1.20 and 0.13 for QSOs and galaxies, respectively. This table was created by the HEASARC in August 2008 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/384/775">CDS Catalog J/MNRAS/384/775</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/athdfs3frq
- Title:
- Australia Telescope Hubble Deep Field-South 2.5, 5.2 and 8.7-GHz Source Catalog
- Short Name:
- ATHDFS3FRQ
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Deep radio observations of a wide region centered on the Hubble Deep Field-South (HDF-S) have been performed, providing one of the most sensitive sets of radio observations acquired on the Australia Telescope Compact Array (ATCA) to date. A central rms of ~ 10 microJy is reached at four frequencies (1.4, 2.5, 5.2, and 8.7 GHz). In this table, the full source catalogs from the 2.5, 5.2, and 8.7 GHz observations are presented to complement the data for the 1.4 GHz observations which were presented in Paper II (Huynh et al., 2005, AJ, 130, 1373, available at the HEASARC as the ATHDFS1P4G table) in this series, along with a detailed analysis of image quality and noise. The authors also have produced a consolidated catalog of all of their ATCA observations of the HDF-S by matching sources across all four of the frequencies in their survey (available at the HEASARC as the ATHDFSCCAT table). The details of the observations and data reduction are discussed in detail in Paper I of this series (Norris et al., 2005, AJ, 130, 1358) and summarized in Table 1 of the reference paper. The observations consist of single pointings centered on RA (J2000.0) = 22<sup>h</sup> 33<sup>m</sup> 25.96<sup>s</sup>, Dec (J2000.0) = -60<sup>o</sup> 38' 09.0" (2.5 GHz), and RA (J2000.0) = 22<sup>h</sup> 32<sup>m</sup> 56.22<sup>s</sup>, Dec (J2000.0) = -60<sup>o</sup> 33' 02.7" (5.2 and 8.7 GHz). The 5.2 and 8.7 GHz observations are centered on the HST WFPC field, while the 2.5 GHz observations were pointed halfway between the WFPC field and a bright confusing source to allow the bright source to be well cleaned from the 2.5 GHz image. At 5 sigma, the 5.2 and 8.7 GHz catalogs have over 96% reliability. At 2.5 GHz, the authors have enough statistics to examine the 5 - 5.5 sigma sources, and find that these are only about 40% reliable. With a SNR greater than 5.5 sigma, the 2.5 GHz catalog would have about 99% reliability. The authors thus cut off the catalogs at 5.5, 5, and 5 sigma for 2.5, 5.2, and 8.7 GHz, respectively. The final catalogs have 71, 24, and 6 sources at 2.5, 5.2, and 8.7 GHz, respectively. Given a prior 1.4 GHz position, it may be feasible to push the detection limit lower than 5 sigma. The authors searched for low-SNR sources by matching 3 - 5 sigma sources that lie within 2 sigma positional uncertainty of a 1.4 GHz source. The positional uncertainty was determined by adding the average 1.4 GHz uncertainty (1.1") in quadrature with the positional uncertainty of a 3 sigma source. At 2.5 GHz the allowed positional offset is 3.8", and for 5.2 and 8.7 GHz it is 2.8". Thus, there are 71, 18, and 2 sources at 2.5, 5.2, and 8.7 GHz, respectively, which are low-SNR high-frequency counterparts to 1.4 GHz sources. The authors included these sources in supplementary catalogs. This HEASARC table contains all 101 primary sources detected at 2.5, 5.2, and 8.7 GHz, as well as the 91 supplementary sources described above (the latter are flagged by having source_flag values of 'S'), for a grand total of 192 radio sources. This table was created by the HEASARC in December 2012 based on the CDS Catalog J/AJ/130/1371 files table47.dat, table58.dat and table68.dat, which contain the entire contents of Tables 4, 5, 6, 7 and 8 from the published paper. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/athdfsccat
- Title:
- Australia Telescope Hubble Deep Field-South Combined Source Catalog
- Short Name:
- ATHDFSCCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Deep radio observations of a wide region centered on the Hubble Deep Field-South (HDF-S) have been performed, providing one of the most sensitive sets of radio observations acquired on the Australia Telescope Compact Array (ATCA) to date. A central rms of ~ 10 microJy is reached at four frequencies (1.4, 2.5, 5.2, and 8.7 GHz). In this table, the combined 4-frequency AT-HDFS Catalog including fluxes and spectral indices for sources detected at 1.4, 2.5, 5.2, and/or 8.7 GHz observations is presented to complement the single-frequency radio data for the 1.4 GHz observations which were presented in Paper II (Huynh et al., 2005, AJ, 130, 1373, available at the HEASARC as the ATHDFS1P4G table) in this series, and for the 2.5, 5.2, and/or 8.7 GHz observations which were presented in the reference paper (Paper III, Huynh et al., 2007, AJ, 133, 1331, available at the HEASARC as the ATHDFS3FRQ table). The details of the observations and data reduction are discussed in detail in Paper I of this series (Norris et al., 2005, AJ, 130, 1358) and summarized in Table 1 of the reference paper. The radio observations were carried out by the ATCA over 4 years from 1998 to 2001. The observations at 1.4 and 2.5 GHz consist of single pointings centered on RA (J2000.0) = 22<sup>h</sup> 33<sup>m</sup> 25.96<sup>s</sup>, Dec (J2000.0) = -60<sup>o</sup> 38' 09.0". The observations at 5.2 and 8.7 GHz consist of single pointings centered on RA (J2000.0) = 22<sup>h</sup> 32<sup>m</sup> 56.22<sup>s</sup>, Dec (J2000.0) = -60<sup>o</sup> 33' 02.7". The 5.2 and 8.7 GHz observations are centered on the HST WFPC field, while the 1.4 and 2.5 GHz observations were pointed halfway between the WFPC field and a bright confusing source to allow the bright source to be well cleaned from the 1.4 and 2.5 GHz images. This HEASARC table contains the final consolidated catalog of 473 individual sources and gives the flux densities at all frequencies for each individual radio source. It contains the 466 1.4-GHz sources from Paper II together with 5 unmatched 2.5-GHz sources and 2 unmatched 8.7-GHz sources. The procedure that the authors used to construct this catalog is discussed in Section 6 of the reference paper. This table was created by the HEASARC in December 2012 based on the CDS Catalog J/AJ/130/1371 file table9.dat which contains the entire contents of Table 9 from the published paper. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/athdfs1p4g
- Title:
- Australia Telescope Hubble Deep Field-South 1.4-GHz Source Catalog
- Short Name:
- ATHDFS1P4G
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table derives from a paper which is part of a series describing the results from the Australia Telescope Hubble Deep Field-South (ATHDFS) survey obtained with the Australia Telescope Compact Array. This survey consists of observations at 1.4, 2.5, 5.2, and 8.7 GHz, all centered on the Hubble Deep Field-South. Herein are presented the first results from the extended observing campaign at 1.4 GHz. A total of 466 sources have been cataloged to a local sensitivity of 5-sigma (11 microJy rms). A source extraction technique is developed that (1) successfully excludes spurious sources from the final source catalogs and (2) accounts for the nonuniform noise in the image. A source catalog is presented, and the general properties of the 1.4-GHz image are discussed in the reference paper. In the latter, the authors also present source counts derived from their ATHDFS 1.4-GHz catalog. The 1.4 GHz observations were carried out by the Australia Telescope Compact Array over 4 years from 1998 to 2001. They consist of single pointings centered on RA (J2000.0) = 22<sup>h</sup> 33<sup>m</sup> 25.96<sup>s</sup>, Dec (J2000.0) = -60<sup>o</sup> 38' 09.0". This table was created by the HEASARC in November 2012 based on the CDS Catalog J/AJ/130/1371 file table1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/athdfsoid
- Title:
- Australia Telescope Hubble Deep Field-South Optical Identifications Catalog
- Short Name:
- ATHDFSOID
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope Hubble Deep Field-South (ATHDF-S) survey of the Hubble Deep Field-South (HDF-S) reaches sensitivities of ~ 10 microJy (uJy) at 1.4, 2.5, 5.2, and 8.7 GHz, making the ATHDF-S one of the deepest surveys ever performed with the Australia Telescope Compact Array (ATCA). This table contains the optical identifications of the ATHDF-S radio sources (the radio data from which are available in summarized form in the HEASARC ATHDFSCCAT table) using data from the literature. The authors find that ~ 66% of the radio sources have optical counterparts to an I magnitude of 23.5 mags. Deep Hubble Space Telescope (HST) imaging of the area identifies a further 12% of the radio sources. In this table, the authors present data from new spectroscopic observations for 98 of the radio sources and supplement these spectroscopic redshifts with photometric ones calculated from five-band optical imaging. The radio observations and data reduction are detailed in Papers I-III of this series: <pre> I = Norris et al., 2005, AJ, 130, 1358; II = Huynh et al., 2005, AJ, 130, 1373, available at the HEASARC as the ATHDFS1P4G table; III = Huynh et al., 2007, AJ, 133, 1331, available at the HEASARC as the ATHDFSCCAT and ATHDFS3FRQ tables. </pre> Palunas et al. (2000, ApJ, 541, 61) observed the HDF-S region using the Big Throughput Camera (BTC) on the Cerro Tololo Inter-American Observatory (CTIO) 4m during 1998 September. Images were taken in the Sloan Digital Sky Survey (SDSS) u, Johnson B and V, and Cousins R and I filters. In addition, the authors obtained spectra of the ATHDF-S radio sources over two service nights in 2001 July and 2003 October using the multi-fiber 2dF instrument of the Anglo-Australian Telescope (AAT). They acquired low-resolution (9 Angstrom) spectra over the wavelength range from 3800 to 8000 Angstroms. This table was created by the HEASARC in December 2012 based on the CDS Catalog J/AJ/135/2470 files table1.dat and table10.dat which contain the entire contents of Tables 1 and 10 from the published paper. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlgds2p1g
