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  <title>Chandra COSMOS (C-COSMOS) Survey X-Ray Point Source Catalog</title>
  <shortName>CCOSMOSCAT</shortName>
  <identifier>ivo://nasa.heasarc/ccosmoscat</identifier>
  <curation>
    <publisher ivo-id="ivo://nasa.heasarc/ASD">NASA/GSFC HEASARC</publisher>
    <creator>
      <name>Elvis et al.</name>
    </creator>
    <contributor/>
    <date>2026-10-09</date>
    <contact>
      <name>NASA/GSFC HEASARC help desk</name>
      <email>heasarc-vo at athena.gsfc.nasa.gov</email>
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    <subject>Survey Source</subject>
    <description>
      The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.5 deg&amp;lt;sup&amp;gt;2&amp;lt;/sup&amp;gt; of the COSMOS field (centered at RA, Dec of 10 hours , +02 degrees) with an effective exposure of ~ 160 ks, and an outer 0.4 deg&amp;lt;sup&amp;gt;2&amp;lt;/sup&amp;gt; area with an effective exposure of ~ 80 ks. The limiting source detection depths are 1.9 x 10&amp;lt;sup&amp;gt;-16&amp;lt;/sup&amp;gt; erg cm&amp;lt;sup&amp;gt;-2&amp;lt;/sup&amp;gt; s&amp;lt;sup&amp;gt;-1&amp;lt;/sup&amp;gt; in the soft (0.5 - 2 keV) band, 7.3 x 10&amp;lt;sup&amp;gt;-16&amp;lt;/sup&amp;gt; erg cm&amp;lt;sup&amp;gt;-2&amp;lt;/sup&amp;gt; s&amp;lt;sup&amp;gt;-1&amp;lt;/sup&amp;gt; in the hard (2 - 10 keV) band, and 5.7 x 10&amp;lt;sup&amp;gt;-16&amp;lt;/sup&amp;gt; erg cm&amp;lt;sup&amp;gt;-2&amp;lt;/sup&amp;gt; s&amp;lt;sup&amp;gt;-1&amp;lt;/sup&amp;gt; in the full (0.5 - 10 keV) band. In this paper, the authors 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 &amp;lt; 2 x 10&amp;lt;sup&amp;gt;-5&amp;lt;/sup&amp;gt; (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 0.5 deg&amp;lt;sup&amp;gt;2&amp;lt;/sup&amp;gt; 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 log N-log S curve, with sub-arcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper. Supporting data products for this table (including images, event files, and exposure maps) are available at the &amp;lt;a href="https://cosmos.astro.caltech.edu/page/xray/"&amp;gt;COSMOS Survey website&amp;lt;/a&amp;gt; and at &amp;lt;a href="https://irsa.ipac.caltech.edu/data/COSMOS/"&amp;gt;IRSA&amp;lt;/a&amp;gt;. At the IRSA website, it is also possible to search a database that includes &amp;quot;postage stamps&amp;quot; of the X-ray data for each source, along with the multi-wavelength optical and infrared data, including the I-band, K-band, and Spitzer 3.6-micron (Band 1) images used in the Part III paper (Civano et al. 2012) to identify the sources. See also the related table &amp;lt;a href="ccosmosoid.html"&amp;gt;CCOSMOSOID&amp;lt;/a&amp;gt; for the optical and infrared identifications of the surveyed X-ray point sources. This table was created by the HEASARC in November 2009 based on an electronic version of the C-COSMOS Catalog which was obtained from the Astrophysical Journal web site. This is a service provided by NASA HEASARC .
    </description>
    <source format="">
      2009ApJS..184..158E
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          Chandra COSMOS (C-COSMOS) Survey X-Ray Point Source Catalog
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            Soft 0.5-2 keV Count Rate
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            Full 0.5-7 keV Aperture Photometry Net Counts
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