Modeling the Fe K Line Profiles in Type I AGN with a Compton-Thick Disk Wind
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.
Cite
@article{arxiv.1204.2535,
title = {Modeling the Fe K Line Profiles in Type I AGN with a Compton-Thick Disk Wind},
author = {M. M. Tatum and T. J. Turner and S. A. Sim and L. Miller and J. N. Reeves and A. R. Patrick and K. S. Long},
journal= {arXiv preprint arXiv:1204.2535},
year = {2012}
}