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The Corona of the Broad-Line Radio Galaxy 3C 390.3

Lohfink, A. M. and Ogle, P. and Tombesi, F. and Walton, D. and Baloković, M. and Zoghbi, A. and Ballantyne, D. R. and Boggs, S. E. and Christensen, F. E. and Craig, W. W. and Fabian, A. C. and Hailey, C. J. and Harrison, F. A. and King, A. L. and Madejski, G. and Matt, G. and Reynolds, C. S. and Stern, D. and Ursini, F. and Zhang, W. W. (2015) The Corona of the Broad-Line Radio Galaxy 3C 390.3. Astrophysical Journal, 814 (1). Art. No. 24. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20151022-144502050

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Abstract

We present the results from a joint Suzaku/NuSTAR broadband spectral analysis of 3C 390.3. The high quality data enables us to clearly separate the primary continuum from the reprocessed components allowing us to detect a high energy spectral cut-off (E_(cut) = 117 ^(+18)_(−14) keV), and to place constraints on the Comptonization parameters of the primary continuum for the first time. The hard over soft compactness is 69 ^(+124)_(−24) and the optical depth is 4.1 ^(+0.5)_(−3.6), his leads to an electron temperature of 30 ^(+32)_(−8) keV. Expanding our study of the Comptonization spectrum to the optical/UV by studying the simultaneous Swift-UVOT data, we find indications that the compactness of the corona allows only a small fraction of the total UV/optical flux to be Comptonized. Our analysis of the reprocessed emission show that 3C 390.3 only has a small amount of reflection (R ∼ 0.3), and of that the vast majority is from distant neutral matter. However, we also discover a soft-X-ray excess in the source, which can be described by a weak ionized reflection component from the inner parts of the accretion disk. In addition to the backscattered emission, we also detect the highly ionized iron emission lines Fe xxv and Fe xxvi.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1510.01333arXivDiscussion Paper
http://dx.doi.org/10.1088/0004-637X/814/1/24DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/814/1/24PublisherArticle
ORCID:
AuthorORCID
Ogle, P.0000-0002-3471-981X
Walton, D.0000-0001-5819-3552
Ballantyne, D. R.0000-0001-8128-6976
Boggs, S. E.0000-0001-9567-4224
Harrison, F. A.0000-0003-2992-8024
Stern, D.0000-0003-2686-9241
Additional Information:© 2015 The American Astronomical Society. Received 2015 July 3; accepted 2015 October 5; published 2015 November 13. We thank the anonymous referee for helpful comments. A.L. thanks Julien Malzac for helpful discussions and acknowledges support from the ERC Advanced Grant FEEDBACK. F.T. would like to thank M. Coleman Miller and Brian Morsony for useful comments. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA).
Group:NuSTAR, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASA Earth and Space Science FellowshipNNX14AQ07H
European Research Council (ERC)FEEDBACK
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:galaxies: active; X-rays: individual (3C 390.3)
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2015-21
Record Number:CaltechAUTHORS:20151022-144502050
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20151022-144502050
Official Citation:A. M. Lohfink et al 2015 ApJ 814 24
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:61450
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:22 Oct 2015 21:59
Last Modified:30 Nov 2017 22:07

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