A new SNR with TeV shell-type morphology: HESS J1731-347
A. Abramowski
,
Fabio Acero
(1)
,
F. Aharonian
,
A. G. Akhperjanian
,
G. Anton
,
Agnès Balzer
,
A. Barnacka
(2)
,
U. Barres de Almeida
,
Y. Becherini
(3, 4)
,
J. Becker
,
B. Behera
,
K. Bernlöhr
,
A. Bochow
,
C. Boisson
(5)
,
J. Bolmont
(6)
,
P. Bordas
,
J. Brucker
,
F. Brun
(3)
,
P. Brun
(2)
,
T. Bulik
,
I. Büsching
,
S. Carrigan
,
S. Casanova
,
M. Cerruti
(5)
,
P. M. Chadwick
,
A. Charbonnier
(6)
,
R. C. G. Chaves
,
A. Cheesebrough
,
L. -M. Chounet
(3)
,
A. C. Clapson
,
G. Coignet
(7)
,
J. Conrad
,
M. Dalton
,
M. K. Daniel
,
I. D. Davids
,
B. Degrange
(3)
,
C. Deil
,
H. J. Dickinson
,
A. Djannati-Ataï
(8)
,
W. Domainko
,
L. O'C. Drury
,
F. Dubois
(7)
,
G. Dubus
(9)
,
J. Dyks
,
M. Dyrda
,
K. Egberts
,
P. Eger
,
P. Espigat
(4)
,
L. Fallon
,
C. Farnier
(1)
,
S. Fegan
(3)
,
F. Feinstein
,
M. V. Fernandes
,
A. Fiasson
(7)
,
G. Fontaine
(3)
,
A. Förster
,
M. Füssling
,
Y. A. Gallant
(1)
,
H. Gast
,
L. Gérard
(4)
,
D. Gerbig
,
B. Giebels
(3)
,
J. F. Glicenstein
(2)
,
B. Glück
,
P. Goret
(2)
,
D. Göring
,
S. Häffner
,
J. D. Hague
,
D. Hampf
,
M. Hauser
,
S. Heinz
,
G. Heinzelmann
,
G. Henri
(9)
,
G. Hermann
,
J. A. Hinton
,
A. Hoffmann
,
W. Hofmann
,
P. Hofverberg
,
M. Holler
,
D. Horns
,
A. Jacholkowska
(6)
,
O. C. de Jager
,
C. Jahn
,
M. Jamrozy
,
I. Jung
,
M. A. Kastendieck
,
K. Katarzynski
,
U. Katz
,
S. Kaufmann
,
D. Keogh
,
D. Khangulyan
,
B. Khélifi
(3)
,
D. Klochkov
,
W. Kluzniak
,
T. Kneiske
,
Nu. Komin
(7)
,
K. Kosack
(2)
,
R. Kossakowski
(7)
,
H. Laffon
(3)
,
G. Lamanna
(7)
,
D. Lennarz
,
T. Löhse
,
A. Lopatin
,
C. -C. Lu
,
V. Marandon
(4)
,
Alexandre Marcowith
(1)
,
Julien Masbou
(7)
,
D. Maurin
(6)
,
N. Maxted
,
T. J. L. Mccomb
,
M. C. Medina
(2)
,
J. Méhault
(1)
,
R. Moderski
,
Emmanuel Moulin
(2)
,
C. L. Naumann
(6)
,
M. Naumann-Godo
(2)
,
M. de Naurois
(3)
,
D. Nedbal
,
D. Nekrassov
,
N. Nguyen
,
B. Nicholas
,
J. Niemiec
,
S. J. Nolan
,
S. Ohm
,
E. de Oña Wilhelmi
(4)
,
B. Opitz
,
M. Ostrowski
,
M. Panter
,
M. Paz Arribas
,
G. Pedaletti
,
G. Pelletier
(9)
,
P. -O. Petrucci
(9)
,
S. Pita
(4)
,
G. Pühlhofer
,
M. Punch
(4)
,
A. Quirrenbach
,
M. Raue
,
S. M. Rayner
,
A. Reimer
,
O. Reimer
,
Matthieu Renaud
(1)
,
R. de Los Reyes
,
F. Rieger
,
J. Ripken
,
L. Rob
,
S. Rosier-Lees
(7)
,
G. Rowell
,
B. Rudak
,
C. B. Rulten
,
J. Ruppel
,
F. Ryde
,
V. Sahakian
,
A. Santangelo
,
R. Schlickeiser
,
F. M. Schöck
,
A. Schulz
,
U. Schwanke
,
S. Schwarzburg
,
S. Schwemmer
,
M. Sikora
,
J. L. Skilton
,
H. Sol
(5)
,
G. Spengle
,
L. Stawarz
,
R. Steenkamp
,
C. Stegmann
,
F. Stinzing
,
K. Stycz
,
I. Sushch
,
A. Szostek
(9)
,
J. -P. Tavernet
(6)
,
R. Terrier
(4)
,
M. Tluczykont
,
K. Valerius
,
C. van Eldik
,
George Vasileiadis
(1)
,
C. Venter
,
J. P. Vialle
(7)
,
A. Viana
(2)
,
P. Vincent
(6)
,
M. Vivier
(2)
,
H. J. Völk
,
F. Volpe
,
S. Vorobiov
(1)
,
M. Vorster
,
S. J. Wagner
,
M. Ward
,
A. Wierzcholska
,
M. Zacharias
,
A. Zajczyk
,
A. A. Zdziarski
,
A. Zech
(5)
,
H. -S. Zechlin
1
LUPM -
Laboratoire Univers et Particules de Montpellier
2 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
3 LLR - Laboratoire Leprince-Ringuet
4 APC (UMR_7164) - AstroParticule et Cosmologie
5 LUTH (UMR_8102) - Laboratoire Univers et Théories
6 LPNHE - Laboratoire de Physique Nucléaire et de Hautes Énergies
7 LAPP - Laboratoire d'Annecy de Physique des Particules
8 APC - AHE - APC - Astrophysique des Hautes Energies
9 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble
