Volume 470, Number 1, July IV 2007
|Page(s)||73 - 81|
|Published online||02 May 2007|
An X-ray look at the Seyfert 1 Galaxy Mrk 590: XMM-Newton and Chandra reveal complexity in circumnuclear gas
European Space Astronomy Centre, Apartado 50727, 28080 Madrid, Spain
2 Departamento de Física Teórica, C-XI, Universidad Autónoma de Madrid, 28049 Madrid, Spain e-mail: email@example.com
Accepted: 8 January 2007
Context.This paper reports on a partially simultaneous observation of the bright Seyfert 1 Galaxy Mrk 590, performed by XMM-Newton and Chandra.
Aims.The long exposure (~100 ks) allows us to investigate the Fe K complex at 6-7 keV and the presence of soft X-ray spectral features in great detail.
Methods.We have analysed XMM-Newton data from the European Photon Imaging Camera (EPIC) in the 0.5-12 keV band and from the Reflection Grating Spectrometer (RGS) in the 0.35-2.5 keV band, and data from the High Energy Transmission Gratings (HETGs) onboard Chandra. UV and optical data from the Optical Monitor (OM) onboard XMM-Newton are also included in the analysis.
Results.The broad band spectrum is well described by an unabsorbed power law and three unresolved Fe K lines in the 6-7 keV range. The presence of a Compton reflection component and a narrow Fe K line at 6.4 keV is consistent with an origin via torus reflection. The ionised Fe lines at ~6.7 and 7 keV are instead most likely originated by scattering on a warm and ionised gas. The soft X-ray spectrum appears to be almost featureless due to the very bright continuum emission, except for one emission line identified as OVIII Lyα detected at ~19 by both RGS and Chandra-MEG. The emerging picture consists of an active nucleus seen directly on a “clean” line of sight without intervening material, surrounded by photoionised circumnuclear gas at a high ionisation level. We also study three serendipitous sources in the field of view of Chandra and XMM-Newton. One of these sources may be identified with an ULX of erg/s.
Key words: galaxies: active / galaxies: individual: Mrk 590 / line: profiles
© ESO, 2007
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