- Title:
- Australia Telescope Local Group Dwarf Spheroidals 2.1-GHz Components Catalog
- Short Name:
- ATLGDS2P1G
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Dwarf spheroidal (dSph) galaxies are key objects in near-field cosmology, especially in connection to the study of galaxy formation and evolution at small scales. In addition, dSphs are optimal targets to investigate the nature of dark matter. However, while we begin to have deep optical photometric observations of the stellar population in these objects, little is known so far about their diffuse emission at any observing frequency, and hence on thermal and non-thermal plasma possibly residing within dSphs. In this paper, the authors present deep radio observations of six local dSphs performed with the Australia Telescope Compact Array (ATCA) at 16 cm wavelength (2100 MHz frequency). They mosaicked a region of radius of about 1 degree around three 'classical' dSphs (CDS), Carina, Fornax, and Sculptor, and of about half of degree around three 'ultrafaint' dSphs (UDS), Bootes II, Segue 2, and Hercules. The rms noise level is below 0.05 mJy for all the maps. The restoring beams full width at half-maximum (FWHM) ranged from (4.2 arcseconds by 2.5 arcseconds) to (30.0 arcseconds by 2.1 arcseconds) in the most elongated case. A catalog, including the 1392 sources detected in the six dSph fields, is presented here. In the reference paper, the main properties of the background sources are discussed, with the positions and fluxes of the brightest objects compared with the FIRST, NVSS, and SUMSS observations of the same fields. The observed population of radio emitters in these fields is dominated by synchrotron sources.The authors have computed the associated source number counts at 2 GHz down to fluxes of 0.25 mJy, which prove to be in agreement with AGN count models. The observations presented in this paper were performed during 2011 July. The project was allocated a total of 123 h of ATCA observing time. The spectral setup included the simultaneous observation of a 2-GHz-wide band centered at 2100 MHz with a 1 MHz spectral resolution for continuum observations (recording all four polarization signals). The mapping of the three CDS required a 19 field-mosaic with a total on-source integration time of about 1 hour per field. For Bootes II and Hercules, a 7 field-mosaic with an on-source integration time of about 2 hours per field was chosen, while Segue 2, due to its smaller size,was imaged with a 3 field-mosaic with about 4 hours per field of integration time (with the purpose of maximizing the sensitivity). More precisely, a total of 16.5, 15.0, 17.0, 13.0, 10.9, and 9.6 hours were spent on-source for Carina, Fornax, Sculptor, Bootes II, Hercules, and Segue 2, respectively. The nominal rms sensitivity in each panel for the actual observing time was 36, 38, 35, 25, 28, and 20 microJy for Carina, Fornax, Sculptor, Bootes II, Hercules, and Segue 2, respectively. See Table 1 of the reference paper for the details of the average restoring beam parameters across all mosaic panels for each field of view (FoV). The authors used two automated routines for source extraction and cataloging, which are provided by the SEXTRACTOR package (Bertin & Arnouts 1996, A&AS, 117, 393) and the task SFIND in MIRIAD. In these maps, SFIND and SEXTRACTOR give nearly identical results for astrometry (number of sources and positions), once the threshold parameters in SEXTRACTOR are tuned (the authors found a threshold typically slightly above 5 sigma). The mismatch in positions is random, and about 1 arcsecond on average for all FoVs. This value can be taken as an estimate of the positional accuracy. Photometry on the other hand, gave quite different results for some sources: in the catalog, the authors used the results from SFIND since this was specifically written to analyze radio images, accounting for artifacts and sidelobes. The number of sources in each dSph FoV is reported in Table 2 of the reference paper. Radio sources can be made up of different components. To decide whether nearby sources are separated sources or components of a single source, the authors visually inspected all the fields where either the angular distance, theta, between sources was < 1 arcminute, or the criterion of Magliocchetti et al. (1998, MNRAS, 300, 257: theta < 100 arcseconds x sqrt[S<sub>peak</sub>/10 mJy]), was satisfied. A more detailed study of the 178 possible multiple sources will be reported in a future paper by these authors. This table was created by the HEASARC in June 2015 based on an electronic version of the source components catalog (Table 4 of the reference paper) which was obtained from the MNRAS web site. In Section 4 of the reference paper, the authors state that they "found 1835 entries in the catalog corresponding to a total of 1392 extracted sources with 178 cases being (possibly) multiple component sources". We note that the table downloaded from the MNRAS web site and used as the basis for this current HEASARC table actually contained only 1834 entries, The reason for this small discrepancy is not known. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atlbs1p4gh
- Title:
- Australia Telescope Low-Brightness Survey Source Catalog
- Short Name:
- ATLBS1P4GH
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Australia Telescope Low-brightness Survey (ATLBS) regions have been mosaic imaged at a radio frequency of 1.4 GHz with 6 arcseconds angular resolution and 72 microJansky per beam (uJy/beam) rms noise. The images (centered at RA 00<sup>h</sup> 35<sup>m</sup> 00<sup>s</sup>, Dec -67<sup>o</sup> 00' 00" and RA 00<sup>h</sup> 59<sup>m</sup> 17<sup>s</sup>, Dec -67<sup>o</sup> 00' 00", J2000 epoch) cover 8.42 deg<sup>2</sup> sky area and have no artifacts or imaging errors above the image thermal noise. Multi-resolution radio and optical r-band images (made using the 4 m CTIO Blanco telescope) were used to recognize multi-component sources and prepare a source list of 1366 1.4-GHZ sources; the detection threshold was 0.38 mJy in a low-resolution radio image made with beam FWHM of 50 arcseconds. Radio source counts in the flux density range 0.4-8.7 mJy are estimated, with corrections applied for noise bias, effective area correction, and resolution bias. The resolution bias is mitigated using low-resolution radio images, while effects of source confusion are removed by using high-resolution images for identifying blended sources. Below 1 mJy the ATLBS counts are systematically lower than the previous estimates. Showing no evidence for an upturn down to 0.4 mJy, they do not require any changes in the radio source population down to the limit of the survey. The work suggests that automated image analysis for counts may be dependent on the ability of the imaging to reproduce connecting emission with low surface brightness and on the ability of the algorithm to recognize sources, which may require that source finding algorithms effectively work with multi-resolution and multi-wavelength data. The work underscores the importance of using source lists - as opposed to component lists - and correcting for the noise bias in order to precisely estimate counts close to the image noise and determine the upturn at sub-mJy flux density. This table was created by the HEASARC in April 2013 based on an electronic version of Table 2 from the reference paper that was obtained from the ApJ web site.. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/atpmncat
- Title:
- Australia Telescope-PMN Catalog of Southern Radio Sources
- Short Name:
- ATPMNCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a source catalog of 9040 radio sources derived from high-resolution observations of a selection of 8385 Parkes-MIT-NRAO (PMN) sources made with the Australia Telescope Compact Array (ATCA). The catalog lists flux density and structural measurements at 4.8 and 8.6 GHz, derived from observations of all PMN sources in the declination range -87 degrees < Dec < -38.5 degrees (exclusive of galactic latitudes |b| < 2 degrees) with PMN flux density S<sub>4850</sub> > 70mJy (> 50 mJy south of Dec = -73 degrees). The authors assess the quality of the data, which was gathered in the 1992-1994 time period, and the resulting source parameters. They describe the population of catalogued sources, and compare it to samples from complementary catalogs. In particular, they find 122 radio sources with highly probable association with gamma-ray sources observed by the orbiting Fermi Large Area Telescope (LAT), and 11 more radio sources with possible associations with Fermi LAT sources. This Australia Telescope PMN (ATPMN) catalog lists the source measurements of flux density, position and structure of a selection of sources from the PMN catalog. Each catalog entry corresponds to a discrete source observed by the ATCA. In many cases, a single PMN source yields several ATPMN sources. Apart from the name of the parent PMN source, there is no indication of physical association: multiple sources in the one field may be aligned by chance, or may be components of the one object. This catalog contains the following information for each source: position; the flux density at 4.8 and 8.6 GHz; uncertainties in each flux density; the source size modelled as an ellipse (major axes, minor axes, position angle) of the best fit for a Gaussian brightness distribution; the spectral index computed between 4.8 and 8.6 GHz; the uncertainty in the spectral index; a code denoting the epoch of the observation. In the table as given in the original reference, the positions were given with varying degrees of precision, from 0.001 to 1 second of time in RA and from 0.01 to 1 arcsecond in Declination. The authors state in Section 4 of the reference paper that the error in a position coordinate is less than 10 times the final digit given in the coordinate. The positions as displayed in this table do not reflect this system: e.g., a Dec value displayed as '-79 58 34.00' may have been given in the original table as '-79 58 34.00' or '-79 58 34.0' or '-79 58 34'. To recover this information about positional precision the HEASARC has created two additional parameters ra_accuracy and dec_accuracy which list the number of digits after the decimal point given in the original table for the RA and Dec, respectively. Thus, if ra_accuracy = 3, the RA was given to a precision of 0.001 s in the original table, implying that the actual error in RA was less than 10 * 0.001 = 0.01 s. This table was created by the HEASARC in July 2012 based on CDS Catalog J/MNRAS/422/1527 file atpmncat.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/axis
- Title:
- AXIS XMM-Newton Source Catalog
- Short Name:
- AXIS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Recent results have revised upwards the total X-ray background (XRB) intensity below ~10 keV, therefore an accurate determination of the source counts is needed. There are also contradictory results on the clustering of X-ray selected sources. The authors have studied the X-ray source counts in four energy bands: soft (0.5 - 2 keV), hard (2 - 10 keV), XID (0.5 - 4.5 keV) and ultra-hard (4.5 - 7.5 keV) in order to evaluate the contribution of sources at different fluxes to the X-ray background. They have also studied the angular clustering of X-ray sources in those bands. AXIS (An XMM International Survey) is a survey of 36 high Galactic latitude XMM observations covering 4.8 square degrees in the Northern sky and containing 1433 serendipitous X-ray sources detected with 5-sigma significance. This survey has similar depth to the XMM catalogs and therefore serves as a pathfinder to explore their possibilities. The authors in their paper combined this survey with shallower and deeper surveys, and fitted the source counts with a Maximum Likelihood technique. Using only AXIS sources they studied the angular correlation using a novel robust technique. The AXIS source counts results are compatible with most previous samples in the soft, XID, ultra-hard and hard bands. This study has improved on previous results in the hard band. The fractions of the XRB resolved in the surveys used in this work are 87%, 85%, 60% and 25% in the soft, hard, XID and ultra-hard bands, respectively. Extrapolation of the source counts to zero flux is not sufficient to saturate the XRB intensity. Only galaxies and/or absorbed AGN could contribute the remaining unresolved XRB intensity. These results are compatible, within the errors, with recent revisions of the XRB intensity in the soft and hard bands. The maximum fractional contribution to the XRB comes from fluxes within about a decade of the break in the source counts (~10<sup>-14</sup> cgs), reaching ~50% of the total in the soft and hard bands. Angular clustering (widely distributed over the sky and not confined to a few deep fields) is detected at 99-99.9% significance in the soft and XID bands, with no detection in the hard and ultra-hard band (probably due to the smaller number of sources). The authors cannot confirm the detection of significantly stronger clustering in the hard-spectrum hard sources. Medium-depth surveys such as AXIS are essential to determine the evolution of the X-ray emission in the Universe below 10 keV. Included here are the basic data for the 2560 X-ray sources in the reference paper which satified the selection criteria of having an emldetect detection likelihood >= 10 (the default value) in at least one band, namely: (i) XMM-Newton pn count-rates in four XMM-Newton Science Analysis System (SAS) bands (band 2: 0.5 - 2 keV, band 3: 2 - 4.5 keV, band 4: 4.5 - 7.5 keV, band 5: 7.5 - 12 keV); (ii) spectral photon indices in the 0.5 - 4.5 keV band, the 2 - 10 keV band and the 0.5 - 10 keV band; (iii) fluxes in the soft (0.5 - 2 keV), hard (2 - 10 keV), XID (0.5 - 4.5 keV), ultra-hard (4.5 - 7.5 keV) and "total" (0.5 - 10 keV) bands; and (iv) flags describing to which of the samples discussed in the paper (soft, hard, XID or ultra-hard) each source belongs. There is no spectral or flux information given for the sources not belonging to any of the samples, but the count-rates of such sources are given for completeness. This table was created by the HEASARC in August 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/469/27">CDS catalog J/A+A/469/27</a> file table23.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/baxgalclus
- Title:
- BAX X-Ray Galaxy Clusters and Groups Catalog
- Short Name:
- BAXGalClus
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see <a href="http://bax.ast.obs-mip.fr/">http://bax.ast.obs-mip.fr/</a> for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at <a href="http://bax.ast.obs-mip.fr/">http://bax.ast.obs-mip.fr/</a>) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck. This table was created by the HEASARC in October 2004 based on CDS table B/bax/bax.dat. This is a service provided by NASA HEASARC .
69. BBXRT Archive
- ID:
- ivo://nasa.heasarc/bbxrt
- Title:
- BBXRT Archive
- Short Name:
- BBXRT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The BBXRT database table contains information about each observation made by the Broad Band X-Ray Telescope. It includes a catalog of observations and spectral and lightcurve products for each of the 10 pixels per observation. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxao
- Title:
- BeppoSAX Approved Pointings
- Short Name:
- SAXAO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The SAXAO database contains the list of the all accepted AO1/AO2/AO3/A04/AO5 SAX CORE and GO program proposals, approved for the first year of operations. The database also includes targets scheduled for the Science Verification Phase (SVP) (from launch, 30 April 1996, till August 1996). The CORE program includes proposals led by Principal Investigator belonging to Italian or Dutch institutions, to the Space Science Department of ESA or to the Max Planck Institute for Extraterrestial Physics in Garching. Approximately 80 percent of the first year observing time is allocated to the CORE program. The remaining 20 percent of time for the first year operations is reserved for the GO program. For the AO2 60 percent is allocated to the CORE program and 40 percent to the GO. For the AO3 and AO4 50 percent is allocated to the CORE program and 50 percent to the GO. More information on the SAX mission is available at the following address <a href="http://www.asdc.asi.it">http://www.asdc.asi.it</a> and also <a href="https://heasarc.gsfc.nasa.gov/docs/sax/saxgof.html">https://heasarc.gsfc.nasa.gov/docs/sax/saxgof.html</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxgrbmgrb
- Title:
- BeppoSAX/GRBM Gamma-Ray Burst Catalog
- Short Name:
- SAXGRBMGRB
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This is the catalog of gamma-ray bursts (GRBs) detected with the Gamma Ray Burst Monitor (GRBM) aboard the BeppoSAX satellite. It includes 1082 GRBs with 40 - 700 keV fluences in the range from 1.3 x 10<sup>-7</sup> to 4.5 x 10<sup>-4</sup> erg/cm<sup>2</sup>, and 40 - 700 keV peak fluxes from 3.7x10<sup>-8</sup> to 7.0 x 10<sup>-5</sup> erg/cm<sup>2</sup>/s. Some relevant parameters of each GRB are reported in the catalog. This table was created by the HEASARC in January 2010 based on the CDS catalog J/ApJS/180/192, file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxhellasr
- Title:
- BeppoSAX High-Energy Large Area Survey (HELLAS) Radio Source Catalog
- Short Name:
- SAXHELLASR
