A new SNR with TeV shell-type morphology: HESS J1731-347

被引：72

作者：

Abramowski, A. ^{[1
,21
]}

Acero, F. ^{[2
]}

Aharonian, F. ^{[3
,4
,5
]}

Akhperjanian, A. G. ^{[5
,6
]}

Anton, G. ^{[7
]}

Balzer, A. ^{[7
]}

Barnacka, A. ^{[8
,9
]}

de Almeida, U. Barres ^{[10
]}

Becherini, Y. ^{[11
,12
]}

Becker, J. ^{[13
]}

Behera, B. ^{[14
]}

Bernloehr, K. ^{[3
,15
]}

Bochow, A. ^{[3
]}

Boisson, C. ^{[16
]}

Bolmont, J. ^{[17
]}

Bordas, P. ^{[18
]}

Brucker, J. ^{[7
]}

Brun, F. ^{[12
]}

Brun, P. ^{[9
]}

Bulik, T. ^{[19
]}

Buesching, I. ^{[13
,20
]}

Carrigan, S. ^{[3
]}

Casanova, S. ^{[13
]}

Cerruti, M. ^{[16
]}

Chadwick, P. M. ^{[10
]}

Charbonnier, A. ^{[17
]}

Chaves, R. C. G. ^{[3
]}

Cheesebrough, A. ^{[10
]}

Chounet, L. -M. ^{[12
]}

Clapson, A. C. ^{[3
]}

Coignet, G. ^{[21
]}

Cologna, G. ^{[14
]}

Conrad, J. ^{[22
]}

Dalton, M. ^{[15
]}

Daniel, M. K. ^{[10
]}

Davids, I. D. ^{[23
]}

Degrange, B. ^{[12
]}

Deil, C. ^{[3
]}

Dickinson, H. J. ^{[22
]}

Djannati-Atai, A. ^{[11
]}

Domainko, W. ^{[3
]}

Drury, L. O'C. ^{[4
]}

Dubois, F. ^{[21
]}

Dubus, G. ^{[24
]}

Dutson, K. ^{[25
]}

Dyks, J. ^{[8
]}

Dyrda, M. ^{[26
]}

Egberts, K. ^{[27
]}

Eger, P. ^{[7
]}

Espigat, P. ^{[11
]}

机构：

[1] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany

[2] Univ Montpellier 2, Lab Univers & Particules Montpellier, IN2P3, CNRS, F-34095 Montpellier 5, France

[3] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

[4] Dublin Inst Adv Studies, Dublin 2, Ireland

[5] Natl Acad Sci Republ Armenia, Yerevan, Armenia

[6] Yerevan Phys Inst, Yerevan 375036, Armenia

[7] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany

[8] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland

[9] CEA Saclay, DSM IRFU, F-91191 Gif Sur Yvette, France

[10] Univ Durham, Dept Phys, Durham DH1 3LE, England

[11] Univ Paris 07, CNRS, Observ Paris, UMR 7164,CNRS, F-75205 Paris 13, France

[12] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[13] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany

[14] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany

[15] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[16] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France

[17] Univ Paris 07, Univ Paris 06, CNRS, LPNHE,IN2P3, F-75252 Paris 5, France

[18] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

[19] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland

[20] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa

[21] Univ Savoie, CNRS, IN2P3, Lab Annecy le Vieux Phys Particules, F-74941 Annecy Le Vieux, France

[22] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden

[23] Univ Namibia, Dept Phys, Windhoek, Namibia

[24] Univ Grenoble 1, INSU, CNRS, Lab Astrophys Grenoble, F-38041 Grenoble 9, France

[25] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[26] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland

[27] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[28] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland

[29] Nicolaus Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland

[30] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[31] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic

[32] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[33] CNRS, European Associated Lab Gamma Ray Astron, F-75700 Paris, France

[34] Royal Inst Technol KTH, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 531卷

基金：

英国科学技术设施理事会; 新加坡国家研究基金会;

关键词：

astroparticle physics; ISM: supernova remnants; cosmic rays; XMM-NEWTON OBSERVATIONS; X-RAY-EMISSION; MOLECULAR CLOUDS; SPIRAL STRUCTURE; MILKY-WAY; SUPERNOVA; DISCOVERY; RADIO; ACCELERATION; COUNTERPART;

D O I：

10.1051/0004-6361/201016425

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The recent discovery of the radio shell-type supernova remnant (SNR), G353.6-0.7, in spatial coincidence with the unidentified TeV source HESS J1731-347 has motivated further observations of the source with the High Energy Stereoscopic System (HESS) Cherenkov telescope array to test a possible association of the gamma-ray emission with the SNR. Methods. With a total of 59 h of observation, representing about four times the initial exposure available in the discovery paper of HESS J1731-347, the gamma-ray morphology is investigated and compared with the radio morphology. An estimate of the distance is derived by comparing the interstellar absorption derived from X-rays and the one obtained from (CO)-C-12 and HI observations. Results. The deeper gamma-ray observation of the source has revealed a large shell-type structure with similar position and extension (r similar to 0.25 degrees) as the radio SNR, thus confirming their association. By accounting for the HESS angular resolution and projection effects within a simple shell model, the radial profile is compatible with a thin, spatially unresolved, rim. Together with RX J1713.7-3946, RX J0852.0-4622 and SN 1006, HESS J1731-347 is now the fourth SNR with a significant shell morphology at TeV energies. The derived lower limit on the distance of the SNR of 3.2 kpc is used together with radio and X-ray data to discuss the possible origin of the gamma-ray emission, either via inverse Compton scattering of electrons or the decay of neutral pions resulting from proton-proton interaction.

引用

页数：9

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