Ultraluminous X-ray sources out to z ∼ 0.3 in the COSMOS field

被引：15

作者：

Mainieri, V. ^{[1
]}

Vignali, C. ^{[2
,3
]}

Merloni, A. ^{[4
,5
]}

Civano, F. ^{[6
]}

Puccetti, S. ^{[7
]}

Brusa, M. ^{[5
]}

Gilli, R. ^{[3
]}

Bolzonella, M. ^{[3
]}

Comastri, A. ^{[3
]}

Zamorani, G. ^{[3
]}

Aller, M. ^{[9
]}

Carollo, M. ^{[9
]}

Scarlata, C. ^{[9
,10
]}

Elvis, M. ^{[6
]}

Aldcroft, T. L. ^{[6
]}

Cappelluti, N. ^{[5
]}

Fabbiano, G. ^{[6
]}

Finoguenov, A. ^{[5
]}

Fiore, F. ^{[8
]}

Fruscione, A. ^{[6
]}

Koekemoer, A. M. ^{[11
]}

Contini, T. ^{[12
]}

Kneib, J. -P. ^{[13
]}

Le Fevre, O. ^{[13
]}

Lilly, S. ^{[9
]}

Renzini, A. ^{[14
]}

Scodeggio, M. ^{[15
]}

Bardelli, S. ^{[3
]}

Bongiorno, A. ^{[5
]}

Caputi, K. ^{[9
]}

Coppa, G. ^{[3
]}

Cucciati, O. ^{[16
]}

de la Torre, S. ^{[13
]}

de Ravel, L. ^{[13
]}

Franzetti, P. ^{[15
]}

Garilli, B. ^{[15
]}

Iovino, A. ^{[16
]}

Kampczyk, P. ^{[9
]}

Knobel, C. ^{[9
]}

Kovac, K. ^{[9
]}

Lamareille, F. ^{[12
]}

Le Borgne, J. -F. ^{[12
]}

Le Brun, V. ^{[13
]}

Maier, C. ^{[9
]}

Mignoli, M. ^{[3
]}

Pello, R. ^{[12
]}

Peng, Y. ^{[9
]}

Montero, E. Perez ^{[12
]}

Ricciardelli, E. ^{[17
]}

Silverman, J. D. ^{[9
]}

机构：

[1] ESO, D-85748 Garching, Germany

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

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

[4] TUM, D-85748 Garching, Germany

[5] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany

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

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

[8] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[9] ETH Honggerberg, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland

[10] Spitzer Sci Ctr, Pasadena, CA 91125 USA

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

[12] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France

[13] Lab Astrophys Marseille, Marseille, France

[14] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[15] INAF IASF Milano, Milan, Italy

[16] INAF Osservatorio Astron Brera, Milan, Italy

[17] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy

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

[19] CALTECH, Pasadena, CA 91125 USA

[20] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 514卷

关键词：

X-rays: galaxies; X-rays: binaries; X-rays: general; surveys; STAR-FORMATION; BLACK-HOLES; LUMINOSITY FUNCTION; BINARIES; CLASSIFICATION; POPULATION; REDSHIFT; GALAXIES; EVOLUTION; INDICATOR;

D O I：

10.1051/0004-6361/200912544

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Using Chandra observations we identified a sample of seven off-nuclear X-ray sources in the redshift range z = 0.072-0.283, located within optically bright galaxies in the COSMOS Survey. All of them, if associated with their closest bright galaxy, would have L[0.5-7 keV] > 10(39) erg s(-1) and therefore can be classified as ultraluminous X-ray sources (ULXs). Aims. Using the multi-wavelength coverage available in the COSMOS field, we studied the properties of the host galaxies of these ULXs. In detail, we derived their star formation rate from Ha measurements and their stellar masses using SED fitting techniques with the aim to compute the probability to have an off-nuclear source based on the host galaxy properties. We divided the host galaxies in different morphological classes with the available ACS/HST imaging. Methods. We selected off-nuclear candidates with the following criteria: 1) the distance between the X-ray and the optical centroid has to be larger than 0.9 '', larger than 1.8 times the radius of the Chandra positional error circle and smaller than the Petrosian radius of the host galaxy; 2) the optical counterpart is a bright galaxy (R-AB < 22); 3) the redshift of the counterpart is lower than z = 0.3; 4) the source has been observed in at least one Chandra pointing at an off-axis angle smaller than 5'; 5) the X-ray positional error is smaller than 0.8 ''. We verified each candidate super-imposing the X-ray contours on the optical/IR images. We expect less than one misidentified AGN due to astrometric errors and on average 1.3 serendipitous background source matches. Results. We find that our ULXs candidates are located in regions of the SFR versusM(*) plane where one or more off-nuclear detectable sources are expected. From a morphological analysis of the ACS imaging and the use of rest-frame colours, we find that our ULXs are hosted both in late and early type galaxies. Finally, we find that the fraction of galaxies hosting a ULX ranges from approximate to 0.5% to approximate to 0.2% going from L0.5-2 (keV) = 3 x 10(39) erg s(-1) to L0.5-2 keV = 2 x 10(40) erg s(-1).

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