Combined Analysis of X-Ray Spectra of NGC 3227
  The 1.5 Seyfert galaxy NGC 3227 has been observed by several X-ray missions.
We carried out combined analysis of the data obtained by more recent major
observations of this source - two observations performed by XMM-Newton in 2000
and 2006 and six observations performed by Suzaku in 2008.
  A unified model was constructed which is consistent with all eight of the
observations by the two satillites with large intensity and spectral changes.
The model consists of a hard power law with the spectral index of
Gamma_Hard=1.4-1.7 which is interpreted as the Comptonized emission from the
corona above an accretion disk. In the high flux states an additional soft
excess component dominates, which is consistent with a model with either a
steeper power law with Gamma_Soft=3.3-3.85 or the warm Comptonization
component. These emissions from the central engine are absorbed by a neutral
partial covering material and warm absorbers. A reflection component and
several emission lines are also present. We examined the relationship between
the intrinsic luminosity and the absorbers' physical parameters such as the
column density, which suggests that the source expanded significantly during
the bright states where the soft excess is greatly enhanced.
