EDP Sciences
Free access
Volume 470, Number 1, July IV 2007
Page(s) 73 - 81
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20066248

A&A 470, 73-81 (2007)
DOI: 10.1051/0004-6361:20066248

An X-ray look at the Seyfert 1 Galaxy Mrk 590: XMM-Newton and Chandra reveal complexity in circumnuclear gas

A. L. Longinotti1, S. Bianchi1, M. Santos-Lleo1, P. Rodrìguez-Pascual1, M. Guainazzi1, M. Cardaci1, 2, and A. M. T. Pollock1

1  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: alonginotti@sciops.esa.int

(Received 14 August 2006 / 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 Ly$\alpha$ detected at ~19 $\AA$ 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 $L_{0.3{-}10~{\rm keV}}\sim 4\times10^{40}$ erg/s.

Key words: galaxies: active -- galaxies: individual: Mrk 590 -- line: profiles

© ESO 2007

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