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results of a complete radio follow-up obtained with the VLA and ATCA radio telescopes down to a 6-cm flux limit of about 0.3 mJy (3-sigma) of all the 147 X-ray sources detected in the BeppoSAX HELLAS survey (Fiore et al. 2001, MNRAS, 327, 771). The authors found 53 X-ray/radio likely associations, corresponding to about one-third of the X-ray sample. Using the two-point spectral index alpha<sub>ro</sub> = 0.35 they divided all the HELLAS X-ray sources into radio-quiet and radio-loud. They have 26 sources classified as radio-loud objects, corresponding to 18 per cent of the HELLAS sample. In agreement with previous results, the identified radio-loud sources are associated mainly with Type 1 active galactic nuclei (AGNs) with L<sub>5-10keV</sub> >~ 10<sup>44</sup> erg/s, while all the identified Type 2 AGNs and emission-line galaxies are radio-quiet objects with L<sub>5-10keV</sub> <~ 10<sup>44</sup> erg/s. The 20 HELLAS sources with Declinations south of -40<sup>o</sup> were observed with the ATCA, while the 127 sources with more northerly Declinations were observed with the VLA. For these latter sources a complete covering at 20 cm down to the 5-sigma flux limit of 2.5 mJy is already available with the NRAO/VLA Sky Survey (NVSS) while the FIRST survey (Faint Images of the Radio Sky at Twenty centimeters) is available only for 27 HELLAS sources (5-sigma limit of ~ 1 mJy).In order to obtain information also on the radio spectral properties of the HELLAS sources the authors adopted the following strategy. All the 147 HELLAS sources were observed at 6 cm down to a 1 -sigma flux limit of ~ 0.10 - 0.25 mJy. For the 20 HELLAS sources observed with the ATCA, they took advantage of the fact that the 6 and 3 cm receivers of the ATCA share a common feed-horn and they observed simultaneously also at 3 cm, obtaining a 3-cm flux limit of ~ 0.22 mJy (1-sigma level). Starting from the radio position of the 53 X-ray/radio associations, the authors searched for optical counterparts within 5 arcseconds from the radio position using the optical positions of the 61 HELLAS sources identified by La Franca et al. (2002, ApJ, 570, 100 = LF02), the USNO-A2.0 1 optical catalog, the APM 2 optical catalog and the NASA Extragalactic Database (NED). 24 X-ray/radio associations have been identified with sources in LF02 (10 Type 1 AGN, 4 Type 2 AGN, 2 BL Lacs, 3 Clusters, 4 ELGs and 1 Radio galaxy), 1 has been identified with a z = 0.708 Radio galaxy in the Lockman Hole using NED (see Table 2 source 116 in Lehmann et al. 2000, A&A, 354, 35 for a description of this source), 13 have an optical (R-band) identification in the USNO and/or APM catalogue while 15 X-ray/radio associations do not have an optical identification brighter than R=20. This table was created by the HEASARC in July 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/342/575">CDS Catalog J/MNRAS/342/575</a> file table1.dat. There was a minor update to the HEASARC's implementation in June 2022 to make the two probability parameters into unitless quantities for improved clarity. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxhellas
- Title:
- BeppoSAX High-Energy Large Area Survey (HELLAS) X-Ray Source Catalog
- Short Name:
- SAXHELLAS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The BeppoSAX High Energy Large Area Survey (HELLAS) has surveyed about 85 deg<sup>2</sup> of sky in the 4.5 - 10 keV band down to a flux of 4 - 5 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s using 142 high Galactic latitude (|b| > 20<sup>o</sup>) observations made by the BeppoSAX Medium Energy Concentrator Spectrometer (MECS). The source surface density of 16.9 +/- 6.4 deg<sup>2</sup> at the survey limit corresponds to a resolved fraction of the 5 - 10 keV X-ray background (XRB) of the order of 20-30 per cent. Hardness ratio analysis indicates that the spectra of a substantial fraction of the HELLAS sources (at least one-third) are harder than a alpha<sub>E</sub> = 0.6 power law. This hardness may be caused by large absorbing columns. The hardness ratio analysis also indicates that many HELLAS sources may have a spectrum more complex than a single absorbed power law. A soft component, superimposed on a strongly cut-off power law, is likely to be present in several sources. There is no overlap among the 142 fields used and, wherever possible, multiple observations of the same field have been merged in one single pointing to increase the sensitivity. Fields were selected among public data (such as that of March 1999) and the authors' proprietary data. Fields centered on bright extended sources and bright Galactic sources were excluded from the survey, as were fields close to the Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC) and M 33. Most of the fields have exposures between 30 and 100 ks, and 20 fields have an exposure higher than 80 ks (see Fig. 1 of reference paper). Sources were detected in images accumulated between 4.5 and 10 keV. Source count rates in four bands (1.3 - 10 keV, total or T; 1.3 - 2.5 keV, low band or L; 2.5 - 4.5 keV, middle band or M; 4.5 - 10 keV, high band or H) were extracted and corrected for the energy-dependent vignetting and for the MECS PSF. The count rates were converted to fluxes using a conversion factor of 7.8 x 10<sup>-11</sup> erg cm<sup>-2</sup> s<sup>-1</sup> (5 - 10 keV flux) per one '3 ECS count' (4.5 - 10 keV) appropriate for a power-law spectrum with alpha<sub>E</sub> = 0:6. The factor is not strongly sensitive to the spectral shape, owing to the narrow band: thus, for alpha<sub>E</sub> = 0.4 and 0.8 it is 8.1 and 7.6 x 10<sup>-11</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, respectively. A conversion factor of 9:9 x 10<sup>-11</sup> erg cm<sup>-2</sup> s<sup>-1</sup> per one '3 MECS count' has been used for sources under the 550 micron (um) beryllium strongback supporting the MECS window to account for the reduced detector sensitivity. This table was created by the HEASARC in July 2014 based on CDS Catalog J/MNRAS/327/771 file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/sax2to10
- Title:
- BeppoSAX 2-10 keV Survey
- Short Name:
- SAX2-10keV
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This catalog presents the results of a 2 - 10 keV BeppoSAX survey based on 140 high galactic latitude Medium Energy Concentrator Spectrometers (MECS) fields, 12 of which are deep exposures of ``blank'' parts of the sky. The limiting sensitivity is 5 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s (or mW/m<sup>2</sup>) where about 25% of the Cosmic X-ray Background (CXB) is resolved into discrete sources. The log N - log S function, built with a statistically complete sample of 177 sources, is steep and in good agreement with the counts derived from ASCA surveys. This database was created by the HEASARC in December 2000 based upon <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/362/799">CDS Catalog J/A+A/362/799</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxnfilog
- Title:
- BeppoSAX NFI Archive and Observation Log
- Short Name:
- SAXNFI
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The SAXNFILOG database contains the SAX Narrow Field Instruments (NFI) approved pointings, but it also served as an observations log. It includes data taken during AO1, AO2, AO3, A04 and AO5 cycles and the Science Verification Phase (SVP). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxwfclog
- Title:
- BeppoSAX WFC Observation Log
- Short Name:
- SAXWFC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The SAXWFCLOG database contains the SAX WFCs observations log for the AO cycles and the Science Verification Phase (SVP). The two WFCs are located at 90 degrees from the NFI and set 180 degrees apart. The field of view is 40 deg X 40 deg and the coordinates given in this databases are the pointing positions. The database is updated regularly to include the most recent timeline, and updates are provided by the SAX-Science Data Center in Rome. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxwfccat2
- Title:
- BeppoSAX Wide Field Camera Unbiased X-Ray Source Catalog
- Short Name:
- SAXWFCCAT2
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- During the operational life of the Italian/Dutch X-ray satellite (1996-2002), BeppoSAX, its two Wide Field Cameras (WFCs) performed observations that covered the full sky at different epochs. Although the majority of the analyses performed on BeppoSAX WFC data concentrated on the detection of transient sources, the authors have now applied the same techniques developed for the INTEGRAL/IBIS survey so as to produce a similar analysis of the BeppoSAX WFC data. This work represents the first unbiased source list compilation produced from the overall WFC data set which is optimized for faint persistent source detection. This approach recovered 182 more sources compared to the previous WFC catalog reported in Verrecchia et al. (2007, A&A, 472, 705; the HEASARC SAXWFCCAT table). The present catalog contains 404 sources detected between 3 and 17 keV, 10 of which are yet to be seen by the new generation of telescopes. This table was created by the HEASARC in July 2011 based on an electronic version of Table 3 from the reference paper which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/saxwfccat
- Title:
- BeppoSAX Wide Field Camera X-Ray Source Catalog
- Short Name:
- SAXWFCCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the catalog of X-ray sources detected by the two Wide Field Cameras (WFCs) in complete observations on board BeppoSAX during its 6 years of operational lifetime, i.e., between April 1996 and April 2002. The BeppoSAX WFCs were coded mask instruments sensitive in the 2 - 28 keV energy band with a 40 x 40 square degree fields of view, pointing in opposite directions and perpendicularly to the BeppoSAX Narrow Field Instruments (NFI). The WFCs were usually operated simultaneously to NFI observations, each lasting up to several days. The WFCs observed thus the entire sky several times with a typical sensitivity of 2 to 10 mCrab. A systematic analysis of all WFC observations in the BeppoSAX archive has been carried out using the latest post-mission release of the WFC analysis software and calibrations. The catalog includes 253 distinct sources, obtained from a total sample of 8253 WFC detections. This table was created by the HEASARC in November 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/472/705">CDS catalog J/A+A/472/705</a> file table3.dat. This is a service provided by NASA HEASARC .
