Modeling the FeK line profiles in type i active galactic nuclei 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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25 Citations (Scopus)

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 FeK-shell emission and are ideal candidates for testing the applicability of a Compton-thick accretion disk wind model to active galactic nucleus (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 FeK emission line profiles are well described with a model of a Compton-thick accretion disk wind of solar abundances, arising tens to hundreds of gravitational radii from the central black hole. Further, the fits require a neutral component of FeKa 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.
Original languageEnglish
JournalAstrophysical Journal
Volume752
Issue number2
DOIs
Publication statusPublished - 20 Jun 2012

Bibliographical note

Copyright 2012 Elsevier B.V., All rights reserved.

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