dc.contributor.author | Abramowski, A. | |
dc.contributor.author | Büsching, I. | |
dc.contributor.author | De Jager, O.C. | |
dc.contributor.author | Venter, C. | |
dc.contributor.author | Vorster, M. | |
dc.contributor.author | H.E.S.S. Collaboration | |
dc.date.accessioned | 2012-09-05T08:29:39Z | |
dc.date.available | 2012-09-05T08:29:39Z | |
dc.date.issued | 2011 | |
dc.identifier.citation | Abramowski, A. et al. 2011. A new SNR with TeV shell-type morphology: HESS J1731-347. Astronomy & astrophysics, 531: Article no A81. [https://doi.org/10.1051/0004-6361/201016425] | en_US |
dc.identifier.issn | 0004-6361 | |
dc.identifier.issn | 1432-0746 (Online) | |
dc.identifier.uri | http://hdl.handle.net/10394/7232 | |
dc.identifier.uri | https://doi.org/10.1051/0004-6361/201016425 | |
dc.description.abstract | 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 γ-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 γ-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.
Results. The deeper γ-ray observation of the source has revealed a large shell-type structure with similar position and extension (r ∼ 0.25◦) 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 γ-ray emission, either via inverse Compton scattering of electrons or the decay of neutral pions resulting from proton-proton interaction. | en_US |
dc.language.iso | en | en_US |
dc.publisher | EDP Sciences | en_US |
dc.subject | Astroparticle physics | en_US |
dc.subject | ISM: supernova remnants | en_US |
dc.subject | Cosmic rays | en_US |
dc.title | A new SNR with TeV shell-type morphology: HESS J1731-347 | en_US |
dc.type | Article | en_US |
dc.contributor.researchID | 12792322 - Vorster, Michael Johannes | |
dc.contributor.researchID | 12006653 - Venter, Christo | |
dc.contributor.researchID | 10065857 - De Jager, Ocker Cornelis | |
dc.contributor.researchID | 13235176 - Büsching, Ingo | |