79. Be Stars Catalog
- ID:
- ivo://nasa.heasarc/bestars
- Title:
- Be Stars Catalog
- Short Name:
- Be
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The BESTARS database tables contains a compilation of data concerning stars of type Be. For the purposes of this compilation, a Be star is defined as a non-supergiant B star which showed emission in one Balmer line at least once. Stars without published MK spectral types have been excluded, except for 132 stars from Bidelman and MacConnell (1973), who used the above definition but included no spectral types. There are 1,159 stars included in this list. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/askapbeta
- Title:
- BETA Pilot Multi-Epoch Continuum Survey of Spitzer SPT Deep Field
- Short Name:
- ASKAPBETA
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Boolardy Engineering Test Array (BETA) is a 6 x 12m-dish interferometer and the prototype of the Australian Square Kilometre Array Pathfinder (ASKAP), equipped with the first generation of ASKAP's phased array feed (PAF) receivers. These facilitate rapid wide-area imaging via the deployment of simultaneous multiple beams within an ~30 deg<sup>2</sup> field of view. By cycling the array through 12 interleaved pointing positions and using nine digitally formed beams, the authors have effectively mimicked a traditional 1 hours x 108 pointing survey, covering ~150 deg<sup>2</sup> over 711-1015 MHz in just 12 hours of observing time. Three such observations were executed over the course of a week. The authors verified the full bandwidth continuum imaging performance and stability of the system via self-consistency checks and comparisons to existing radio data. The combined three epoch image has arcminute resolution and a 1-sigma thermal noise level of 375 µJy/beam, although the effective noise is a factor of ~3 higher due to residual sidelobe confusion. From this, the authors have derived a catalog of 3,722 discrete radio components, using the 35% fractional bandwidth to measure in-band spectral indices for 1037 of them. A search for transient events reveals one significantly variable source within the survey area. The survey covers approximately two-thirds of the Spitzer South Pole Telescope (SPT) Deep Field. This pilot project demonstrates the viability and potential of using PAFs to rapidly and accurately survey the sky at radio wavelengths. The target field was observed with BETA on three separate occasions as part of the commissioning and verification of the instrument. The telescope delivers 304 MHz of instantaneous bandwidth and for these observations the sky frequency range was 711-1015 MHz, corresponding to a fractional bandwidth of 35%. The data were captured with a frequency resolution of 18.5 kHz, using 16,416 frequency channels across the band. The PYBDSM source finder was used to extract a component catalog from the deep mosaic image formed from a combination of all epochs and sub-bands. Components were fit to islands of emission that had a peak brightness of >5 sigma and an island boundary threshold of >3 sigma, where sigma is the local estimate of the background noise level. Component spectral indices were assigned by matching positions at which spectral indices were successfully fit (Section 4.5 of the reference paper). Following the excision of some spurious detections at the noisy edge of the mosaic, the final catalog contains 3,722 components, 1,037 of which have in-band spectral index measurements. This table was created by the HEASARC in March 2017 based on CDS Catalog J/MNRAS/457/4160 file table3.dat, the list of source components found in the ASKAP-BETA Survey covering two-thirds of the Spitzer SPT Deep Field. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/bootesdf
- Title:
- Bootes Deep Field WSRT 1.4-GHz Source Catalog
- Short Name:
- Bootes
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This radio source catalog is the result of deep (16x12 hour) Westerbork Synthesis Radio Telescope (WSRT) observations of the approximately 7 square degree Bootes Deep Field, centered at an RA and Declination (J2000) of 14 hr 32 min 5.75 sec, +34 deg 16 arcmin 47.5 arcsec. The survey consisted of 42 discrete pointings, with enough overlap to ensure a uniform sensitivity across the entire field, and with a limiting sensitivity of 28 microJansky (1 sigma rms). The catalog consists of 3172 distinct sources detected with a significance of 5 sigma or greater, of which 316 are resolved by the 13 x 27 arcsec beam. This database table was created by the HEASARC in December 2001 based on the a data file obtained from the authors' FTP site (no longer available). It was modified slightly in March 2011 (using the CDS data file <a href="ftp://cdsarc.u-strasbg.fr/pub/cats/J/AJ/123/1784/catalog.dat">ftp://cdsarc.u-strasbg.fr/pub/cats/J/AJ/123/1784/catalog.dat</a>) to make the source names adhere to the naming convention of the Dictionary of Nomenclature of Celestial Objects. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/boof153mhz
- Title:
- Bootes Field GMRT 153-MHz Source Catalog
- Short Name:
- BOOF153MHZ
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors obtained deep, high-resolution radio interferometric observations at 153 MHz to complement the extensively studied NOAO Bootes field. In their paper, they provide a description of the observations, data reduction and source catalog construction. From their single-pointing GMRT observation of ~12 hours, they obtained a high-resolution (26" x 22") image of ~11.3 square degrees, fully covering the Bootes field region and beyond. The image has a central noise level of ~1.0 mJy beam<sup>-1</sup>, which rises to 2.0 - 2.5 mJy beam<sup>-1</sup> at the field edge, placing it amongst the deepest ~150 MHz surveys to date. The catalog of 598 extracted sources is estimated to be ~92% complete for > 10 mJy sources, while the estimated contamination by false detections is < 1%. The low rms positional uncertainty of 1.24" facilitates accurate matching against catalogs at optical, infrared and other wavelengths. Differential source counts were determined down to < ~10 mJy. The authors find no evidence for flattening of the counts towards lower flux densities as observed in deep radio surveys at higher frequencies, suggesting that their catalog is dominated by the classical radio-loud AGN population that explains the counts at higher flux densities. Combination with available deep 1.4 GHz observations yields an accurate determination of spectral indices for 417 sources down to the lowest 153 MHz flux densities, of which 16 have ultra-steep spectra with spectral indices below -1.3. The authors confirm that flattening of the median spectral index towards low flux densities also occurs at this frequency. The detection fraction of the radio sources in the NIR K<sub>s</sub>-band is found to drop with radio spectral index, which is in agreement with the known correlation between spectral index and redshift for brighter radio sources. This table contains the list of 598 153-MHz sources detected in the GMRT observation and their properties at this frequency. There are a number of other tables of objects in the Bootes field made at other frequencies: <pre> HEASARC Table | Title | Reference BOOTESDF | 1.4GHz imaging of the Bootes field | de Vries+ 2002,AJ,123,1784 LALABOOCXO | LALA Bootes field X-ray source catalog | Wang+ 2004,AJ,127,213 --- | Faint radio sources in NOAO Bootes field | Wrobel+ 2005,AJ,130,923 --- | 16um sources in the NOAO Bootes field | Kasliwal+ 2005,ApJ,634,L1 XBOOTES | X-ray survey of the NDWFS Bootes field | Kenter+ 2005,ApJS,161,9 XBOOTESOID | Optical counterparts in the NDWFS Bootes | Brand+ 2006,ApJ,64,140 | field | </pre> This table was created by the HEASARC in December 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/535/A38">CDS Catalog J/A+A/535/A38</a> file table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/bmwchancat
- Title:
- Brera Multi-scale Wavelet Chandra Source Catalog
- Short Name:
- BMWCHANCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the BMW-Chandra source catalog drawn from essentially all Chandra ACIS-I pointed observations with an exposure time in excess of 10 ks that were public as of March 2003 (136 observations). Using the wavelet detection algorithm developed by Lazzati et al. (1999ApJ...524..414) and Campana et al. (1999ApJ...524..423C), which can characterize both point-like and extended sources, the authors identified 21325 sources. Among them, 16758 are serendipitous, i.e. not associated with the targets of the pointings, and do not require a non-automated analysis. This makes this catalog the largest compilation of Chandra sources as of the date of publication of this catalog (August 2008). The 0.5 - 10 keV absorption corrected fluxes of these sources range from ~3 x 10<sup>-16</sup> to 9 x 10<sup>-12</sup> erg/cm<sup>2</sup>/s with a median of 7 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s. The catalog consists of count rates and relative errors in three energy bands (total, 0.5 - 7 keV; soft, 0.5 - 2 keV; and hard, 2 - 7 keV), and source positions relative to the highest signal-to-noise detection among the three bands. The wavelet algorithm also provides an estimate of the extension of the source. The authors include information drawn from the headers of the original files, as well, and extracted source counts in four additional energy bands, SB1 (0.5 - 1 keV), SB2 (1 - 2 keV), HB1 (2 - 4 keV), and HB2 (4 - 7 keV). They computed the sky coverage for the full catalog and for a subset at high Galactic latitude (|b| > 20 degrees). The complete catalog provides a sky coverage in the soft band (0.5 - 2 keV, S/N = 3) of ~8 deg<sup>2</sup> at a limiting flux of 10<sup>-13</sup> erg/cm<sup>2</sup>/s, and ~2 deg<sup>2</sup> at a limiting flux of ~10<sup>-15</sup> erg/cm<sup>2</sup>/s. The total numbers of matches with the FIRST, IRASPSC, 2MASS, and GSC2 catalogs obtained after a closest-distance selection are 13, 87, 6700, and 4485, respectively. This table was created by the HEASARC in September 2008 based on the CDS table J/A+A/488/1221 file catalog.dat. The catalog version is BMC 1.0.1F. All sources in this version of the catalog were from observations in POINTING and TIMED ACIS read modes. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/bmwhricat
- Title:
- Brera Multi-scale Wavelet ROSAT HRI Source Catalog
- Short Name:
- BMW-HRI
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Brera Multi-scale Wavelet ROSAT High Resolution Imager Source Catalog (BMW-HRI) is derived from all ROSAT HRI pointed observations with exposure time longer than 100 seconds available in the ROSAT public archives. The data were analyzed automatically using a wavelet detection algorithm suited to the detection and characterization of both point-like and extended sources. This algorithm is able to detect and disentangle sources in very crowded fields and/or in presence of extended or bright sources. Images have been also visually inspected after the analysis to ensure verification. The final catalog, derived from 4,303 observations, consists of 29,089 sources detected with a detection probability of greater or equal 4.2 sigma. For each source, the primary catalog entries provide name, position, count rate, flux and extension along with the relative errors. In addition, results of cross-correlations with existing catalogs at different wavelengths (FIRST, IRAS, 2MASS, and GSC2) are also reported. As an external check, the authors compared their catalog with the previously available ROSHRICAT catalog (both in its short and long versions) and were able to recover, for the short version, ~90% of the entries. The sky coverage of the entire HRI data set was computed by means of simulations. The complete BMW-HRI catalog provides a sky coverage of 732 square degrees down to a limiting flux of ~1x10<sup>-12</sup> erg/s/cm<sup>2</sup> and of 10 square degrees down to ~1x10<sup>-14</sup> erg/s/cm<sup>2</sup>. The authors were able to compute the cosmological log(N)-log(S) distribution down to a flux of about 1.2x10<sup>-14</sup> erg/s/cm<sup>2</sup>. This catalog was ingested by the HEASARC in March 2003, based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/IX/34">CDS Catalog IX/34</a> file catalog.dat.gz. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/bnmdspecat
