Context :

Aims : The unification scheme of Seyfert galaxies predicts that the observed differences between type 1 and type 2 Seyfert galaxies are solely due to the differing orientations of the toroidal-shaped obscuring material around AGN .
The observed X-ray spectra of Seyfert type 2s compared to type 1s are expected to be affected by higher absorbing column density due to the edge-on view of the obscuring torus .
We study the 0.5 - 10 keV X-ray spectral properties of Seyfert type 1s and type 2s with the aim to test the predictions of Seyfert unification scheme in the X-ray regime .

Methods : We use an optically selected Seyfert sample in which type 1s and type 2s have matched distributions in the orientation independent parameters of AGN and host galaxy .

Results : The 0.5 - 10 keV XMM-Newton pn X-ray spectra of Seyfert galaxies are in general best fitted with a model consists of an absorbed power-law , a narrow Gaussian fitted to the Fe K \alpha emission line and an often seen soft excess component characterized by either a thermal plasma model with temperature kT \sim 0.1 - 1.0 keV and/or a steep power-law .
The 2.0 - 10 keV hard X-ray continuum emission in several Seyfert type 2s is reflection dominated and suggests the Compton-thick obscuration .
Results on the statistical comparison of the distributions of the observed X-ray luminosities in the soft ( 0.5 - 2.0 keV ) and hard ( 2.0 - 10.0 keV ) bands , the X-ray absorbing column densities , the equivalent widths of Fe K \alpha line and the flux ratios of hard X-ray to [ OIII ] \lambda 5007 Å for the two Seyfert subtypes are consistent with the obscuration and orientation based unification scheme .

Conclusions :