Volume 534, October 2011
|Number of page(s)||26|
|Published online||29 September 2011|
Multiwavelength campaign on Mrk 509
Space Telescope Science Institute,
3700 San Martin Drive,
2 Department of Physics & Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
3 Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA
4 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
5 Astronomical Institute, University of Utrecht, Postbus 80000, 3508 TA Utrecht, The Netherlands
6 Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Casilla 1280, Antofagasta, Chile
7 Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
8 Department of Physics, Technion, Haifa 32000, Israel
9 Dipartimento di Fisica, Universita degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
10 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
11 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK
12 INAF-IASF Bologna, via Gobetti 101, 40129 Bologna, Italy
13 UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France
14 School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK
Received: 21 April 2011
Accepted: 26 May 2011
We present medium-resolution (λ/Δλ ~ 20 000) ultraviolet spectra covering the 1155−1760 Å spectral range of the Seyfert 1 galaxy Mrk 509 obtained using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST). Our observations were obtained simultaneously with a Low Energy Transmission Grating Spectrometer observation using the Chandra X-ray Observatory, and they are part of a multiwavelength campaign in September through December 2009 which also included observations with XMM-Newton, Swift, and INTEGRAL. Our spectra are the highest signal-to-noise observations to date of the intrinsic absorption components seen in numerous prior ultraviolet observations. To take advantage of the high S/N, we describe special calibrations for wavelength, flat-field and line-spread function corrections that we applied to the COS data. We detect additional complexity in the absorption troughs compared to prior observations made with the Space Telescope Imaging Spectrograph (STIS) on HST. We attribute the UV absorption to a variety of sources in Mrk 509, including an outflow from the active nucleus, the interstellar medium and halo of the host galaxy, and possible infalling clouds or stripped gaseous material from a merger that are illuminated by the ionizing radiation of the active nucleus. Variability between the STIS and COS observation of the most blue-shifted component (#1) allows us to set an upper limit on its distance of <250 pc. Similarly, variability of component 6 between FUSE observations limits its distance to <1.5 kpc. The absorption lines in all components only partially cover the emission from the active nucleus with covering fractions that are lower than those seen in the prior STIS observations and are comparable to those seen in spectra from the Far Ultraviolet Spectroscopic Explorer (FUSE). Given the larger apertures of COS and FUSE compared to STIS, we favor scattered light from an extended region near the active nucleus as the explanation for the partial covering. As observed in prior X-ray and UV spectra, the UV absorption has velocities comparable to the X-ray absorption,but the bulk of the ultraviolet absorption is in a lower ionization state with lower total column density than the gas responsible for the X-ray absorption. We conclude that the outflow from the active nucleus is a multiphase wind.
Key words: galaxies: active / galaxies: individual: Mrk 509 / quasars: absorption lines / galaxies: Seyfert / ultraviolet: galaxies / X-rays: galaxies
Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program # 12022.
Tables 3–7, 9–12, and Appendix are available in electronic form via http://www.aanda.org
© ESO, 2011
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