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28 March 2024
 
  » arxiv » 0912.4166

 Article overview


The X-ray to optical-UV luminosity ratio of X-ray selected Type 1 AGN in XMM-COSMOS
E. Lusso ; A. Comastri ; C. Vignali ; G. Zamorani ; M. Brusa ; R. Gilli ; K. Iwasawa ; M. Salvato ; F. Civano ; M. Elvis ; A. Merloni ; A. Bongiorno ; J.R. Trump ; A.M. Koekemoer ; E. Schinnerer ; E. Le Floc'h ; N. Cappelluti ; K. Jahnke ; M. Sargent ; J. Silverman ; V. Mainieri ; F. Fiore ; M. Bolzonella ; O. Le Fèvre ; B. Garilli ; A. Iovino ; J.P. Kneib ; F. Lamareille ; S. Lilly ; M. Mignoli ; M. Scodeggio ; D. Vergani ;
Date 21 Dec 2009
AbstractWe present a study of the X-ray to optical properties of a sample of 545 X-ray selected Type 1 AGN, from the XMM-COSMOS survey, over a wide range of redshifts ($0.04<z<4.25$) and X-ray luminosities ($40.6 leq Log Lhard leq 45.3$). About 60% of them are spectroscopically identified Type 1 AGN, while the others have a reliable photometric redshift and are classified as Type 1 AGN on the basis of their multi-band Spectral Energy Distributions. We discuss the relationship between UV and X-ray luminosity, as parameterized by the $alphaox$ spectral slope, and its dependence on redshift and luminosity. We compare our findings with previous investigations of optically selected broad-line AGN (mostly from SDSS). A highly significant correlation between $alphaox$ and $lo$ is found, in agreement with previous investigations of optically selected samples. We calculate bolometric corrections, $kbol$, for the whole sample using hard X-ray luminosities ($Lhard$), and the Eddington ratios for a subsample of 150 objects for which black hole mass estimates are available. We confirm the trend of increasing bolometric correction with increasing Eddington ratio as proposed in previous works. A tight correlation is found between $alphaox$ and $kbol$, which can be used to estimate accurate bolometric corrections using only optical and X-ray data. We find a significant correlation between $alphaox$ and Eddington ratio, in which $alphaox$ increases for increasing Eddington ratios.
Source arXiv, 0912.4166
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