THE CHANDRA COSMOS SURVEY. III. OPTICAL AND INFRARED IDENTIFICATION OF X-RAY POINT SOURCES

被引：211

作者：

Civano, F. ^{[1
]}

Elvis, M. ^{[1
]}

Brusa, M. ^{[2
]}

Comastri, A. ^{[3
]}

Salvato, M. ^{[2
,4
]}

Zamorani, G. ^{[3
]}

Aldcroft, T. ^{[1
]}

Bongiorno, A. ^{[2
,5
]}

Capak, P. ^{[6
]}

Cappelluti, N. ^{[3
]}

Cisternas, M. ^{[7
]}

Fiore, F. ^{[5
]}

Fruscione, A. ^{[1
]}

Hao, H. ^{[1
]}

Kartaltepe, J. ^{[8
]}

Koekemoer, A. ^{[9
,10
]}

Gilli, R. ^{[3
]}

Impey, C. D. ^{[11
]}

Lanzuisi, G. ^{[1
,5
]}

Lusso, E. ^{[3
]}

Mainieri, V. ^{[12
]}

Miyaji, T. ^{[13
]}

Lilly, S. ^{[14
]}

Masters, D. ^{[15
]}

Puccetti, S. ^{[16
]}

Schawinski, K. ^{[17
]}

Scoville, N. Z. ^{[6
]}

Silverman, J. ^{[18
]}

Trump, J. ^{[11
]}

Urry, M. ^{[17
]}

Vignali, C. ^{[3
,19
]}

Wright, N. J. ^{[1
]}

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[3] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy

[4] Excellence Cluster, D-85748 Garching, Germany

[5] INAF Osservatorio Astron Roma, I-00040 Rome, Italy

[6] CALTECH, Pasadena, CA 91125 USA

[7] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[8] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[9] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[10] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA

[11] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[12] ESO, D-85748 Garching, Germany

[13] Univ Nacl Autonoma Mexico Ensenada, Ensenada 22860, Baja California, Mexico

[14] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland

[15] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[16] ASI Sci Data Ctr, I-00044 Frascati, Italy

[17] Yale Univ, Dept Phys, New Haven, CT 06511 USA

[18] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan

[19] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2012年 / 201卷 / 02期

基金：

美国国家科学基金会;

关键词：

galaxies: active; surveys; X-rays: galaxies: clusters; ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; SUPERMASSIVE BLACK-HOLES; GALAXY LIGHT CONCENTRATION; HUBBLE-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; MEDIUM-SENSITIVITY SURVEY; EVOLUTION SURVEY COSMOS; MS SOURCE CATALOGS; DIGITAL SKY SURVEY;

D O I：

10.1088/0067-0049/201/2/30

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 x 10(-16) erg cm(-2) s(-1) in the soft (0.5-2 keV) band, 7.3 x 10(-16) erg cm(-2) s(-1) in the hard (2-10 keV) band, and 5.7 x 10(-16) erg cm(-2) s(-1) in the full (0.5-10 keV) band. In this paper we report the i, K, and 3.6 mu m 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 two sources are truly empty fields. The full catalog, including spectroscopic and photometric redshifts and classification described here in detail, is available online. Making use of the large number of X-ray sources, we update the "classic locus" of active galactic nuclei (AGNs) defined 20 years ago in soft X-ray surveys and define a new locus containing 90% of the AGNs in the survey with full-band luminosity >10(42) erg s(-1). We present the linear fit between the total i-band magnitude and the X-ray flux in the soft and hard bands, drawn over two 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 X/O computed in the hard band and C and that 90% of the obscured AGNs 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 black hole growth at X-ray luminosities of 10(43)-10(44.5) erg s(-1). We also investigate the degree of obscuration of the sample using the hardness ratio, and we compare the X-ray color with the near-infrared to optical color.

引用

页数：21

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