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The hard X-ray spectrum of NGC 5506 as seen by NuSTAR

Matt, G. and Baloković, M. and Marinucci, A. and Ballantyne, D. R. and Boggs, S. E. and Christensen, F. E. and Comastri, A. and Craig, W. W. and Gandhi, P. and Hailey, C. J. and Harrison, F. A. and Madejski, G. and Madsen, K. K. and Stern, D. and Zhang, W. W. (2014) The hard X-ray spectrum of NGC 5506 as seen by NuSTAR. Monthly Notices of the Royal Astronomical Society, 447 (4). pp. 3029-3033. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20150404-122323766

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Abstract

NuSTAR observed the bright Compton-thin, narrow-line Seyfert 1 galaxy, NGC 5506, for about 56 ks. In agreement with past observations, the spectrum is well fitted by a power law with Γ ∼ 1.9, a distant reflection component and narrow ionized iron lines. A relativistically blurred reflection component is not required by the data. When an exponential high-energy cutoff is added to the power law, a value of 720+130/190 keV (90 per cent confidence level) is found. Even allowing for systematic uncertainties, we find a 3σ lower limit to the high-energy cutoff of 350 keV, the highest lower limit to the cutoff energy found so far in an AGN by NuSTAR.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stu2653DOIArticle
http://mnras.oxfordjournals.org/content/447/4/3029PublisherArticle
http://arxiv.org/abs/1412.4541arXivDiscussion Paper
ORCID:
AuthorORCID
Ballantyne, D. R.0000-0001-8128-6976
Boggs, S. E.0000-0001-9567-4224
Comastri, A.0000-0003-3451-9970
Gandhi, P.0000-0003-3105-2615
Harrison, F. A.0000-0003-2992-8024
Madsen, K. K.0000-0003-1252-4891
Stern, D.0000-0003-2686-9241
Additional Information:© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 December 12. Received 2014 November 25. In original form 2014 October 8. First published online January 14, 2015. This work has 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. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. 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). GM, AM and AC acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. GM and AM also acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. MB acknowledges support from the Fulbright International Science and Technology Award.
Group:NuSTAR, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Agenzia Spaziale Italiana (ASI)ASI/INAF I/037/12/0- 011/13
European Community Seventh Framework ProgrammeFP7/2007-2013, 312789
Fulbright International Science and Technology AwardUNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Non-Subject Keywords:accretion, accretion discs – galaxies: active – galaxies: individual: NGC 5506
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2015-69
Record Number:CaltechAUTHORS:20150404-122323766
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20150404-122323766
Official Citation:G. Matt, M. Baloković, A. Marinucci, D. R. Ballantyne, S. E. Boggs, F. E. Christensen, A. Comastri, W. W. Craig, P. Gandhi, C. J. Hailey, F. A. Harrison, G. Madejski, K. K. Madsen, D. Stern, and W. W. Zhang The hard X-ray spectrum of NGC 5506 as seen by NuSTAR MNRAS (March 11, 2015) Vol. 447 3029-3033 doi:10.1093/mnras/stu2653 First published online January 14, 2015
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:56359
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:06 Apr 2015 22:35
Last Modified:21 Mar 2019 19:02

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