Spectral Analysis of the Accretion Flow in NGC 1052 with Suzaku

Details Spectral Analysis of the Accretion Flow in NGC 1052 with Suzaku Spectral Analysis of the Accretion Flow in NGC 1052 with Suzaku

2009-03-20

arxiv.org/abs/0903.3583v1

Astrophys.J.698:528-540,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

33 pages, 8 figures, accepted for publication in ApJ

Scientific paper

10.1088/0004-637X/698/1/528

We present an analysis of the 101 ks, 2007 Suzaku spectrum of the LINER galaxy NGC 1052. The 0.5-10 keV continuum is well-modeled by a power-law modified by Galactic and intrinsic absorption, and it exhibits a soft, thermal emission component below 1 keV. Both a narrow core and a broader component of Fe K emission centered at 6.4 keV are robustly detected. While the narrow line is consistent with an origin in material distant from the black hole, the broad line is best fit empirically by a model that describes fluorescent emission from the inner accretion disk around a rapidly rotating black hole. We find no evidence in this observation for Comptonized reflection of the hard X-ray source by the disk above 10 keV, however, which casts doubt on the hypothesis that the broad iron line originates in the inner regions of a standard accretion disk. We explore other possible scenarios for producing this spectral feature and conclude that the high equivalent width (EW ~ 185 keV) and full-width-half-maximum velocity of the broad iron line (v ~ 0.37c) necessitate an origin within d ~ 8 gravitational radii of the hard X-ray source. Based on the confirmed presence of a strong radio jet in this galaxy nucleus, the broad iron line may be produced in dense plasma near the base of the jet, implying that emission mechanisms in the centralmost portions of active galactic nuclei are more complex than previously thought.

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