The XMM-Newton view of Mrk3 and IXO30
We present the analysis of the XMM-Newton EPIC pn spectrum of the Seyfert 2 galaxy, Mrk3. We confirm that the source is dominated by a pure Compton reflection component and an iron K$α$ line, both produced as reflection from a Compton-thick torus, likely responsible also for the large column density which is pierced by the primary powerlaw only at high energies. A low inclination angle and an iron underabundance, suggested by the amount of reflection and the depth of the iron edge, are consistent with the iron K$α$ line EW with respect to the Compton reflection component. Moreover, the iron line width, if interpreted in terms of Doppler broadening due to the Keplerian rotation of the torus, puts an estimate to the inner radius of the latter, $r=0.6^{+1.3}_{-0.3} \sin^2{i}$ pc. Finally, two different photoionised reflectors are needed to take into account a large number of soft X-ray emission lines from N, O, Ne, Mg, Si, Fe L and the FeXXV emission line. RGS spectra show that the soft X-ray spectrum is dominated by emission lines, while the underlying continuum is best fitted by an unabsorbed powerlaw with the same photon index of the primary continuum, produced as reflection by a photoionised material with a column density of a few $10^{22}$ cm$^{-2}$. We also present the first X-ray spectrum of ROSAT source IXO30, which shows a huge iron line and is well represented either by an absorbed powerlaw or bremsstrahlung emission. Its spectral properties point to a likely identification in terms of a weak Galactic Cataclysmic Variable, but the lack of any optical counterpart precludes excluding other possibilities, like an ULX at the distance of Mrk3.