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Accretion and outflow of gas in Markarian 509

Published online by Cambridge University Press:  21 February 2013

Jelle Kaastra ,
Pierre-Olivier Petrucci ,
Massimo Cappi ,
Nahum Arav ,
Ehud Behar ,
Stefano Bianchi ,
Graziella Branduardi-Raymont ,
Elisa Costantini ,
Jacobo Ebrero  and
Jerry Kriss
...Show all authors
Jelle Kaastra
Affiliation:
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands email: [email protected] Utrecht University, Utrecht, The Netherlands
Pierre-Olivier Petrucci
Affiliation:
UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG)UMR 5274, Grenoble 38041, France
Massimo Cappi
Affiliation:
INAF-IASF Bologna, via Gobetti 101, 40129 Bologna, Italy
Nahum Arav
Affiliation:
Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA
Ehud Behar
Affiliation:
Department of Physics, Technion-Israel Institute of Technology, 32000 Haifa, Israel
Stefano Bianchi
Affiliation:
Dipartimento di Fisica, Universitá degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
Graziella Branduardi-Raymont
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK
Elisa Costantini
Affiliation:
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands email: [email protected]
Jacobo Ebrero
Affiliation:
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands email: [email protected]
Jerry Kriss
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
Missagh Mehdipour
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK
Stephane Paltani
Affiliation:
ISDC Data Centre for Astrophysics, Astronomical Observatory of the University of Geneva, 16, ch. d'Ecogia, 1290 Versoix, Switzerland
Ciro Pinto
Affiliation:
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands email: [email protected]
Gabriele Ponti
Affiliation:
Max-Planck Institut für Extraterrestrische Physik, Garching, Germany
Katrien Steenbrugge
Affiliation:
Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Casilla 1280, Antofagasta, Chile Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
Cor de Vries
Affiliation:
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands email: [email protected]
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Abstract

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A major uncertainty in models for photoionised outflows in AGN is the distance of the gas to the central black hole. We present the results of a massive multiwavelength monitoring campaign on the bright Seyfert 1 galaxy Mrk 509 to constrain the location of the outflow components dominating the soft X-ray band. Mrk 509 was monitored by XMM-Newton, Integral, Chandra, HST/COS and Swift in 2009. We have studied the response of the photoionised gas to the changes in the ionising flux produced by the central regions. We were able to put tight constraints on the variability of the absorbers from day to year time scales. This allowed us to develop a model for the time-dependent photoionisation in this source. We find that the more highly ionised gas producing most X-ray line opacity is at least 5 pc away from the core; upper limits to the distance of various absorbing components range between 20 pc up to a few kpc. The more lowly ionised gas producing most UV line opacity is at least 100 pc away from the nucleus. These results point to an origin of the dominant, slow (v<1000 km s−1) outflow components in the NLR or torus-region of Mrk 509. We find that while the kinetic luminosity of the outflow is small, the mass carried away is likely larger than the 0.5 Solar mass per year accreting onto the black hole. We also determined the chemical composition of the outflow as well as valuable constraints on the different emission regions. We find for instance that the resolved component of the Fe-K line originates from a region 40–1000 gravitational radii from the black hole, and that the soft excess is produced by Comptonisation in a warm (0.2–1 keV), optically thick (τ~ 10–20) corona near the inner part of the disk.

Keywords

Active Galactic NucleiX-raysoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 45 - 48
Copyright
Copyright © International Astronomical Union 2013

References

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