Black hole spin and size of the X-ray-emitting region(s) in the Seyfert 1.5 galaxy ESO 362-G18

作者：Agis Gonzalez B^*; Miniutti G; Kara E; Fabian A C; Sanfrutos M; Risaliti G; Bianchi S; Strotjohann N L; Saxton R D; Parker M L

来源：Monthly Notices of the Royal Astronomical Society, 2014, 443(4): 2862-2873.

DOI：10.1093/mnras/stu1358

• galaxies: active
• galaxies: Seyfert
• X-rays: galaxies

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 %26gt;= 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 similar to 2 months after a typical mildly absorbed one, is heavily absorbed by a cold column density of similar to 3-4 x 10(23) cm(-2), 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 similar to 50 gravitational radii. Such result holds not only for the X-ray continuum, but also for the soft excess.

• 出版日期2014-10-1