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<ri:Resource created="2017-09-22T07:30:12Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>A catalog of nearby galaxies with Chandra obs.</title><shortName>J/ApJ/835/223</shortName><identifier>ivo://CDS.VizieR/J/ApJ/835/223</identifier><altIdentifier>doi:10.26093/cds/vizier.18350223</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>She R.</name></creator><creator><name>Ho L.C.</name></creator><creator><name>Feng H.</name></creator><date role="Updated">2017-10-31T12:00:15Z</date><date role="Created">2017-09-22T07:30:12Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>active-galactic-nuclei</subject><subject>x-ray-sources</subject><subject>galaxy-kinematics</subject><description>We searched the public archive of the Chandra X-ray Observatory as of 2016 March and assembled a sample of 719 galaxies within 50Mpc with available Advanced CCD Imaging Spectrometer observations. By cross-correlation with the optical or near-infrared nuclei of these galaxies, 314 of them are identified to have an X-ray active galactic nucleus (AGN). The majority of them are low-luminosity AGNs and are unlikely X-ray binaries based upon their spatial distribution and luminosity functions. The AGN fraction is around 60% for elliptical galaxies and early-type spirals, but drops to roughly 20% for Sc and later types, consistent with previous findings in the optical. However, the X-ray survey is more powerful in finding weak AGNs, especially from regions with active star formation that may mask the optical AGN signature. For example, 31% of the H II nuclei are found to harbor an X-ray AGN. For most objects, a single power-law model subject to interstellar absorption is adequate to fit the spectrum, and the typical photon index is found to be around 1.8. For galaxies with a non-detection, their stacked Chandra image shows an X-ray excess with a luminosity of a few times 10^37^erg/s on average around the nuclear region, possibly composed of faint X-ray binaries. This paper reports on the technique and results of the survey; in-depth analysis and discussion of the results will be reported in forthcoming papers.</description><source format="bibcode">2017ApJ...835..223S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/835/223</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/chandra">B/chandra : The Chandra Archive Log (CXC, 1999-2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/141">VII/141 : Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VIII/76">VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/233">VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/259">VII/259 : 6dF galaxy survey final redshift release (Jones+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/258">VII/258 : Quasars and Active Galactic Nuclei (13th Ed.) 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Hardness ratio H1: (medium-soft)/full (1)</description><ucd>phot.flux;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>H2</name><description>[-0.6/1]? Hardness ratio H2: (hard-medium)/full (1)</description><ucd>phot.flux;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_H2</name><description>? Error of H2</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>NH</name><description>[0.3/9.1]? Intrinsic absorption inferred from hardness ratio</description><unit>1e+22cm**-2</unit><ucd>phys.columnDensity</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>b_NH</name><description>[0.01/8]? Lower limit in NH</description><unit>1e+22cm**-2</unit><ucd>phys.columnDensity;stat.min</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>B_NH</name><description>[0.01/27]? Upper limit in NH</description><unit>1e+22cm**-2</unit><ucd>phys.columnDensity;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Flux</name><description>[0.08/17100]? Observed flux in 2-10keV</description><unit>1e-17W.m**-2</unit><ucd>phot.flux;em.X-ray</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>b_Flux</name><description>[0/16800]? Lower limit in Flux</description><unit>1e-17W.m**-2</unit><ucd>phot.flux;stat.min</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>B_Flux</name><description>[0.01/17400]? Upper limit in Flux</description><unit>1e-17W.m**-2</unit><ucd>phot.flux;stat.max</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>logLX</name><description>[35/44]? Log of 2-10keV luminosity; in erg/s</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.X-ray</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>b_logLX</name><description>[35/43]? Lower limit in LogLX</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.X-ray;stat.min</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>B_logLX</name><description>[30/43]? Upper limit in LogLX</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.X-ray;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>n_logLX</name><description>Note on luminosity or references for sources suffering from pileup (G1)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="5*">char</dataType></column></table></schema></tableset></ri:Resource>