Statistical Characterization of the Chandra Source Catalog

• Published in: arXiv.org
• Main Authors: Primini, Francis A, Houck, John C, Davis, John E, Nowak, Michael A, Evans, Ian N, Glotfelty, Kenny J, Anderson, Craig S, Bonaventura, Nina R, Chen, Judy C, Doe, Stephen M, Evans, Janet D, Fabbiano, Giuseppina, Galle, Elizabeth C, Gibbs, Danny G, Grier, John D, Hain, Roger M, Hall, Diane M, Harbo, Peter N, Xiangqun, He, Karovska, Margarita, Kashyap, Vinay L, Lauer, Jennifer, McCollough, Michael L, McDowell, Jonathan C, Miller, Joseph B, Mitschang, Arik W, Morgan, Douglas L, Mossman, Amy E, Nichols, Joy S, Plummer, David A, Refsdal, Brian L, Rots, Arnold H, Siemiginowska, Aneta, Sundheim, Beth A, Tibbetts, Michael S, Van Stone, David W, Winkelman, Sherry L, Zografou, Panagoula
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 05.05.2011
• Subjects: Physics - High Energy Astrophysical Phenomena; X ray sources
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1105.0691

The first release of the Chandra Source Catalog (CSC) contains ~95,000 X-ray sources in a total area of ~0.75% of the entire sky, using data from ~3,900 separate ACIS observations of a multitude of different types of X-ray sources. In order to maximize the scientific benefit of such a large, heterogeneous data-set, careful characterization of the statistical properties of the catalog, i.e., completeness, sensitivity, false source rate, and accuracy of source properties, is required. Characterization efforts of other, large Chandra catalogs, such as the ChaMP Point Source Catalog (Kim et al. 2007) or the 2 Mega-second Deep Field Surveys (Alexander et al. 2003), while informative, cannot serve this purpose, since the CSC analysis procedures are significantly different and the range of allowable data is much less restrictive. We describe here the characterization process for the CSC. This process includes both a comparison of real CSC results with those of other, deeper Chandra catalogs of the same targets and extensive simulations of blank-sky and point source populations.