The Chandra COSMOS Survey, I: Overview and Point Source Catalog
The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra} program that has imaged the central 0.5 sq.deg of the COSMOS field (centered at 10h, +02deg) with an effective exposure of ~160ksec, and an outer 0.4sq.deg. area with an effective exposure of ~80ksec. The limiting source detection dep...
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| creator | Martin, Elvis Civano, Francesca Vignali, Cristian Puccetti, Simonetta Fiore, Fabrizio Cappelluti, Nico Aldcroft, T L Fruscione, Antonella Zamorani, G Comastri, Andrea Brusa, Marcella Gilli, Roberto Miyaji, Takamitsu Damiani, Francesco Koekemoer, Anton Finoguenov, Alexis Brunner, Hermann Urry, C M Silverman, John Mainieri, Vincenzo Guenther Hasinger Griffiths, Richard Carollo, Marcella Heng Hao Guzzo, Luigi Blain, Andrew Calzetti, Daniela Carilli, C Capak, Peter Ettori, Stefano Fabbiano, Giuseppina Impey, Chris Lilly, Simon Mobasher, Bahram Rich, Michael Salvato, Mara Sanders, D B Schinnerer, Eva Scoville, N Shopbell, Patrick Taylor, James E Taniguchi, Yoshiaki Volonteri, Marta |
| description | The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra} program that has imaged the central 0.5 sq.deg of the COSMOS field (centered at 10h, +02deg) with an effective exposure of ~160ksec, and an outer 0.4sq.deg. area with an effective exposure of ~80ksec. The limiting source detection depths are 1.9e-16 erg cm(-2) s(-1) in the Soft (0.5-2 keV) band, 7.3e(-16) erg cm^-2 s^-1 in the Hard (2-10 keV) band, and 5.7e(-16) erg cm(-2) s(-1) in the Full (0.5-10 keV) 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 |
| doi_str_mv | 10.48550/arxiv.0903.2062 |
| format | Article |
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The limiting source detection depths are 1.9e-16 erg cm(-2) s(-1) in the Soft (0.5-2 keV) band, 7.3e(-16) erg cm^-2 s^-1 in the Hard (2-10 keV) band, and 5.7e(-16) erg cm(-2) s(-1) in the Full (0.5-10 keV) 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 <2e(-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 (to 12%) exposure across the inner 0.5 sq.deg field was obtained, leading to a sharply defined lower flux limit. The widely different PSFs 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. (Puccetti et al. Paper II). This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with sub-arcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper (Civano et al. Paper III). The full catalog is described here in detail, and is available on-line.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.0903.2062</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Cosmos ; Exposure ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Point sources ; Tiling</subject><ispartof>arXiv.org, 2009-04</ispartof><rights>2009. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with sub-arcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper (Civano et al. Paper III). 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The limiting source detection depths are 1.9e-16 erg cm(-2) s(-1) in the Soft (0.5-2 keV) band, 7.3e(-16) erg cm^-2 s^-1 in the Hard (2-10 keV) band, and 5.7e(-16) erg cm(-2) s(-1) in the Full (0.5-10 keV) 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 <2e(-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 (to 12%) exposure across the inner 0.5 sq.deg field was obtained, leading to a sharply defined lower flux limit. The widely different PSFs 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. (Puccetti et al. Paper II). This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with sub-arcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper (Civano et al. Paper III). The full catalog is described here in detail, and is available on-line.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.0903.2062</doi><oa>free_for_read</oa></addata></record> |
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| ispartof | arXiv.org, 2009-04 |
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| language | eng |
| recordid | cdi_arxiv_primary_0903_2062 |
| source | arXiv.org; Free E- Journals |
| subjects | Cosmos Exposure Physics - Cosmology and Nongalactic Astrophysics Physics - High Energy Astrophysical Phenomena Point sources Tiling |
| title | The Chandra COSMOS Survey, I: Overview and Point Source Catalog |
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