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The Chandra COSMOS Legacy survey: overview and point source catalog

The COSMOS-Legacy survey is a 4.6 Ms Chandra program that has imaged 2.2 deg\(^2\) of the COSMOS field with an effective exposure of \(\simeq\)160 ks over the central 1.5 deg\(^2\) and of \(\simeq\)80 ks in the remaining area. The survey is the combination of 56 new observations, obtained as an X-ra...

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Published in:arXiv.org 2016-01
Main Authors: Civano, F, Marchesi, S, Comastri, A, Urry, M C, Elvis, M, Cappelluti, N, Puccetti, S, Brusa, M, Zamorani, G, Hasinger, G, Aldcroft, T, Alexander, D M, Allevato, V, Brunner, H, Capak, P, Finoguenov, A, Fiore, F, Fruscione, A, Gilli, R, Glotfelty, K, Griffiths, R E, Hao, H, Harrison, F A, Jahnke, K, Kartaltepe, J, Karim, A, LaMassa, S M, Lanzuisi, G, Miyaji, T, Ranalli, P, Salvato, M, Sargent, M, Scoville, N J, Schawinski, K, Schinnerer, E, Silverman, J, Smolcic, V, Stern, D, Toft, S, Trakhenbrot, B, Treister, E, Vignali, C
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Language:English
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Summary:The COSMOS-Legacy survey is a 4.6 Ms Chandra program that has imaged 2.2 deg\(^2\) of the COSMOS field with an effective exposure of \(\simeq\)160 ks over the central 1.5 deg\(^2\) and of \(\simeq\)80 ks in the remaining area. The survey is the combination of 56 new observations, obtained as an X-ray Visionary Project, with the previous C-COSMOS survey. We describe the reduction and analysis of the new observations and the properties of 2273 point sources detected above a spurious probability of 2\(\times 10^{-5}\). We also present the updated properties of the C-COSMOS sources detected in the new data. The whole survey includes 4016 point sources (3814, 2920 and 2440 in the full, soft and hard band). The limiting depths are 2.2 \(\times\) 10\(^{-16}\), 1.5 \(\times\) 10\(^{-15}\) and 8.9\(\times\) 10\(^{-16}\) \({\rm erg~cm}^{-2}~{\rm s}^{-1}\) in the 0.5-2, 2-10 and 0.5-10 keV bands, respectively. The observed fraction of obscured AGN with column density \(> 10^{22}\) cm\(^{-2}\) from the hardness ratio (HR) is \(\sim\)50\(^{+17}_{-16}\)%. Given the large sample, we compute source number counts in the hard and soft bands, significantly reducing the uncertainties of 5-10%. For the first time, we compute number counts for obscured (HR\(>\)-0.2) and unobscured (HR\(
ISSN:2331-8422
DOI:10.48550/arxiv.1601.00941