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arXiv · 1205.5030

The Chandra COSMOS Survey: III. Optical and Infrared Identification of X-ray Point Sources

F. Civano·M. Elvis·M. Brusa·A. Comastri·M. Salvato·G. Zamorani·T. Aldcroft·A. Bongiorno·P. Capak·N. Cappelluti·M. Cisternas·F. Fiore·A. Fruscione·H. Hao·J. Kartaltepe·A. Koekemoer·R. Gilli·C. D. Impey·G. Lanzuisi·E. Lusso·V. Mainieri·T. Miyaji·S. Lilly·D. Masters·S. Puccetti·K. Schawinski·N. Z. Scoville·J. Silverman·J. Trump·M. Urry·C. Vignali·N. J. Wright
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Abstract

The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.9 deg^2 of the COSMOS field down to limiting depths of 1.9 10^-16 erg cm^-2 s-1 in the 0.5-2 keV band, 7.3 10^-16 erg cm^-2 s^-1 in the 2-10 keV band, and 5.7 10^-16 erg cm^-2 s-1 in the 0.5-10 keV band. In this paper we report the i, K and 3.6micron identifications of the 1761 X-ray point sources. We use the likelihood ratio technique to derive the association of optical/infrared counterparts for 97% of the X-ray sources. For most of the remaining 3%, the presence of multiple counterparts or the faintness of the possible counterpart prevented a unique association. For only 10 X-ray sources we were not able to associate a counterpart, mostly due to the presence of a very bright field source close by. Only 2 sources are truly empty fields. Making use of the large number of X-ray sources, we update the "classic locus" of AGN and define a new locus containing 90% of the AGN in the survey with full band luminosity >10^42 erg/s. We present the linear fit between the total i band magnitude and the X-ray flux in the soft and hard band, drawn over 2 orders of magnitude in X-ray flux, obtained using the combined C-COSMOS and XMM-COSMOS samples. We focus on the X-ray to optical flux ratio (X/O) and we test its known correlation with redshift and luminosity, and a recently introduced anti-correlation with the concentration index (C). We find a strong anti-correlation (though the dispersion is of the order of 0.5 dex) between C and X/O, computed in the hard band, and that 90% of the obscured AGN in the sample with morphological information live in galaxies with regular morphology (bulgy and disky/spiral), suggesting that secular processes govern a significant fraction of the BH growth at X-ray luminosities of 10^43- 10^44.5 erg/s.

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F. Civano, M. Elvis, M. Brusa, A. Comastri, M. Salvato, G. Zamorani, T. Aldcroft, A. Bongiorno, P. Capak, N. Cappelluti, M. Cisternas, F. Fiore, A. Fruscione, H. Hao, J. Kartaltepe, A. Koekemoer, R. Gilli, C. D. Impey, G. Lanzuisi, E. Lusso, V. Mainieri, T. Miyaji, S. Lilly, D. Masters, S. Puccetti, K. Schawinski, N. Z. Scoville, J. Silverman, J. Trump, M. Urry, C. Vignali, N. J. Wright. 2012-05-22. The Chandra COSMOS Survey: III. Optical and Infrared Identification of X-ray Point Sources. https://doi.org/10.1088/0067-0049%2F201%2F2%2F30

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