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Start Over Publisher NASA/GSFC HEASARC Capability Type Table Access Protocol
1. AAVSO International Variable Star Index
ID:
ivo://nasa.heasarc/aavsovsx
Title:
AAVSO International Variable Star Index
Short Name:
AAVSOVSX
Date:
26 Apr 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 .
2. Abell Clusters
ID:
ivo://nasa.heasarc/abell
Title:
Abell Clusters
Short Name:
Abell
Date:
26 Apr 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 .
3. Abell Clusters Measured Redshifts Catalog
ID:
ivo://nasa.heasarc/abellzcat
Title:
Abell Clusters Measured Redshifts Catalog
Short Name:
ABELLZCAT
Date:
26 Apr 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 .
4. ACT Massive and Distant Clusters of WISE Survey (MaDCoWS) Candidates Catalog
ID:
ivo://nasa.heasarc/actmadcows
Title:
ACT Massive and Distant Clusters of WISE Survey (MaDCoWS) Candidates Catalog
Short Name:
ACTMADCOWS
Date:
26 Apr 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 .
5. AEGIS-X Chandra Extended Groth Strip X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/aegisx
Title:
AEGIS-X Chandra Extended Groth Strip X-Ray Point Source Catalog
Short Name:
AEGISX
Date:
26 Apr 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 .
6. AEGIS-X Deep Survey Chandra X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/aegisxdcxo
Title:
AEGIS-X Deep Survey Chandra X-Ray Point Source Catalog
Short Name:
AEGISXDCXO
Date:
26 Apr 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 .
7. AKARI/FIS All-Sky Survey Bright Source Catalog, Version 1
ID:
ivo://nasa.heasarc/akaribsc
Title:
AKARI/FIS All-Sky Survey Bright Source Catalog, Version 1
Short Name:
AKARIBSC
Date:
26 Apr 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 .
8. AKARI/IRC All-Sky Survey Point Source Catalog, Version 1
ID:
ivo://nasa.heasarc/akaripsc
Title:
AKARI/IRC All-Sky Survey Point Source Catalog, Version 1
Short Name:
AKARIPSC
Date:
26 Apr 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 .
9. AKARI NEP WSRT 20-cm Source Catalog
ID:
ivo://nasa.heasarc/wsrt20anep
Title:
AKARI NEP WSRT 20-cm Source Catalog
Short Name:
WSRT20ANEP
Date:
26 Apr 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 .
10. Akari North Ecliptic Pole Deep Field Chandra X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/aknepdfcxo
Title:
Akari North Ecliptic Pole Deep Field Chandra X-Ray Point Source Catalog
Short Name:
AKNEPDFCXO
Date:
26 Apr 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 .