- Title:
- Brightest M Dwarfs in the Northern Sky Spectroscopic Catalog
- Short Name:
- BNMDSPECAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a spectroscopic catalog of the 1564 brightest (J < 9<sup>m</sup>) M-dwarf candidates in the northern sky, as selected from the SUPERBLINK proper-motion catalog (Lepine and Shara 2005, AJ, 129, 1483). Observations confirm 1408 of the candidates to be late-K and M dwarfs with spectral subtypes K7 - M6. From the low (mu > 40 mas yr<sup>-1</sup>) proper motion limit and high level of completeness of the SUPERBLINK catalog in that magnitude range, the authors estimate that their spectroscopic census most likely includes > 90% of all existing, northern-sky M dwarfs with apparent magnitude J < 9<sup>m</sup>. Only 682 stars in this sample are listed in the Third Catalog of Nearby Stars (CNS3, Gliese and Jahreiss 1991); most others are relative unknowns and have spectroscopic data presented here for the first time. Spectral subtypes are assigned based on spectral index measurements of CaH and TiO molecular bands; a comparison of spectra from the same stars obtained at different observatories, however, reveals that spectral band index measurements are dependent on spectral resolution, spectrophotometric calibration, and other instrumental factors. As a result, the authors find that a consistent classification scheme requires that spectral indices be calibrated and corrected for each observatory/instrument used. After systematic corrections and a recalibration of the subtype-index relationships for the CaH2, CaH3, TiO5, and TiO6 spectral indices, the authors find that they can consistently and reliably classify all the stars to a half-subtype precision. The use of corrected spectral indices further requires them to recalibrate the zeta parameter, a metallicity indicator based on the ratio of TiO and CaH optical bandheads. However, the authors find that their zeta values are not sensitive enough to diagnose metallicity variations in dwarfs of subtypes M2 and earlier (+/- 0.5 dex accuracy) and are only marginally useful at later M3-M5 subtypes (+/- 0.2 dex accuracy). Fits of their spectra to the Phoenix atmospheric model grid are used to estimate effective temperatures. These suggest the existence of a plateau in the M1-M3 subtype range, in agreement with model fits of infrared spectra but at odds with photometric determinations of T<sub>eff</sub>. Existing geometric parallax measurements are extracted from the literature for 624 stars, and are used to determine spectroscopic and photometric distances for all the other stars. Active dwarfs are identified from measurements of H-alpha equivalent widths, and the authors find a strong correlation between H-alpha emission in M dwarfs and detected X-ray emission from ROSAT and/or a large UV excess in the GALEX point source catalog. Proper motion data and photometric distances are combined in order to evaluate the (U, V, W) distribution in velocity space, which is found to correlate tightly with the velocity distribution of G dwarfs in the solar neighborhood. However, active stars show a smaller dispersion in their space velocities, which is consistent with those stars being younger on average. The authors state that this catalog will be very useful for guiding the selection of the best M dwarf targets for exoplanet searches, in particular those using high-precision radial velocity measurements. This online catalog was created by the HEASARC in June 2013 based on a machine-readable version of Tables 1, 3 and 7 from the paper which were obtained from the AJ website (Tables 1 and 3) or from the first author (Table 7). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/at20gbspol
- Title:
- Bright Extra-Galactic AT20G Sources Polarizations Catalog
- Short Name:
- AT20GBSPOL
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains polarization data for 180 extragalactic sources extracted from the Australia Telescope 20-GHz (AT20G) survey catalog and observed with the Australia Telescope Compact Array (ATCA) during a dedicated, high sensitivity run (sigma<sub>P</sub> ~ 1 mJy). For the sake of completeness, the authors extracted the polarization information for seven extended sources from the 9-yr Wilkinson Microwave Anisotropy Probe co-added maps at 23 GHz. The full sample of 187 sources constitutes a ~ 99% complete sample of extragalactic sources brighter than S<sub>20GHz</sub> = 500 mJy at the selection epoch with Declination below -30<sup>o</sup>. The sample has a 91.4% detection rate in polarization at ~ 20 GHz (94% if considering the sub-sample of point-like sources). The authors have measurements also at 4.8 and 8.6 GHz within ~1 month of the 20-GHz observations for 172 sources so as to reconstruct the spectral properties of the sample in total intensity and in polarization: 143 of them have a polarization detection at all three frequencies. The authors find that there is no statistically significant evidence of a relationship either between the fraction of polarization and frequency or between the fraction of polarization and the total intensity flux density. This indicates that Faraday depolarization is not very important above 4.8 GHz and that the magnetic field is not substantially more ordered in the regions dominating the emission at higher frequencies (up to 20 GHz). The authors estimate the distribution of the polarization fraction and the polarized flux density source counts at ~20 GHz. The selection of the sample was based on the list of confirmed AT20G sources available at the epoch of these observations (2006 October). The authors selected all objects with flux density S<sub>20GHz</sub> > 500 mJy and Declination below -30<sup>o</sup>, excluding the Galactic plane region (|b| <= 1.5o^) and the Large Magellanic Cloud (LMC) region (inside a circle of 5.5<sup>o</sup> radius centered at RA =05:23:34.7 and Dec=-69:45:22 in J2000.0 coordinates). This resulted in a complete sample of 189 sources. The observations were taken on October 1, 2006 using the most compact hybrid configuration of ATCA, H75, excluding the data from the farthest antenna. The longest baseline of this configuration is 75 m, and its T-shape ensures adequate Fourier coverage for snapshots taken on a relatively small range of hour angles and at high elevation. In a number of cases, indicated by source_flags values of 's', 'f' or 'w', the highest frequency data is not at 18 GHz, but at 20 or 23 GHz. This table was created by the HEASARC in January 2015 based on the CDS Catalog J/MNRAS/436/2915 file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mdwarfasc
- Title:
- Bright M Dwarf All-Sky Catalog
- Short Name:
- MDWARFASC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains an all-sky catalog of M dwarf stars with apparent infrared magnitude J < 10. The 8889 stars are selected from the ongoing SUPERBLINK survey of stars with proper motion mu > 40 mas yr<sup>-1</sup>, supplemented on the bright end with the Tycho-2 catalog. Completeness tests which account for kinematic (proper motion) bias suggest that this catalog represents ~75% of the estimated ~11,900 M dwarfs with J < 10 expected to populate the entire sky. The catalog is, however, significantly more complete for the northern sky (~90%) than it is for the south (~60%). Stars are identified as cool, red M dwarfs from a combination of optical and infrared color cuts, and are distinguished from background M giants and highly reddened stars using either existing parallax measurements or, if such measurements are lacking, using their location in an optical-to-infrared reduced proper motion diagram. These bright M dwarfs are all prime targets for exoplanet surveys using the Doppler radial velocity or transit methods; the combination of low-mass and bright apparent magnitude should make possible the detection of Earth-size planets on short-period orbits using currently available techniques. Parallax measurements, when available, and photometric distance estimates are provided for all stars, and these place most systems within 60 pc of the Sun. Spectral type estimated from V-J color shows that most of the stars range from K7 to M4, with only a few late M dwarfs, all within 20 pc. Proximity to the Sun also makes these stars good targets for high-resolution exoplanet imaging searches, especially if younger objects can be identified on the basis of X-ray or UV excess. For that purpose, we include X-ray flux from ROSAT and FUV/NUV ultraviolet magnitudes from GALEX for all stars for which a counterpart can be identified in those catalogs. Additional photometric data include optical magnitudes from Digitized Sky Survey plates and infrared magnitudes from the Two Micron All Sky Survey. This table was first created by the HEASARC in October 2011 based on electronic versions of Tables 1 and 2 from the reference paper which were obtained from the AJ web site. A slightly revised version based on corrected versions of the input tables received from the author was ingested in December 2011. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/bsc5p
- Title:
- Bright Star Catalog
- Short Name:
- BSC
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The BSC5P database table contains data derived from the Bright Star Catalog, 5th Edition, preliminary, which is widely used as a source of basic astronomical and astrophysical data for stars brighter than magnitude 6.5. The database contains the identifications of included stars in several other widely-used catalogs, double- and multiple-star identifications, indication of variability and variable-star identifiers, equatorial positions for B1900.0 and J2000.0, galactic coordinates, UBVRI photoelectric photometric data when they exist, spectral types on the Morgan-Keenan (MK) classification system, proper motions (J2000.0), parallax, radial- and rotational-velocity data, and multiple-star information (number of components, separation, and magnitude differences) for known non-single stars. This table was created by the HEASARC in 1995 based upon a file obtained from either the ADC or the CDS. A number of revisions have been made by the HEASARC to this original version, e.g., celestial positions were added for the 14 non-stellar objects which have received HR numbers: HR 92, 95, 182, 1057, 1841, 2472, 2496, 3515, 3671, 6309, 6515, 7189, 7539 and 8296. In January 2014, the very incorrect position for HR 3671 = NGC 2808 was fixed (the Declination is -65 degrees not +65 degrees!), and smaller corrections were made to the positions of HR 2496, 3515 and 6515 so as to bring them in better agreement with the positions listed in SIMBAD and NED This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/bhrfscid
- Title:
- Byurakan/Hamburg/ROSAT Catalog of Optical IDs
- Short Name:
- BHROSATOpt.
