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Statements

Subject Item
n2:RIV%2F00216208%3A11320%2F11%3A10104592%21RIV12-GA0-11320___
rdf:type
n6:Vysledek skos:Concept
dcterms:description
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 (12)CO 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. 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 (12)CO 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.
dcterms:title
A new SNR with TeV shell-type morphology: HESS J1731-347 A new SNR with TeV shell-type morphology: HESS J1731-347
skos:prefLabel
A new SNR with TeV shell-type morphology: HESS J1731-347 A new SNR with TeV shell-type morphology: HESS J1731-347
skos:notation
RIV/00216208:11320/11:10104592!RIV12-GA0-11320___
n6:predkladatel
n7:orjk%3A11320
n4:aktivita
n8:Z n8:P
n4:aktivity
P(GPP203/11/P363), P(LC527), Z(MSM0021620859)
n4:cisloPeriodika
1
n4:dodaniDat
n17:2012
n4:domaciTvurceVysledku
n13:6144063 n13:9283439
n4:druhVysledku
n12:J
n4:duvernostUdaju
n21:S
n4:entitaPredkladatele
n20:predkladatel
n4:idSjednocenehoVysledku
183970
n4:idVysledku
RIV/00216208:11320/11:10104592
n4:jazykVysledku
n16:eng
n4:klicovaSlova
cosmic rays; ISM: supernova remnants; astroparticle physics
n4:klicoveSlovo
n5:astroparticle%20physics n5:ISM%3A%20supernova%20remnants n5:cosmic%20rays
n4:kodStatuVydavatele
DE - Spolková republika Německo
n4:kontrolniKodProRIV
[0128C785EF33]
n4:nazevZdroje
Astronomy and Astrophysics
n4:obor
n18:BF
n4:pocetDomacichTvurcuVysledku
2
n4:pocetTvurcuVysledku
190
n4:projekt
n15:GPP203%2F11%2FP363 n15:LC527
n4:rokUplatneniVysledku
n17:2011
n4:svazekPeriodika
531
n4:tvurceVysledku
Abramowski, A. Aharonian, F. Nedbal, Dalibor Acero, F. Rob, Ladislav
n4:wos
000293017700080
n4:zamer
n9:MSM0021620859
s:issn
0004-6361
s:numberOfPages
9
n11:doi
10.1051/0004-6361/201016425
n19:organizacniJednotka
11320