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arXiv · 1204.2535

Modeling the Fe K Line Profiles in Type I AGN with a Compton-Thick Disk Wind

M. M. Tatum·T. J. Turner·S. A. Sim·L. Miller·J. N. Reeves·A. R. Patrick·K. S. Long
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Abstract

We have modeled a small sample of Seyfert galaxies that were previously identified as having simple X-ray spectra with little intrinsic absorption. The sources in this sample all contain moderately broad components of Fe K-shell emission and are ideal candidates for testing the applicability of a Compton-thick accretion-disk wind model to AGN emission components. Viewing angles through the wind allow the observer to see the absorption signature of the gas, whereas face-on viewing angles allow the observer to see the scattered light from the wind. We find that the Fe K emission line profiles are well described with a model of a Compton-thick accretion-disk wind of solar abundances, arising tens to hundred of gravitational radii from the central black hole. Further, the fits require a neutral component of Fe K alpha emission that is too narrow to arise from the inner part of the wind, and likely comes from a more distant reprocessing region. Our study demonstrates that a Compton-thick wind can have a profound effect on the observed X-ray spectrum of an AGN, even when the system is not viewed through the flow.

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M. M. Tatum, T. J. Turner, S. A. Sim, L. Miller, J. N. Reeves, A. R. Patrick, K. S. Long. 2012-04-11. Modeling the Fe K Line Profiles in Type I AGN with a Compton-Thick Disk Wind. https://doi.org/10.1088/0004-637x/752/2/94

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