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

Wereportresultsfrommulti-epochX-rayobservationsoftheSeyfert1.5galaxyESO362−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 10keV, 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 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 ∼50 gravitational radii. Such result holds not only for the X-ray continuum, but also for the soft excess.