Abstract
The AGN MCG-6-30-15, which shares many similarities with narrow line Seyfert 1 (NLS1) galaxies, shows a broad Fe K-α line that is generally explained as reflection from the inner part of an accretion disc around a fast spinning black hole. The flux of the line was expected to follow that of the powerlaw component, but little variability was found. The disconnection of continuum and line variability may be caused by strong gravitational light bending. However, some workers have built an absorption model and attribute most variability to the warm absorbers. They claim relativistic reflection is not needed to explain the source behaviour and the hard excess. We reexamine the XMM-Newton, Chandra and Suzaku data taken in different epochs and construct a model consisting of several warm absorbers, together with a relativistic reflection component that explains both the soft and hard excesses. Our model works well on all data, implying it provides a consistent interpretation of the broadband spectrum of MCG-6-30-15.
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