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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)