X-ray illuminated accretion discs - A model for the iron line in NGC 3227

Details X-ray illuminated accretion discs - A model for the iron line in NGC 3227 X-ray illuminated accretion discs - A model for the iron line in NGC 3227

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.242p..28g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 242, Jan. 1, 1990, p. 28P-31P. Research supported by SE

Other

33

Accretion Disks, Active Galactic Nuclei, Astronomical Models, Metallicity, X Ray Spectra, Astronomical Spectroscopy, Emission Spectra, Iron, Optical Thickness, Spectral Line Width

Scientific paper

Substantial amounts of optically thick, 'cold' gas close to the central regions of Active Galactic Nuclei reprocess the underlying nonthermal continuum. In the X-ray band, features due to bound-free absorption, fluorescence, and electron scattering, as well as thermal re-emission are imprinted on the observed spectrum. Iron K-shell features are particularly evident, and provide a strong diagnostic of the geometry and kinematics of the innermost regions of the accretion flow. Here a specific geometry of the cold material is considered, namely that of a Keplerian accretion disk illuminated by an external X-ray source. The results from Monte Carlo simulations of the composite spectrum are fitted to Ginga data from NGC 3227, a Seyfert galaxy with an established emission feature. It is found that the form of the X-ray spectrum of NGC 3227 is consistent with such a model if it is viewed almost face-on. The consequences of our findings for this and other sources are discussed briefly.

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