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog <IX/29>) with galactic latitude |b| >= 30 degrees, declination >= 0 degrees, and ROSAT PSPC count rate CR > 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources. This table was created by the HEASARC in June 2006 based on CDS table J/A+A/449/425/table1.dat This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cyder
- Title:
- Calan-Yale Deep Extragalactic Research Survey X-Ray Source Catalog
- Short Name:
- CYDER
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The main goal of the Calan-Yale Deep Extragalactic Research (CYDER) Survey X-ray survey is to study serendipitous X-ray sources detected by Chandra in an intermediate flux range (10<sup>-15</sup> to 10<sup>-12</sup> ergs/s) that comprises most of the X-ray background. A total of 267 X-ray sources spread over five archived fields were detected. The log N - log S distribution obtained for this sample is consistent with the results of other surveys. Deep V and I images were taken of these fields in order to calculate X-ray-to-optical flux ratios. Identifications and redshifts were obtained for 106 sources using optical spectroscopy from 8 m class telescopes to reach the optically faintest sources, to the same level as deeper X-ray fields like the Chandra Deep Fields, showing that the nature of sources detected depends mostly on the optical limit for spectroscopy. This table was created by the HEASARC in March 2007 based on the CDS table J/ApJ/621/104, file table4.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/calchdmstr
- Title:
- CALET CHarge Detector (CHD) Master Catalog
- Short Name:
- CALCHDMSTR
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The CALCHDMSTR database table records high-level information of the lightcurves obtained with the CHarge Detector (CHD), the top layer of the calorimeter instrument on the CALorimetric Electron Telescope (CALET) mission. CALET is a Japanese mission led by JAXA, in collaboration with the Italian Space Agency (ASI) and NASA, and is dedicated to the study of high energy cosmic rays. CALET was launched on August 19, 2015, by a Japanese carrier, H2 Transfer Vehicle, and robotically installed on the Japanese Experiment Module-Exposed Facility (JEM-EF) on the International Space Station (ISS). CALET started scientific observations in October, 2015. The CALET CHD lightcurves are delivered by the CALET team in Japan as ASCII files to the DARTS archive located at ISAS (Japan). The HEASARC developed software to create the FITS versions of the lightcurves. This is run at DARTS, and the output is placed online at <a href="https://darts.isas.jaxa.jp/astro/calet/">https://darts.isas.jaxa.jp/astro/calet/</a>. The HEASARC hosts a copy of these lightcurves and generates this database table by collecting high-level information from the data. The Data and the database table are updated regularly during operation. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/calgbmmstr
- Title:
- CALET Gamma-Ray Burst Monitor (GBM) Master Catalog
- Short Name:
- CALGBMMSTR
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The CALGBMMSTR database table records high-level information of the observations obtained with the CALET Gamma-ray Burst Monitor (CGBM), the second scientific payload on the CALorimetric Electron Telescope (CALET) mission. The Gamma-ray Burst Monitor provides a broadband energy coverage from 7 keV to 20 MeV and simultaneous observations with the primary instrument CALET Calorimeter (CCAL) in the GeV - TeV gamma-ray range and with the Advanced Star Camera (ASC) in the optical for gamma-ray bursts (GRBs) and other X-ray/gamma-ray transients. CALET is a Japanese mission led by JAXA, in collaboration with the Italian Space Agency (ASI) and NASA, and it is dedicated to the study of high energy cosmic rays. CALET was launched on August 19, 2015, by a Japanese carrier, H2 Transfer Vehicle, and robotically installed on the Japanese Experiment Module-Exposed Facility (JEM-EF) on the International Space Station (ISS). CALET started scientific observations in October, 2015. The CALET GBM Team in collaboration with DARTS and HEASARC developed the FITS file structure for the GBM data and their archive. The CALET GBM data are delivered by the CALET GBM team in Japan to the DARTS archive located at ISAS (Japan). The HEASARC hosts a copy of these data and generates this database table by collecting high-level information from the data. The data and the database table are updated regularly during operation. The first data release includes PH and TH data. Event data and the image from the ASC are added in a second phase. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cgpsngpcat
- Title:
- Canadian Galactic Plane Survey (CGPS) 1420-MHz Compact Source Catalog
- Short Name:
- CGPSNGPCAT
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a catalog of compact sources of radio emission at 1420 MHz in the northern Galactic plane from the Canadian Galactic Plane Survey (CGPS). The catalog contains 72,758 compact sources with an angular size less than 3 arcminutes within the Galactic longitude range 52 < l<sub>II</sub> < 192 degrees down to a 5-sigma detection level of ~1.2 mJy. Linear polarization properties are included for 12,368 sources with signals greater than 4 x sigma<sub>QU</sub> in the CGPS Stokes Q and U images at the position of the total intensity peak. In the reference paper, the authors compare the CGPS flux densities with the catalogued flux densities in the Northern VLA Sky Survey (NVSS) catalog for 10,897 isolated unresolved sources with CGPS flux density greater than 4 mJy in order to search for sources that show variable flux density on timescales of several years. They identify 146 candidate variables that exhibit high fractional variations between the two surveys. In addition, they identify 13 candidate transient sources that have CGPS flux density above 10 mJy but that are not detected in the NVSS. In the CGPS, the Synthesis Telescope at the Dominion Radio Astrophysical Observatory (the DRAO ST) provided arcminute-resolution images of the radio continuum and atomic-hydrogen line emission of the northern Galactic Plane. The CGPS DRAO radio continuum observations provided images of Stokes I, Q, and U in four 7.5-MHz sub-bands spanning 35 MHz, centered on 1420 MHz. The observations were carried out in three phases beginning in 1995 and ending in 2009. The sky coverage of each phase and the observing dates are listed in Table 1 of the reference paper. The Galactic plane was covered with a width in Galactic latitude of 9 degrees, centered at b<sub>II</sub> = 1 degree to accommodate the warp of the Galactic disk. The longitude coverage was constrained by the southern Declination limit of ~20 degrees, the range that could be effectively imaged by a linear east-west synthesis telescope array. The Phase II observations included an extension to higher latitudes (b<sub>II</sub> = 17.5 degrees) over a restricted range of longitude. In this table, we present the CGPS 1420-MHz compact source catalog covering 1,464 square degrees and spanning a range of 140 degrees of Galactic longitude between 52 and 192 degrees. This table was created by the HEASARC in June 2017 based upon a machine-readable version of Table 2 from the reference paper that was obtained from the AJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/candelscxo
- Title:
- CANDELS H-Band Selected Chandra Source Catalog
- Short Name:
- CANDELSCXO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Improving the capabilities of detecting faint X-ray sources is fundamental to increase the statistics on faint high-z AGN and star-forming galaxies. The authors performed a simultaneous maximum likelihood point-spread function (PSF) fit in the 0.5-2 keV and 2-7 keV energy bands of the 4 Ms Chandra Deep Field South (CDFS) data at the position of the 34,930 CANDELS H-band selected galaxies. For each detected source, they provide X-ray photometry and optical counterpart validation. The authors validated this technique by means of a ray-tracing simulation, and detected a total of 698 X-ray point-sources with a likelihood L > 4.98 (i.e.> 2.7sigma). They show that the prior knowledge of a deep sample of Optical-NIR galaxies leads to a significant increase of the detection of faint (i.e. ~ 10<sup>-17</sup> erg s<sup>-1</sup> cm<sup>-2</sup> in the 0.5-2 keV band) sources with respect to "blind" X-ray detections. By including previous catalogs, this work increases the total number of X-ray sources detected in the 4 Ms CDFS, CANDELS area to 793, which represents the largest sample of extremely faint X-ray sources assembled to date. These results suggest that a large fraction of the optical counterparts of our X-ray sources determined by likelihood ratio actually coincides with the priors used for the source detection. Most of the newly detected sources are likely star-forming galaxies or faint absorbed AGN. The authors identified a few sources with putative photometric redshift z > 4. Despite the low number statistics, this sample significantly increases the number of X-ray selected candidate high-z AGN. The 4-Ms CDFS consists of 23 observations described in Table 1 of Luo et al. (2008, ApJS, 179, 19) plus 31 other pointings described in Xue et al. (2011, ApJS, 195, 10, hereafter X11) for a total exposure of ~4 Ms. For the purpose of this paper, the authors employed only observations taken with a focal temperature of <= -120 C, since at higher temperatures the background cannot be modeled with their technique. This table was created by the HEASARC in July 2016 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/823/95">CDS Catalog J/ApJ/823/95</a> file catalog.dat. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cgmw
- Title:
- Candidate Galaxies Behind the Milky Way
- Short Name:
- CG
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region. This database was created by the HEASARC in October 1999 based on a machine-readable version that was obtained from the CDS Data Center. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cgrabs
- Title:
- Candidate Gamma-Ray Blazar Survey Source Catalog
- Short Name:
