Abramowski, A.Büsching, I.De Jager, O.C.Venter, C.Vorster, M.H.E.S.S. Collaboration2012-09-052012-09-052011Abramowski, 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]0004-63611432-0746 (Online)http://hdl.handle.net/10394/7232https://doi.org/10.1051/0004-6361/201016425Aims. 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.enAstroparticle physicsISM: supernova remnantsCosmic raysArticle