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 } = 1.35 - 1.65 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 } = 3.5 - 3.6 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 .