2012ApJ...752...94T -
Astrophys. J., 752, 94 (2012/June-3)
Modeling the Fe K line profiles in type I active galactic nuclei with a compton-thick disk wind.
TATUM M.M., TURNER T.J., SIM S.A., MILLER L., REEVES J.N., PATRICK A.R. and LONG K.S.
Abstract (from CDS):
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 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 Fe K 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 Fe Kα 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.
Abstract Copyright:
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Journal keyword(s):
accretion, accretion disks - galaxies: active - X-rays: galaxies
Simbad objects:
15
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