Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2

HESS Collaboration

doi:10.1093/mnras/stu2148

Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2

HESS Collaboration

Institut für Experimentalphysik
Universität Hamburg
Universite Paris-Saclay
Max-Planck-Institut für Kernphysik
Dublin Institute for Advanced Studies
National Academy of Sciences of Armenia
Yerevan Physics Institute
Institut für Physik
Humboldt-Universität zu Berlin
Friedrich-Alexander University (FAU) Erlangen-Nürnberg and Universitätsklinikum Erlangen
Durham University
c/o DESY
University of Potsdam
Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
Department of Physics and Electrical Engineering
Linnaeus University, Växjö
Ruhr-University Bochum
University of Innsbruck
Centre for Space Research
North-West University
LUTH - Laboratoire de l'Univers et de ses Theories
Universités Paris VI and VII
University of Tübingen
Institut Pierre Simon Laplace, CNRS and CEA
University of Warsaw
Center for Astrophysics | Harvard & Smithsonian
European Molecular Biology Laboratory Heidelberg
School of Physics
University of the Witwatersrand, Johannesburg
Landessternwarte Heidelberg
Department of Physics
Stockholm University
Univ. Bordeaux
Department of Physics
University of Namibia
University of Adelaide
Astroparticule and Cosmol APC
Université Grenoble Alpes

Research output: Contribution to journal › Article › peer-review

31 Citations (Scopus)

Abstract

The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the HESS Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position RA = 18^h32^m50^s ± 3_stat ^s ± 2_syst ^s, Dec = -9°22'36″ ± 32_stat ^″ ± 20_syst ^″(J2000), spatially coincident with a part of the radio shell of the neighbouring remnant G22.7-0.2. The photon spectrum is well described by a power law of index Γ = 2.6 ± 0.3_stat ± 0.1_syst and a normalization at 1 TeV of Φ₀ = (4.8 ± 0.8_stat ± 1.0_syst) × 10^-13 cm^-2 s^-1 TeV^-1. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multiwavelength observations will help to shed new light on this intriguing VHE source.

Original language	English
Pages (from-to)	1163-1169
Number of pages	7
Journal	Monthly Notices of the Royal Astronomical Society
Volume	446
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stu2148
Publication status	Published - 1 Jan 2015

Keywords

Astroparticle physics
Gamma-rays: general
ISM: individual objects: HESS J1832-093
ISM: individual objects: SNR G22.7-0.2

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10.1093/mnras/stu2148

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@article{1c7939fde6e94ab084c0c89f79fdab76,

title = "Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2",

abstract = "The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the HESS Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position RA = 18h32m50s ± 3stat s ± 2syst s, Dec = -9°22'36″ ± 32stat ″ ± 20syst ″(J2000), spatially coincident with a part of the radio shell of the neighbouring remnant G22.7-0.2. The photon spectrum is well described by a power law of index Γ = 2.6 ± 0.3stat ± 0.1syst and a normalization at 1 TeV of Φ0 = (4.8 ± 0.8stat ± 1.0syst) {\texttimes} 10-13 cm-2 s-1 TeV-1. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multiwavelength observations will help to shed new light on this intriguing VHE source.",

keywords = "Astroparticle physics, Gamma-rays: general, ISM: individual objects: HESS J1832-093, ISM: individual objects: SNR G22.7-0.2",

author = "\{HESS Collaboration\} and A. Abramowski and F. Acero and F. Aharonian and \{Ait Benkhali\}, F. and Akhperjanian, \{A. G.\} and E. Ang{\"u}ner and G. Anton and S. Balenderan and A. Balzer and A. Barnacka and Y. Becherini and \{Becker Tjus\}, J. and K. Bernl{\"o}hr and E. Birsin and E. Bissaldi and J. Biteau and M. B{\"o}ttcher and C. Boisson and J. Bolmont and P. Bordas and J. Brucker and F. Brun and P. Brun and T. Bulik and S. Carrigan and S. Casanova and M. Cerruti and Chadwick, \{P. M.\} and R. Chalme-Calvet and Chaves, \{R. C.G.\} and A. Cheesebrough and M. Chr{\'e}tien and Clapson, \{A. C.\} and S. Colafrancesco and G. Cologna and J. Conrad and C. Couturier and Y. Cui and M. Dalton and Daniel, \{M. K.\} and Davids, \{I. D.\} and B. Degrange and C. Deil and \{de Wilt\}, P. and Dickinson, \{H. J.\} and A. Djannati-Ata{\"i} and W. Domainko and Drury, \{L. O.C.\} and G. Dubus and S. Fegan",

