Fe K line profile in PG quasars: the averaged shape and Eddington ratio dependence

Details Fe K line profile in PG quasars: the averaged shape and Eddington ratio dependence Fe K line profile in PG quasars: the averaged shape and Eddington ratio dependence

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..385i&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Physics

Scientific paper

Fe-K emission is a powerful probe of the inner part of an accretion disk. We analyzed X-ray spectra of 43 Palomar-Green (PG) quasars taken from Boroson & Green (1992) observed with XMM-Newton and made an averaged Fe-K line profile. Their central black hole masses and Eddington ratios have been estimated from the optical spectra. The Eddington ratio, which is one of the most important parameters to characterize accretion disks, ranges from 0.05 to 4.50. This wide range enables us to study the Eddington ratio dependence of Fe line profiles. We fitted the spectra of the 43 quasars systematically by using a canonical model consisting of a power-law, a blackbody, and a Gaussian all modified by the Galactic absorption. The spectra of 39 objects are well reproduced by this model. The spectra of the remaining four objects require additional absorption with a column density of 1023 cm-2 to the power-law component. We studied the Eddington ratio dependence of the Fe-K line profile. We divided the sample into four groups and made averaged spectra for each group. The width of the Fe line becomes broader (sigma=0.1 to 1.0 keV) and its peak energy becomes higher (6.4 to 7.0 keV) as the Eddington ratio gets larger. This results indicates that a physical state of the accretion disk, such as the geometrical structure and/or ionization state, changes with the Eddington ratio.

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