EDP Sciences
Free access
Issue
A&A
Volume 365, Number 1, January I 2001
First Results from XMM-Newton
Page(s) L134 - L139
DOI http://dx.doi.org/10.1051/0004-6361:20000424


A&A 365, L134-L139 (2001)
DOI: 10.1051/0004-6361:20000424

XMM-Newton observation of an unusual iron line in the quasar Markarian 205

J. N. Reeves1, M. J. L. Turner1, K. A. Pounds1, P. T. O'Brien1, Th. Boller2, P. Ferrando3, E. Kendziorra4 and S. Vercellone5.

1  X-Ray Astronomy Group, Department of Physics and Astronomy, Leicester University, Leicester LE1 7RH, UK
2  Max-Planck-Institut für extraterrestrische Physik, Postfach 1603, 85748 Garching, Germany
3  Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France
4  Institut für Astronomie und Astrophysik - Astronomie, University of Tübingen, Waldhäuser Strasse 64, 72076 Tübingen, Germany
5  Istituto di Fisica Cosmica "G. Occhialini", C.N.R., Via Bassini 15, 20133 Milano, Italy

(Received 28 September 2000 / Accepted 20 October 2000 )

Abstract
XMM-Newton observations of the low luminosity, radio-quiet quasar Markarian 205 have revealed a unique iron K emission line profile. In marked contrast to the broad and redshifted iron K line commonly seen in ASCA observations of Seyfert 1 galaxies, we find that a substantial amount of the line flux in Mrk 205 occurs above the neutral line energy of 6.4 keV. Furthermore, we find that the iron line emission has two distinct components, a narrow, unresolved neutral line at 6.4 keV and a broadened line centred at 6.7 keV. We suggest that the most likely origin of the 6.7 keV line is from X-ray reflection off the surface of a highly ionised accretion disk, whilst the 6.4 keV component may arise from neutral matter distant from the black hole, quite possibly in the putative molecular torus. Overall this observation underlines the potential of XMM-Newton for using the iron K line as a diagnostic of matter in the innermost regions of AGN.


Key words: galaxies: active -quasars: individual: Markarian 205 -X-rays: galaxies

Offprint request: J. N. Reeves

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