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

Journal Article · Wed Jun 20 00:00:00 EDT 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/752/2/94· OSTI ID:22037051

Tatum, M M; Turner, T J ^[1]; Sim, S A ^[2]; Miller, L ^[3]; Reeves, J N; Patrick, A R ^[4]; Long, K S ^[5]

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1. Department of Physics, University of Maryland, Baltimore County, Baltimore, MD 21250 (United States)
2. Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611 (Australia)
3. Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH (United Kingdom)
4. Astrophysics Group, School of Physical and Geographical Sciences, Keele University, Keele, Staffordshire ST5 5BG (United Kingdom)
5. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)

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.

• OSTI ID: 22037051
• Journal Information: Astrophysical Journal, Vol. 752, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ABSORPTION
ABUNDANCE
ACCRETION DISKS
ASTRONOMY
BLACK HOLES
COMPTON EFFECT
COMPUTERIZED SIMULATION
GALAXY NUCLEI
IRON
K SHELL
PHOTON EMISSION
REPROCESSING
SEYFERT GALAXIES
STELLAR WINDS
VISIBLE RADIATION
X-RAY GALAXIES
X-RAY SPECTRA