A Supernova Remnant Counterpart for HESS J1832?085
Maxted,Nigel I.1; Filipovi?,M. D.2; Hurley-Walker,N.3; Boji?i?,I.2; Rowell,G. P.4; Haberl,F.5; Ruiter,A. J.1; Seitenzahl,I. R.1; Panther,F.1; Wong,G. F.2,6; Braiding,C.6; Burton,M.7; Pühlhofer,G.8; Sano,H.9; Fukui,Y.9; Sasaki,M.10; Tian,W.11,12; Su,H.11; Cui,X.11; Leahy,D.13; Hancock,P. J.3,14
Source PublicationThe Astrophysical Journal
AbstractAbstract We examine the new Galactic supernova remnant (SNR) candidate, G23.11+0.18, as seen by the Murchison Widefield Array radio telescope. We describe the morphology of the candidate and find a spectral index of ?0.63?±?0.05 in the 70–170 MHz domain. Coincident TeV gamma-ray detection in High Energy Stereoscopic System (HESS) data supports the SNR nature of G23.11+0.18 and suggests that G23.11+0.18 is accelerating particles beyond TeV energies, thus making this object a promising new cosmic-ray hadron source candidate. The remnant cannot be seen in current optical, infrared and X-ray data sets. We do find, however, a dip in CO-traced molecular gas at a line-of-sight velocity of ~85 km s?1, suggesting the existence of a G23.11+0.18 progenitor wind-blown bubble. Furthermore, the discovery of molecular gas clumps at a neighboring velocity toward HESS J1832?085 adheres to the notion that a hadronic gamma-ray production mechanism is plausible toward the north of the remnant. Based on these morphological arguments, we propose an interstellar medium association for G23.11+0.18 at a kinematic distance of 4.6?±?0.8 kpc.
KeywordSupernova remnants Interstellar medium Interstellar molecules Gamma-ray sources Galactic cosmic-rays
WOS IDIOP:0004-637X-885-2-ab3e3f
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.School of Science, The University of New South Wales, Australian Defence Force Academy, Canberra 2610, Australia;
2.Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia
3.International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia
4.School of Physical Sciences, The University of Adelaide, Adelaide 5005, Australia
5.Max-Planck-Institut für extraterrestrische Physik, Giessenbachstra?e, D-85748 Garching, Germany
6.School of Physics, The University of New South Wales, Sydney 2052, Australia
7.Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, UK
8.Institut für Astronomie und Astrophysik, Universit?t Tübingen, D-72076 Tübingen, Germany
9.Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan
10.Dr. Karl Remeis Observatory and ECAP, Universit?t Erlangen-Nürnberg, Sternwartstr. 7, D-96049 Bamberg, Germany
11.National Astronomical Observatories, CAS, Beijing 100012, People’s Republic of China
12.University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
13.Department of Physics & Astronomy, University of Calgary, Calgary, Alberta T2N 1N4, Canada
14.ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia
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GB/T 7714
Maxted,Nigel I.,Filipovi?,M. D.,Hurley-Walker,N.,et al. A Supernova Remnant Counterpart for HESS J1832?085[J]. The Astrophysical Journal,2019,885(2).
APA Maxted,Nigel I..,Filipovi?,M. D..,Hurley-Walker,N..,Boji?i?,I..,Rowell,G. P..,...&Hancock,P. J..(2019).A Supernova Remnant Counterpart for HESS J1832?085.The Astrophysical Journal,885(2).
MLA Maxted,Nigel I.,et al."A Supernova Remnant Counterpart for HESS J1832?085".The Astrophysical Journal 885.2(2019).
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