The iron emission line complex of MCG‐5‐23‐16: the long XMMNewton look | Zendy

Braito V. | Zendy; Reeves J. N. | Zendy; Dewangan G. | Zendy; George I. | Zendy; Griffiths R. | Zendy; Markowitz A. | Zendy; Nandra K. | Zendy; Porquet D. | Zendy; Ptak A. | Zendy; Turner T. J. | Zendy; Yaqoob T. | Zendy; Weaver K. | Zendy

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The iron emission line complex of MCG‐5‐23‐16: the long XMMNewton look

Author(s) -

Braito V.,

Reeves J. N.,

Dewangan G.,

George I.,

Griffiths R.,

Markowitz A.,

Nandra K.,

Porquet D.,

Ptak A.,

Turner T. J.,

Yaqoob T.,

Weaver K.

Publication year - 2006

Publication title -

astronomische nachrichten

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 0.394

H-Index - 63

eISSN - 1521-3994

pISSN - 0004-6337

DOI - 10.1002/asna.200610694

Subject(s) - physics , astrophysics , emission spectrum , line (geometry) , galaxy , accretion disc , outflow , accretion (finance) , k line , absorption (acoustics) , absorption spectroscopy , gravitation , spectral line , astronomy , stars , optics , geometry , mathematics , meteorology

We present the results of the simultaneous XMM‐ Newton and Chandra observations of the bright Seyfert 1.9 galaxy MCG–5‐23‐16, which is one of the best known examples of a relativistically broadened iron K α line. We find that: a) the soft X‐ray emission is likely to be dominated by photoionized gas, b) the complex iron emission line is best modelled with a narrow and a broad component with a FWHM ∼44000 km/s. This latter component has an EW ∼50 eV and its profile is well described with an emission line mainly originating from the accretion disk a few tens of gravitational radii from the central black hole and viewed with an inclination angle ∼40°. We found evidence of a possible sporadic absorption line at ∼7.7 keV which, if associated with Fe XXVI K α resonance absorption, is indicative of a possible high velocity ( v ∼ 0.1 c ) outflow. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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