An intense and broad Fe K_α line observed in the X-ray luminous quasar Q 0056-363 with XMM-Newton

¹ Max-Plank-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
² Laboratory for High Energy Astrophysics, Code 662.0, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
³ Universities Space Research Association

Corresponding author: D. Porquet, dporquet@mpe.mpg.de

Received: 12 March 2003
Accepted: 16 June 2003

Abstract

We present an XMM-Newton observation of the radio-quiet quasar Q0056-363 (). This is the first time that this quasar is observed in the hard X-ray range (above 2 keV). We find that Q0056-363 is a powerful X-ray quasar, with a 0.3–12 keV unabsorbed luminosity of about erg s^-1 with the largest part (~67%) emitted below 2 keV. The spectrum reveals a large featureless soft X-ray excess below 2 keV and a strong broad Fe K_α line at 6.4 keV (in the quasar frame). The Fe K_α line is due to low to moderate ionization states of iron (i.e., <), with an equivalent width of about 250 eV and a velocity width of about 25 000 km s^-1. Q0056-363 is presently the most luminous AGN known to exhibit such a broad and intense Fe K_α line profile from near neutral iron. The line can be fitted with a relativistic profile from an accretion disc around either a Schwarzschild (non-rotating) or a Kerr (rotating) black hole. A combination of two thermal Comptonization components and a disc reflection model is favored to explain both the continuum over the energy range 0.3–12 keV and the Fe K_α line. A patchy corona covering a large part of the inner disc surface is needed in order to be compatible with the accretion rate inferred from the spectral energy distribution of Q0056-363, unless the mass of the black hole is much higher than about .