Multiwavelength campaign on Mrk 509

XIV. Chandra HETGS spectra

¹ SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
e-mail: J.S.Kaastra@sron.nl
² Department of Physics and Astronomy, Universiteit Utrecht, PO Box 80000, 3508 TA Utrecht, The Netherlands
³ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
⁴ European Space Astronomy Centre (ESAC), PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
⁵ Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA
⁶ Department of Physics, Technion-Israel Institute of Technology, 32000 Haifa, Israel
⁷ Dipartimento di Matematica e Fisica, Università degli Studi Roma Tre, Via della Vasca Navale 84, 00146 Roma, Italy
⁸ Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK
⁹ INAF-IASF Bologna, Via Gobetti 101, 40129 Bologna, Italy
¹⁰ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
¹¹ Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
¹² Max Planck Institut für Extraterrestrische Physik , 85741 Garching, Germany
¹³ University of Geneva, 16, ch. d’Ecogia, 1290 Versoix, Switzerland
¹⁴ Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France
¹⁵ CNRS, IPAG, 38000 Grenoble, France
¹⁶ Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
¹⁷ Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Casilla 1280 Antofagasta, Chile
¹⁸ Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK

Received: 23 July 2014
Accepted: 29 August 2014

Abstract

Context. We present in this paper the results of a 270 ks Chandra HETGS observation in the context of a large multiwavelength campaign on the Seyfert galaxy Mrk 509.

Aims. The HETGS spectrum allows us to study the high ionisation warm absorber and the Fe-K complex in Mrk 509. We search for variability in the spectral properties of the source with respect to previous observations in this campaign, as well as for evidence of ultra-fast outflow signatures.

Methods. The Chandra HETGS X-ray spectrum of Mrk 509 was analysed using the SPEX fitting package.

Results. We confirm the basic structure of the warm absorber found in the 600 ks XMM-Newton RGS observation observed three years earlier, consisting of five distinct ionisation components in a multikinematic regime. We find little or no variability in the physical properties of the different warm absorber phases with respect to previous observations in this campaign, except for component D2 which has a higher column density at the expense of component C2 at the same outflow velocity (−240 km s^-1). Contrary to prior reports we find no −700 km s^-1 outflow component. The O viii absorption line profiles show an average covering factor of 0.81±0.08 for outflow velocities faster than −100 km s^-1, similar to those measured in the UV. This supports the idea of a patchy wind. The relative metal abundances in the outflow are close to proto-solar. The narrow component of the Fe Kα emission line shows no changes with respect to previous observations which confirms its origin in distant matter. The narrow line has a red wing that can be interpreted to be a weak relativistic emission line. We find no significant evidence of ultra-fast outflows in our new spectrum down to the sensitivity limit of our data.