Reference : Black hole spin and size of the X-ray-emitting region(s) in the Seyfert 1.5 galaxy ES...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/231193
Black hole spin and size of the X-ray-emitting region(s) in the Seyfert 1.5 galaxy ESO 362-G18
English
Agis-Gonzalez, Beatriz mailto [Centro de Astrobiología (CSIC-INTA), Dep. de Astrofíica, Villanueva de la Cañada, E-28692, Madrid, Spain > > > >]
Miniutti, G. [Centro de Astrobiologia (CSIC-INTA), Dep. de Astrofisica; ESA, PO Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain]
Kara, E. [Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK]
Fabian, A. C. [Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK]
Sanfrutos, M. [Centro de Astrobiologia (CSIC-INTA), Dep. de Astrofisica; ESA, PO Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain]
Risaliti, G. [Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA; INAF - Osservatorio Astronomico di Arcetri, L.go E. Fermi 5, I-50125 Firenze, Italy]
Bianchi, S. [Dipartimento di Matematica e Fisica, Università degli Studi di Roma Tre, via della Vasca Navale 84, I-00146 Roma, Italy]
Strotjohann, N. L. [Physikalisches Institut, Universität Bonn, Nussallee 12, D-53115 Bonn, Germany]
Saxton, R. D. [XMM SOC, ESA, PO Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain]
Parker, M. L. [Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK)]
1-Oct-2014
Monthly Notices of the Royal Astronomical Society
443
2862-2873
Yes
International
[en] galaxies: active ; galaxies: Seyfert ; X-rays: galaxies
[en] We report results from multi-epoch X-ray observations of the Seyfert 1.5 galaxy ESO 362-G18 performed between 2005 November and 2010 June. ESO 362-G18 generally exhibits the typical X-ray spectrum of type 1 active galactic nuclei. A disc-reflection component accounts for broad residuals in the iron K band and above 10 keV, as well as for a significant soft excess. From our best-fitting reflection model, we measure a black hole spin a ≥ 0.92 at the 99.99 per cent confidence level. ESO 362-G18 is also (typically) mildly absorbed by a column of neutral gas. The absorber is variable and one observation, performed ˜2 months after a typical mildly absorbed one, is heavily absorbed by a cold column density of ˜ 3-4 × 10[SUP]23[/SUP] cm[SUP]-2[/SUP], nearly two orders of magnitude higher than that during any other observation. UV variability between the heavily absorbed observation and the others suggests that the absorber can be identified with a dusty, clumpy torus. The absorption variability time-scale enables us to locate the X-ray-emitting region within the innermost ˜50 gravitational radii. Such result holds not only for the X-ray continuum, but also for the soft excess.
http://hdl.handle.net/2268/231193
10.1093/mnras/stu1358
http://adsabs.harvard.edu/abs/2014MNRAS.443.2862A

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