EDP Sciences
Free access
Volume 435, Number 3, June I 2005
Page(s) 857 - 861
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20042581

A&A 435, 857-861 (2005)
DOI: 10.1051/0004-6361:20042581

A changing inner radius in the accretion disc of Q0056-363?

G. Matt1, D. Porquet2, S. Bianchi1, 3, S. Falocco1, R. Maiolino4, J. N. Reeves5 and L. Zappacosta6

1  Dipartimento di Fisica, Università degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
    e-mail: matt@fis.uniroma3.it
2  Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
3  XMM-Newton Science Operation Center, ESAC/ESA, Apartado 50727, 28080 Madrid, Spain
4  INAF - Osservatorio Astrofisico di Arcetri, Largo Fermi 5, 50125 Firenze, Italy
5  Laboratory for High Energy Astrophysics, NASA/GSFC, Greenbelt Road, Greenbelt, MD 20771, USA
6  Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA

(Received 13 December 2004 / Accepted 15 February 2005 )

Q0056-363 is the most powerful X-ray quasar known to exhibit a broad, likely relativistic iron line (Porquet & Reeves 2003, A&A, 408, 119). It has been observed twice by XMM-Newton, three and half years apart (July 2000 and December 2003). In the second observation, the UV and soft X-ray fluxes were fainter, the hard X-ray power law flatter, and the iron line equivalent width (EW) smaller than in the 2000 observation. These variations can all be explained, at least qualitatively, if the disc is truncated in the second observation. We report also on the possible detection of a transient, redshifted iron absorption line during the 2003 observation.

Key words: accretion, accretion disks -- galaxies: active -- X-rays: galaxies -- galaxies: quasars: individual: Q0056-363

SIMBAD Objects

© ESO 2005