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arxiv: 1105.3206 · v2 · submitted 2011-05-16 · 🌌 astro-ph.HE

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

HESS Collaboration: A. Abramowski , F. Acero , F. Aharonian , A.G. Akhperjanian , G. Anton , A. Balzer , A. Barnacka , U. Barres de Almeida
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A.R. Bazer-Bachi Y. Becherini J. Becker B. Behera K. Bernl\"ohr A. Bochow C. Boisson J. Bolmont P. Bordas V. Borrel J. Brucker F. Brun P. Brun T. Bulik I. B\"usching S. Carrigan S. Casanova M. Cerruti P.M. Chadwick A. Charbonnier R.C.G. Chaves A. Cheesebrough L.-M. Chounet A.C. Clapson G. Coignet J. Conrad M. Dalton M.K. Daniel I.D. Davids B. Degrange C. Deil H.J. Dickinson A. Djannati-Ata\"i W. Domainko L.O'C. Drury F. Dubois G. Dubus J. Dyks M. Dyrda K. Egberts P. Eger P. Espigat L. Fallon C. Farnier S. Fegan F. Feinstein M.V. Fernandes A. Fiasson G. Fontaine A. F\"orster M. F\"u{\ss}ling Y.A. Gallant H. Gast L. G\'erard D. Gerbig B. Giebels J.F. Glicenstein B. Gl\"uck P. Goret D. G\"oring S. H\"affner J.D. Hague D. Hampf M. Hauser S. Heinz G. Heinzelmann G. Henri G. Hermann J.A. Hinton A. Hoffmann W. Hofmann P. Hofverberg M. Holler D. Horns A. Jacholkowska O.C. de Jager C. Jahn M. Jamrozy I. Jung M.A. Kastendieck K. Katarzynski U. Katz S. Kaufmann D. Keogh D. Khangulyan B. Kh\'elifi D. Klochkov W. Kluzniak T. Kneiske Nu. Komin K. Kosack R. Kossakowski H. Laffon G. Lamanna D. Lennarz T. L\"ohse A. Lopatin C.-C. Lu V. Marandon A. Marcowith J. Masbou D. Maurin N. Maxted T.J.L. McComb M.C. Medina J. M\'ehault R. Moderski E. Moulin C.L. Naumann M. Naumann-Godo M. de Naurois D. Nedbal D. Nekrassov N. Nguyen B. Nicholas J. Niemiec S.J. Nolan S. Ohm J-P. Olive E. de O\~na Wilhelmi B. Opitz M. Ostrowski M. Panter M. Paz Arribas G. Pedaletti G. Pelletier P.-O. Petrucci S. Pita G. P\"uhlhofer M. Punch A. Quirrenbach M. Raue S.M. Rayner A. Reimer O. Reimer M. Renaud R. de los Reyes F. Rieger J. Ripken L. Rob S. Rosier-Lees G. Rowell B. Rudak C.B. Rulten J. Ruppel F. Ryde V. Sahakian A. Santangelo R. Schlickeiser F.M. Sch\"ock A. Schulz U. Schwanke S. Schwarzburg S. Schwemmer M. Sikora J.L. Skilton H. Sol G. Spengle L. Stawarz R. Steenkamp C. Stegmann F. Stinzing K. Stycz I. Sushch A. Szostek J.-P. Tavernet R. Terrier O. Tibolla3 M. Tluczykont K. Valerius C. van Eldik G. Vasileiadis C. Venter J.P. Vialle A. Viana P. Vincent M. Vivier H.J. V\"olk F. Volpe S. Vorobiov M. Vorster S.J. Wagner M. Ward A. Wierzcholska M. Zacharias A. Zajczyk A.A. Zdziarski A. Zech H.-S. Zechlin
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classification 🌌 astro-ph.HE
keywords gamma-rayhessj1731-347morphologyradioderivedshell-typesource
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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 (H.E.S.S.) Cherenkov telescope array to test a possible association of the gamma-ray emission with the SNR. With a total of 59 hours 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 12CO and HI observations. The deeper gamma-ray observation of the source has revealed a large shell-type structure with similar position and extension (r~0.25{\deg}) as the radio SNR, thus confirming their association. By accounting for the H.E.S.S. 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.

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Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. CTAO Simulations for Potential PeVatron Candidates

    astro-ph.HE 2026-03 unverdicted novelty 3.0

    CTAO simulations exclude Cassiopeia A, RX J1713.7-3946, and HESS J1731-347 as PeVatrons via PTS metric while HAWC J2227+610 stays inconclusive, with 100 hours required to resolve proton cut-offs near 600 TeV.