  The spectrum of the bright Seyfert I galaxy MCG-6-30-15 shows a broad Fe
K-alpha emission line, generally interpreted to originate very close to the
central black hole which must then have a high spin. The observed X-ray
variability is driven by a powerlaw component, with little variability found in
the iron line energy band. The disconnection of continuum and line variability
may be a consequence of strong gravitational light bending. The X-ray spectrum
of MCG-6-30-15 is however complex, strongly modified at soft X-ray energies by
warm absorbers, which some workers have extended to build an
absorption-dominated model of the whole source behaviour. The absorption model
interprets the whole X-ray spectrum without a relativistic reflection component
and attributes most variability to the warm absorbers. We re-examine the
XMM-Newton, Chandra and Suzaku data taken in 2001, 2004 and 2006, respectively,
and construct a model consisting of several warm absorbers confirmed by
spectral analysis, together with a relativistically blurred reflection
component that explains both the soft and hard excesses as well. The model
works well on data from all epochs, demonstrating that the reflection model
provides a consistent interpretation of the broadband spectrum of MCG-6-30-15.