- CGRABS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors have constructed a uniform all-sky survey of bright blazars, selected primarily by their flat radio spectra, that is designed to provide a large catalog of likely gamma-ray active galactic nuclei (AGNs). The defined sample, the Candidate Gamma-Ray Blazar Survey (CGRaBS) source catalog, has 1625 targets with radio and X-ray properties similar to those of the EGRET blazars, spread uniformly across the |b| > 10 degrees sky. They also report progress toward optical characterization of the sample; of objects with known red magnitude R < 23, 85% have been classified and 81% have measured redshifts. One goal of this program is to focus attention on the most interesting (e.g., high-redshift, high-luminosity, etc.) sources for intensive multi-wavelength study during the observations by the Large Area Telescope (LAT) on the Gamma-Ray Large-Area Space Telescope (GLAST) satellite observatory. This table was created by the HEASARC in April 2008 based on an electronic version of Table 2 of the reference paper obtained from the electronic ApJS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/carinacxo
- Title:
- Carina Nebula Chandra X-Ray Point Source Catalog
- Short Name:
- CARINACXO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains a catalog of >~ 14,000 X-ray sources observed by the ACIS instrument on the Chandra X-ray Observatory within a 1.42 deg<sup>2</sup> survey of the Great Nebula in Carina, known as the Chandra Carina Complex Project (CCCP). The study from which this table is taken appeared in a special ApJS issue which was devoted to the CCCP. In it, the authors described the data reduction and analysis procedures performed on the X-ray observations, including calibration and cleaning of the X-ray event data, point-source detection, and source extraction. The catalog appears to be complete across most of the field to an absorption-corrected total-band luminosity of ~ 10<sup>30.7</sup> erg s<sup>-1</sup> for a typical low-mass pre-main-sequence star. Counterparts to the X-ray sources were identified in a variety of visual, near-infrared, and mid-infrared surveys. The X-ray and infrared source properties presented herein form the basis of many CCCP studies of the young stellar populations in Carina. The prefixes 'fb', 'sb' and 'hb' on the names of photometric quantities designate the full or total (0.5-8 keV), soft (0.5-2 keV), and hard (2-8 keV) energy bands. Source significance quantities (fb_prob_no_src, sb_prob_no_src, hb_prob_no_src, prob_no_src_min) were computed using a subset of each source's extractions chosen to maximize significance (Broos et al. 2010, ApJ, 714, 1582, hereafter B10, Section 6.2). X-ray source position quantities (RA, Dec, error_radius) were computed using a subset of each source's extractions chosen to minimize the position uncertainty (B10, Sections 6.2 and 7.1). All other quantities were computed using a subset of each source's extractions chosen to balance the conflicting goals of minimizing photometric uncertainty and of avoiding photometric bias (B10, Sections 6.2 and 7). A summary of the counterpart catalogs that were correlated with the Chandra Carina sources is given in Table 5 of the reference paper and is listed below: <pre> Catalog Scope Reference Skiff Visual spectral types Skiff (2009, VizieR Online Data Catalog, 1, 2023) KR Visual photometry Kharchenko & Roeser (2009, VizieR Online Data Catalog, 1280, 0) PPMXL CCD proper motions (PMs) Roeser et al. (2010, AJ, 139, 2440) UCAC3 CCD PMs Zacharias et al. (2004, AJ, 127, 3043) BSS Bright star PMs Urban et al. (2004, VizieR Online Data Catalog, 1294, 0) CMD Photographic PMs, Tr 14, Tr 16, Cr 232 Cudworth et al. (1993, AJ, 105, 1822) DETWC Visual photometry, Tr 14 & 16 DeGioia-Eastwood et al. (2001, ApJ, 549, 578) MDW Visual spectral types, Cr 228 Massey et al. (2001, AJ, 121, 1050) MJ Visual photometry, Tr 14 & 16 Massey & Johnson (1993, AJ, 105, 980) CP High-mass photometry, Cr 228 Carraro & Patat (2001, A&A, 379, 136) DAY Low-mass photometry, Cr 228 Delgado et al. (2007, A&A, 467, 1397) HAWK-I Deep near-infrared photometry Preibisch et al. (2011, ApJS, 194, 10, CCCP HAWK-I Paper) 2MASS Shallow near-infrared photometry Skrutskie et al. (2006, AJ, 131, 1163) SOFI Deep near-infrared photometry, Tr 14 Ascenso et al. (2007, A&A, 476, 199) NACO Deep near-infrared photometry, Tr 14 Ascenso et al. (2007, A&A, 476, 199) Sana Deep near-infrared photometry, Tr 14 Sana et al. (2010, A&A, 515, A26) SpVela Mid-infrared photometry (Spitzer) Povich et al. (2011, ApJS, 194, 14, CCCP IR YSOs Paper) SpSmith Mid-infrared photometry (Spitzer) Smith et al. (2010, MNRAS, 406, 952) AC ACIS observation of Tr 16 Albacete-Colombo et al. (2008, A&A, 490, 1055) </pre> This table was created by the HEASARC in May 2011 based on the electronic versions of Tables 2 and 6 from the reference paper which were obtained from the ApJS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/carinaclas
- Title:
- Carina Nebula Chandra X-Ray Point Source Classes
- Short Name:
- CARINACLAS
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Chandra Carina Complex Project (CCCP) provides a sensitive X-ray survey of a nearby starburst region over > 1 deg<sup>2</sup> in extent. Thousands of faint X-ray sources are found, many concentrated into rich young stellar clusters. However, significant contamination from unrelated Galactic and extragalactic sources is present in the X-ray catalog. In their paper, the authors describe the use of a naive Bayes classifier to assign membership probabilities to individual sources, based on source location, X-ray properties, and visual/infrared properties. For the particular membership decision rule adopted, 75% of CCCP sources are classified as members, 11% are classified as contaminants, and 14% remain unclassified. The resulting sample of stars likely to be Carina members is used in several other studies, which appear in the special issue of Astrophysical Journal Supplement (Volume 194, May 2011 Issue) which was devoted to the CCCP. This table was created by the HEASARC in June 2011 based on the electronic version of Table 5 from the reference paper which was obtained from the ApJS web site. In the input source table, the names were truncated by 3 characters from their complete version. The HEASARC corrected these names, and also obtained the Chandra source positions, using the electronic version of Table 2 from the companion paper (Broos et al. 2011, ApJS, 194, 2: available as the HEASARC Browse table CARINACXO), also obtained from the ApJS web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cargm31cxo
- Title:
- Carina Nebula Gum 31 Chandra X-Ray Point Source Catalog
- Short Name:
- CARGM31CXO
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Gum 31 is a prominent, but still rather poorly studied, HII region around the stellar cluster NGC 3324 at the northwestern periphery of the Carina nebula complex. The aim of the authors aim was to reveal and characterize the young stellar population in Gum 31. An X-ray survey is the only efficient way to identify young stars in this region, which has extremely high galactic field-star contamination, that can avoid the strong biases of infrared-excess-selected samples of disk-bearing young stars. The authors used the Chandra observatory to perform a deep (70 ks) X-ray observation of the Gum 31 region and detected 679 X-ray point sources. This extends and complements the X-ray survey of the central Carina nebula regions performed in the Chandra Carina Complex Project (CCCP, available in the HEASARC database system as the CARINACXO table). Using deep near-infrared images from their recent VISTA survey of the Carina nebula complex, their comprehensive Spitzer point-source catalog, and optical archive data, the authors identify counterparts for 75% of these X-ray sources. The aimpoint of the ACIS-I observation was set to be RA(J2000) = 10<sup>h</sup> 37<sup>m</sup> 36.6<sup>s</sup>, Dec(J2000) = -58<sup>o</sup> 41' 18". This position is close to the center of the H II region, and allows both the stellar cluster NGC 3324 and the cluster G286.38-0.26 to be in the inner parts of the field-of-view, where the point-spread function is still very good. The pointing roll angle (i.e., the orientation of the detector with respect to the celestial north direction) was 138.35<sup>o</sup>. The ACIS field-of-view is just wide enough to cover the full spatial extent of the optically bright Gum 31 H II region and some parts of the surrounding dust shell (see Fig. 1 of the reference paper). The ACIS-I field of view is 17' x 17', which corresponds to 11.3 p x 11.3 pc at the Gum 31 distance of 2.3 kpc). The total net exposure time of the observation was 68,909s (19.14 h). The details of the source detection procedures are described in Section 21. of the reference paper. The final X-ray catalog contains 679 individual point sources. The number of extracted counts ranges from 3 for the faintest sources, up to 920 for the strongest source, while the median value is 11 counts. This table contains the basic X-ray properties and near- and mid-infrared photometry of the X-ray sources detected in the Gum 31 field. The details of the IR matching to the X-ray sources are given in Sections 4.1, 4.2 and 4.3 of the reference paper. This table was created by the HEASARC in May 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/564/A120">CDS Catalog J/A+A/564/A120</a> files table1.dat and table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/carinaxmm
- Title:
- Carina OB1 Association XMM-Newton X-Ray Point Source Catalog
- Short Name:
- CARINAXMM
- Date:
- 03 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains the Carina OB1 Association XMM-Newton X-Ray Point Source Catalog. The X-ray properties of the stellar population in the Carina OB1 Association have been examined with special emphasis on early-type stars. Their spectral characteristics provide some clues to understanding the nature of X-ray formation mechanisms in the winds of single and binary early-type stars. A timing and spectral analysis of five observations with XMM-Newton is performed using various statistical tests and thermal spectral models. 235 point sources have been detected within the field of view. Several of these sources are probably pre-main sequence stars with characteristic short-term variability. Seven sources are possible background AGNs. X-ray count rates in three energy bands and the X-ray variability status are given for 557 detections of the 235 point source. Cross-identifications of X-ray sources with optical and infrared catalogs are also presented. This table was created by the HEASARC in April 2008 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/477/593">CDS Catalog J/A+A/477/593</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .