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<ri:Resource created="2010-04-01T08:56:07Z" 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>Chandra COSMOS survey I.</title><shortName>J/ApJS/184/158</shortName><identifier>ivo://CDS.VizieR/J/ApJS/184/158</identifier><altIdentifier>doi:10.26093/cds/vizier.21840158</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Elvis M.</name></creator><creator><name>Civano F.</name></creator><creator><name>Vignali C.</name></creator><creator><name>Puccetti S.</name></creator><creator><name>Fiore F.</name></creator><creator><name>Cappelluti N.,Aldcroft T.L.</name></creator><creator><name>Fruscione A.</name></creator><creator><name>Zamorani G.</name></creator><creator><name>Comastri A.</name></creator><creator><name>Brusa M.</name></creator><creator><name>Gilli R.,Miyaji T.</name></creator><creator><name>Damiani F.</name></creator><creator><name>Koekemoer A.M.</name></creator><creator><name>Finoguenov A.</name></creator><creator><name>Brunner H.,Urry C.M.</name></creator><creator><name>Silverman J.</name></creator><creator><name>Mainieri V.</name></creator><creator><name>Hasinger G.</name></creator><creator><name>Griffiths R.,Carollo M.</name></creator><creator><name>Hao H.</name></creator><creator><name>Guzzo L.</name></creator><creator><name>Blain A.</name></creator><creator><name>Calzetti D.</name></creator><creator><name>Carilli C.</name></creator><creator><name>Capak P.,Ettori S.</name></creator><creator><name>Fabbiano G.</name></creator><creator><name>Impey C.</name></creator><creator><name>Lilly S.</name></creator><creator><name>Mobasher B.</name></creator><creator><name>Rich M.,Salvato M.</name></creator><creator><name>Sanders D.B.</name></creator><creator><name>Schinnerer E.</name></creator><creator><name>Scoville N.</name></creator><creator><name>Shopbell P.,Taylor J.E.</name></creator><creator><name>Taniguchi Y.</name></creator><creator><name>Volonteri M.</name></creator><date role="Updated">2014-05-07T12:31:43Z</date><date role="Created">2010-04-01T08:56:07Z</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>x-ray-sources</subject><subject>surveys</subject><description>The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8Ms, Chandra program that has imaged the central 0.5deg^2^ of the COSMOS field (centered at 10h, +02d) with an effective exposure of ~160ks, and an outer 0.4deg^2^ area with an effective exposure of ~80ks. The limiting source detection depths are 1.9x10^-16^erg/cm2/s in the soft (0.5-2keV) band, 7.3x10^-16^erg/cm2/s in the hard (2-10keV) band, and 5.7x10^-16^erg/cm2/s in the full (0.5-10keV) band. Here we describe the strategy, design, and execution of the C-COSMOS survey, and present the catalog of 1761 point sources detected at a probability of being spurious of &lt;2x10^-5^ (1655 in the full, 1340 in the soft, and 1017 in the hard bands). By using a grid of 36 heavily (~50%) overlapping pointing positions with the ACIS-I imager, a remarkably uniform (+/-12%) exposure across the inner 0.5deg^2^ field was obtained, leading to a sharply defined lower flux limit. The widely different point-spread functions obtained in each exposure at each point in the field required a novel source detection method, because of the overlapping tiling strategy, which is described in a companion paper. This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with subarcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper.</description><source format="bibcode">2009ApJS..184..158E</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/184/158</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/II/284">II/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/172/29">J/ApJS/172/29 : XMM-Newton survey in COSMOS field. I. 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