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NuSTAR Hard X-ray Observation of the Gamma-ray Binary Candidate HESS J1832-093

Mori, Kaya and Gotthelf, E. V. and Hailey, Charles J. and Hord, Ben J. and de Oña Wilhelmi, Emma and Rahoui, Farid and Tomsick, John A. and Zhang, Shuo and Hong, Jaesub and Garvin, Amani M. and Boggs, Steven E. and Christensen, Finn E. and Craig, William W. and Harrison, Fiona A. and Stern, Daniel and Zhang, William W. (2017) NuSTAR Hard X-ray Observation of the Gamma-ray Binary Candidate HESS J1832-093. Astrophysical Journal, 848 (2). Art. No. 80. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20171006-100701228

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Abstract

We present a hard X-ray observation of the TeV gamma-ray binary candidate HESS J1832−093, which is coincident with the supernova remnant G22.7−0.2, using the Nuclear Spectroscopic Telescope Array. Non-thermal X-ray emission from XMMU J183245−0921539, the X-ray source associated with HESS J1832−093, is detected up to ~30 keV and is well-described by an absorbed power-law model with a best-fit photon index Γ = 1.5 ± 0.1. A re-analysis of archival Chandra and XMM-Newtondata finds that the long-term X-ray flux increase of XMMU J183245−0921539 is 50^(+40)_(-20)% (90% C.L.), much less than previously reported. A search for a pulsar spin period or binary orbit modulation yields no significant signal to a pulse fraction limit of f_p < 19% in the range 4 ms < P < 40 ks. No red noise is detected in the FFT power spectrum to suggest active accretion from a binary system. While further evidence is required, we argue that the X-ray and gamma-ray properties of XMMU J183245−0921539 are most consistent with a non-accreting binary generating synchrotron X-rays from particle acceleration in the shock formed as a result of the pulsar and stellar wind collision. We also report on three nearby hard X-ray sources, one of which may be associated with diffuse emission from a fast-moving supernova fragment interacting with a dense molecular cloud.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa8d15DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa8d15/metaPublisherArticle
http://arxiv.org/abs/1710.02118arXivDiscussion Paper
ORCID:
AuthorORCID
Mori, Kaya0000-0002-9709-5389
Gotthelf, E. V.0000-0003-3847-3957
Rahoui, Farid0000-0001-7655-4120
Tomsick, John A.0000-0001-5506-9855
Zhang, Shuo0000-0002-2967-790X
Boggs, Steven E.0000-0001-9567-4224
Christensen, Finn E.0000-0001-5679-1946
Harrison, Fiona A.0000-0003-2992-8024
Stern, Daniel0000-0003-2686-9241
Zhang, William W.0000-0002-1426-9698
Additional Information:© 2017 The American Astronomical Society. Received 2017 June 16; revised 2017 August 19; accepted 2017 September 12; published 2017 October 13. This work was supported under NASA Contract No. NNG08FD60C, and 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).
Group:Space Radiation Laboratory, NuSTAR
Funders:
Funding AgencyGrant Number
NASANNG08FD60C
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:gamma rays: general – radiation mechanisms: non-thermal – X-rays: binaries
Record Number:CaltechAUTHORS:20171006-100701228
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20171006-100701228
Official Citation:Kaya Mori et al 2017 ApJ 848 80
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82158
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:06 Oct 2017 17:13
Last Modified:17 Oct 2017 21:45

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