Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey

被引：353

作者：

Lusso, E. ^{[1
,2
]}

Comastri, A. ^{[2
]}

Simmons, B. D. ^{[3
,4
]}

Mignoli, M. ^{[2
]}

Zamorani, G. ^{[2
]}

Vignali, C. ^{[2
,5
]}

Brusa, M. ^{[6
]}

Shankar, F. ^{[7
]}

Lutz, D. ^{[6
]}

Trump, J. R. ^{[8
]}

Maiolino, R. ^{[9
,10
]}

Gilli, R. ^{[2
]}

Bolzonella, M. ^{[2
]}

Puccetti, S. ^{[11
]}

Salvato, M. ^{[6
,12
]}

Impey, C. D. ^{[13
]}

Civano, F. ^{[14
]}

Elvis, M. ^{[14
]}

Mainieri, V. ^{[15
]}

Silverman, J. D. ^{[16
]}

Koekemoer, A. M. ^{[17
]}

Bongiorno, A. ^{[9
]}

Merloni, A. ^{[6
,12
]}

Berta, S. ^{[6
]}

Le Floc'h, E. ^{[18
]}

Magnelli, B. ^{[6
]}

Pozzi, F. ^{[5
]}

Riguccini, L. ^{[18
]}

机构：

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

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

[3] Yale Univ, Dept Astron, New Haven, CT 06511 USA

[4] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06511 USA

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

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

[7] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92195 Meudon, France

[8] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA

[9] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy

[10] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England

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

[12] Max Planck Inst Plasma Phys & Excellence Cluster, D-85748 Garching, Germany

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

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

[15] ESO, D-85748 Garching, Germany

[16] Univ Tokyo, IPMU, Chiba 2778568, Japan

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

[18] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 425卷 / 01期

基金：

美国国家科学基金会;

关键词：

methods: statistical; galaxies: active; galaxies: evolution; quasars: general; SUPERMASSIVE BLACK-HOLES; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; STELLAR POPULATION SYNTHESIS; STAR-FORMING GALAXIES; HOST GALAXIES; ACCRETION RATE; HELLAS2XMM SURVEY; MASS FUNCTION;

D O I：

10.1111/j.1365-2966.2012.21513.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) active galactic nuclei (AGN) from the XMMNewton survey in the Cosmic Evolution Survey field are presented. The sample is composed of 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65?per cent of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83 and 52?per cent, respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high-quality multiwavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 and 160 mu m) to the opticalultraviolet allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol - Lbol relations derived in this work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. and Hopkins et al. Black hole (BH) masses and Eddington ratios are available for 170 Type-1 AGN, while BH masses for Type-2 AGN are computed for 481 objects using the BH massstellar mass relation and the morphological information. We confirm a trend between kbol and ?Edd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, the Eddington ratio increases with redshift for all types of AGN at any given MBH, while no clear evolution with redshift is seen at any given Lbol.

引用

页码：623 / 640

页数：18

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