Volume 595, November 2016
|Number of page(s)||9|
|Published online||08 November 2016|
Multiwavelength campaign on Mrk 509
XV. Global modeling of the broad emission lines in the optical, UV, and X-ray bands
1 SRON, Netherlands Institute for Space Research, Sorbonnelaan, 2, 3584 CA Utrecht, The Netherlands
2 Anton Pannekoek Institute, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands
3 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
4 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
5 Dipartimento di Matematica e Fisica, Universitá degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
6 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK
7 INAF-IASF Bologna, via Gobetti 101, 40129 Bologna, Italy
8 Max-Planck Institüt für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching bei München, Germany
9 XMM-Newton Science Operations Centre, ESAC, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
10 Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France
11 CNRS, IPAG, 38000 Grenoble, France
12 ISDC Data Centre for Astrophysics, Astronomical Observatory of the University of Geneva, 16 Ch. d’Écogia, 1290 Versoix, Switzerland
13 Instituto de Astronomía, Universidad Católica del Norte, 0610 Avenida Angamos, Antofagasta, Chile
14 Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA
Received: 14 December 2015
Accepted: 17 June 2016
Aims. We model the broad emission lines present in the optical, UV, and X-ray spectra of Mrk 509, a bright type 1 Seyfert galaxy. The broad lines were simultaneously observed during a large multiwavelength campaign, using the XMM-Newton-OM for the optical lines, HST-COS for the UV lines, and XMM-Newton-RGS and Epic for the X-ray lines. We also used FUSE archival data for the broad lines observed in the far-ultraviolet. The goal is to find a physical connection among the lines measured at different wavelengths and to determine the size and the distance from the central source of the emitting gas components.
Methods. We used the Locally Optimally emission Cloud (LOC) model which interprets the emissivity of the broad line region (BLR) as regulated by power law distributions of both gas density and distances from the central source.
Results. We find that one LOC component cannot model all the lines simultaneously. In particular, we find that the X-ray and UV lines may likely originate in the more internal part of the AGN at radii in the range ~5 × 1014−3 × 1017 cm, while the optical lines and part of the UV lines may likely originate farther out at radii ~3 × 1017−3 × 1018 cm. These two gas components are parametrized by a radial distribution of the luminosities with a slope γ of ~1.15 and ~1.10, respectively, both of them covering at least 60% of the source. This simple parametrization points to a structured broad line region where the higher ionized emission comes from closer in, while the emission of the low-ionization lines is more concentrated in the outskirts of the broad line region.
Key words: galaxies: individual: Mrk 509 / galaxies: Seyfert / quasars: emission lines / X-rays: galaxies
© ESO, 2016
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