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