MODELING THE Fe K LINE PROFILES IN TYPE I ACTIVE GALACTIC NUCLEI WITH A COMPTON-THICK DISK WIND

• Published in: The Astrophysical journal Vol. 752; no. 2; pp. 1 - 9
• Main Authors: TATUM, M. M, TURNER, T. J, SIM, S. A, MILLER, L, REEVES, J. N, PATRICK, A. R, LONG, K. S
• Format: Journal Article
• Language: English
• Published: Bristol IOP 20.06.2012
• Subjects: ABSORPTION; ABUNDANCE; ACCRETION DISKS; Active galactic nuclei; ASTRONOMY; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BLACK HOLES; COMPTON EFFECT; COMPUTERIZED SIMULATION; Earth, ocean, space; Emission; Emission analysis; Exact sciences and technology; GALAXY NUCLEI; IRON; K SHELL; Mathematical models; PHOTON EMISSION; REPROCESSING; SEYFERT GALAXIES; STELLAR WINDS; VISIBLE RADIATION; X-RAY GALAXIES; X-RAY SPECTRA; X-rays; Line shape; X-ray galaxies; Black holes; accretion, accretion disks; X-rays: galaxies; Cosmic x-ray sources; K shell; Viewing angle; X-ray spectra; Accretion disks; Active galaxies; Seyfert galaxies; galaxies: active; Scattered light; Active galaxy nuclei; Galaxy nuclei; K line; Cosmology; Models; Modelling; Emission line; Solar wind
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/752/2/94

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 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.