• DOI:10.1111/j.1365-2966.2005.09048.x
• Corpus ID: 17835973

The XMM-Newton view of Mrk 3 and IXO 30

@article{Bianchi2005TheXV,
  title={The XMM-Newton view of Mrk 3 and IXO 30},
  author={Stefano Bianchi and Giovanni Miniutti and Andrew C. Fabian and Kazushi Iwasawa},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2005},
  volume={360},
  pages={380-389}
}

• S. Bianchi, G. Miniutti, +1 author K. Iwasawa
• Published 29 March 2005
• Physics
• Monthly Notices of the Royal Astronomical Society

We present the analysis of the XMM-Newton EPIC pn spectrum of the Seyfert 2 galaxy, Mrk 3. We confirm that the source is dominated by a pure Compton reflection component and an iron Kα line, both produced as reflection from a Compton-thick torus, likely responsible also for the large column density (1.36 +0.03 0.04 × 10 24 cm 2 ) which is pierced by the primary powerlaw only at high energies. A low inclination angle and an iron underabundance of a factor ≃ 0.82, suggested by the amount of reflection and the depth of the iron edge, are consistent with the iron Kα line EW with respect to the Compton reflection component, being 610 +30 50 eV. Moreover, the iron line width, σ = 32 +13 14 eV, 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 Fe xxv emission line at 6.71 +0.03