A Chandra-HETG VIEW OF MCG +8-11-11
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Murphy-2014-A Chandra-HETG view.pdf
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1.03 MB
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Author(s)
Murphy, Kendrah Dawn
Nowak, Michael A.
Date Issued
November 2014
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Murphy, K. D., and M. A. Nowak. “A Chandra-HETG VIEW OF MCG +8-11-11.” The Astrophysical Journal 797, no. 1 (November 19, 2014): 12. © 2014 The American Astronomical Society
Version
Final published version
Abstract
We present a spectral analysis of the 118 ks Chandra High Energy Transmission Gratings (HETG) observation of the X-ray bright Seyfert 1.5 galaxy MCG +8-11-11, in conjunction with 100 ks of archival Suzaku data, aimed at investigating the signatures of warm absorption and Compton reflection reported from previous Suzaku and XMM-Newton studies of the source. Contrary to previous results, we find that warm absorption is not required by the data. Instead, we report upper limits on absorption lines that are below previous (marginal) detections. Fe Kα line emission is clearly detected and is likely resolved with σ ~ 0.02 keV with the HETG data. We applied self-consistent, broadband spectral-fitting models to the Chandra and Suzaku data to investigate this and other signatures of distant absorption and reflection. Utilizing in particular the MYTorus model, we find that the data are consistent with reprocessing by a distant, neutral torus that is marginally Compton-thick (N [subscript H] ~10[superscript 24]cm[superscript –2]) and out of the line of sight. However, we do not find compelling evidence of a relativistically broadened Fe K emission line, which is often expected from type 1 active galactic nuclei. This is consistent with some, although not all, previous studies of MCG +8-11-11. A well-measured edge is identified by the HETG near 0.5 keV, indicating neutral absorption in the line of sight that is consistent with galactic absorption; however, the absorption may be partially intrinsic to the source. The HETG data are consistent with the presence of a soft excess, a feature that may be missed by considering the Suzaku data alone.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637X/797/1/12