note = "Publisher Copyright: {\textcopyright} 2014 The Authors.",

year = "2015",

month = jan,

day = "1",

doi = "10.1093/mnras/stu2148",

language = "English",

volume = "446",

pages = "1163--1169",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

}

TY - JOUR

T1 - Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2

AU - HESS Collaboration

AU - Abramowski, A.

AU - Acero, F.

AU - Aharonian, F.

AU - Ait Benkhali, F.

AU - Akhperjanian, A. G.

AU - Angüner, E.

AU - Anton, G.

AU - Balenderan, S.

AU - Balzer, A.

AU - Barnacka, A.

AU - Becherini, Y.

AU - Becker Tjus, J.

AU - Bernlöhr, K.

AU - Birsin, E.

AU - Bissaldi, E.

AU - Biteau, J.

AU - Böttcher, M.

AU - Boisson, C.

AU - Bolmont, J.

AU - Bordas, P.

AU - Brucker, J.

AU - Brun, F.

AU - Brun, P.

AU - Bulik, T.

AU - Carrigan, S.

AU - Casanova, S.

AU - Cerruti, M.

AU - Chadwick, P. M.

AU - Chalme-Calvet, R.

AU - Chaves, R. C.G.

AU - Cheesebrough, A.

AU - Chrétien, M.

AU - Clapson, A. C.

AU - Colafrancesco, S.

AU - Cologna, G.

AU - Conrad, J.

AU - Couturier, C.

AU - Cui, Y.

AU - Dalton, M.

AU - Daniel, M. K.

AU - Davids, I. D.

AU - Degrange, B.

AU - Deil, C.

AU - de Wilt, P.

AU - Dickinson, H. J.

AU - Djannati-Ataï, A.

AU - Domainko, W.

AU - Drury, L. O.C.

AU - Dubus, G.

AU - Fegan, S.

PY - 2015/1/1

Y1 - 2015/1/1

N2 - The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the HESS Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position RA = 18h32m50s ± 3stat s ± 2syst s, Dec = -9°22'36″ ± 32stat ″ ± 20syst ″(J2000), spatially coincident with a part of the radio shell of the neighbouring remnant G22.7-0.2. The photon spectrum is well described by a power law of index Γ = 2.6 ± 0.3stat ± 0.1syst and a normalization at 1 TeV of Φ0 = (4.8 ± 0.8stat ± 1.0syst) × 10-13 cm-2 s-1 TeV-1. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multiwavelength observations will help to shed new light on this intriguing VHE source.

AB - The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the HESS Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position RA = 18h32m50s ± 3stat s ± 2syst s, Dec = -9°22'36″ ± 32stat ″ ± 20syst ″(J2000), spatially coincident with a part of the radio shell of the neighbouring remnant G22.7-0.2. The photon spectrum is well described by a power law of index Γ = 2.6 ± 0.3stat ± 0.1syst and a normalization at 1 TeV of Φ0 = (4.8 ± 0.8stat ± 1.0syst) × 10-13 cm-2 s-1 TeV-1. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multiwavelength observations will help to shed new light on this intriguing VHE source.

KW - Astroparticle physics

KW - Gamma-rays: general

KW - ISM: individual objects: HESS J1832-093

KW - ISM: individual objects: SNR G22.7-0.2

U2 - 10.1093/mnras/stu2148

DO - 10.1093/mnras/stu2148

M3 - Article

AN - SCOPUS:84987994725

SN - 0035-8711

VL - 446

SP - 1163

EP - 1169

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2

Abstract

Keywords

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