2 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
3 LLR - Laboratoire Leprince-Ringuet
4 APC (UMR_7164) - AstroParticule et Cosmologie
5 LUTH (UMR_8102) - Laboratoire Univers et Théories
6 LPNHE - Laboratoire de Physique Nucléaire et de Hautes Énergies
7 LAPP - Laboratoire d'Annecy de Physique des Particules
8 APC - AHE - APC - Astrophysique des Hautes Energies
9 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble
A. Abramowski
- Function : Author
Fabio Acero
- Function : Author
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F. Aharonian
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A. G. Akhperjanian
- Function : Author
G. Anton
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Agnès Balzer
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U. Barres de Almeida
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Y. Becherini
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J. Becker
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A. Bochow
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P. Bordas
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J. Brucker
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P. Brun
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T. Bulik
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I. Büsching
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S. Carrigan
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M. Cerruti
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P. M. Chadwick
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R. C. G. Chaves
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A. Cheesebrough
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A. C. Clapson
- Function : Author
J. Conrad
- Function : Author
M. Dalton
- Function : Author
M. K. Daniel
- Function : Author
I. D. Davids
- Function : Author
C. Deil
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H. J. Dickinson
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W. Domainko
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L. O'C. Drury
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J. Dyks
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L. Fallon
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F. Feinstein
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A. Förster
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H. Gast
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D. Gerbig
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B. Glück
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D. Göring
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S. Häffner
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J. D. Hague
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D. Hampf
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M. Hauser
- Function : Author
S. Heinz
- Function : Author
G. Heinzelmann
- Function : Author
G. Hermann
- Function : Author
J. A. Hinton
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A. Hoffmann
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W. Hofmann
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I. Jung
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D. Lennarz
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George Vasileiadis
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A. Zajczyk
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H. -S. Zechlin
- Function : Author
Abstract
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.