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H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud

A. Abramowski F. Aharonian F. Ait Benkhali A. Akhperjanian E. Angüner M. Backes S. Balenderan Agnès Balzer A. Barnacka 1 Y. Becherini J. Becker Tjus D. Berge S. Bernhard K. Bernlöhr E. Birsin J. Biteau 2 M. Böttcher C. Boisson 3 J. Bolmont 4 P. Bordas J. Bregeon 5 F. Brun P. Brun M. Bryan 6 T. Bulik 7 S. Carrigan S. Casanova 8 P. Chadwick N. Chakraborty R. Chalme-Calvet 4 R. Chaves 5 M. Chrétien 4 S. Colafrancesco G. Cologna J. Conrad C. Couturier 4 Y. Cui I. Davids B. Degrange 2 C. Deil P. Dewilt A. Djannati-Ataï 9 W. Domainko A. Donath 10 L. O’c. Drury G. Dubus 11 K. Dutson J. Dyks M. Dyrda T. Edwards K. Egberts P. Eger P. Espigat 9 C. Farnier S. Fegan 2 F. Feinstein 5 M. Fernandes 12 D. Fernandez 5 A. Fiasson 13 G. Fontaine 2 A. Förster M. Füssling S. Gabici 9 M. Gajdus Y. Gallant 5 T. Garrigoux 4 G. Giavitto 14 B. Giebels 2 J. Glicenstein D. Gottschall M.-H. Grondin 15 M. Grudzińska D. Hadasch 16 S. Häffner J. Hahn J. Harris G. Heinzelmann G. Henri 11 G. Hermann O. Hervet 3 A. Hillert J. Hinton W. Hofmann P. Hofverberg M. Holler 17 D. Horns A. Ivascenko A. Jacholkowska 4 C. Jahn M. Jamrozy M. Janiak F. Jankowsky I. Jung-Richardt M. Kastendieck K. Katarzyński U. Katz 18 S. Kaufmann B. Khelifi 9 Michel Kieffer 4 S. Klepser 19 D. Klochkov W. Kluźniak D. Kolitzus Nu. Komin K. Kosack 1 S. Krakau F. Krayzel 13 P. Krüger H. Laffon 15 G. Lamanna 13 J. Lefaucheur 9 V. Lefranc 20 A. Lemiere 9 M. Lemoine-Goumard 15 J.-P. Lenain 4 T. Lohse A. Lopatin C.-C. Lu 10 V. Marandon Alexandre Marcowith 5 R. Marx G. Maurin 13 N. Maxted 5 M. Mayer T. Mccomb J. Mehault 15 P. Meintjes U. Menzler M. Meyer A. Mitchell R. Moderski M. Mohamed K. Morå Emmanuel Moulin T. Murach M. de Naurois 2 J. Niemiec S. Nolan L. Oakes H. Odaka S. Ohm B. Opitz M. Ostrowski I. Oya M. Panter R. Parsons M. Paz Arribas N. Pekeur G. Pelletier P.-O. Petrucci 11 B. Peyaud 21 S. Pita 9 H. Poon G. Pühlhofer M. Punch 9 A. Quirrenbach S. Raab I. Reichardt 9 A. Reimer O. Reimer Matthieu Renaud 5 R. de Los Reyes F. Rieger 1 C. Romoli S. Rosier-Lees 13 G. Rowell 22 B. Rudak 3 C. Rulten 3 V. Sahakian D. Salek D. Sanchez 13 A. Santangelo R. Schlickeiser F. Schussler A. Schulz U. Schwanke 23 S. Schwarzburg S. Schwemmer H. Sol 3 F. Spanier G. Spengler 24 F. Spies Ł. Stawarz R. Steenkamp C. Stegmann 3 F. Stinzing K. Stycz I. Sushch 25 J.-P. Tavernet 4 T. Tavernier 9 A. Taylor R. Terrier 9 M. Tluczykont C. Trichard 13 K. Valerius 18 C. van Eldik B. van Soelen George Vasileiadis 5 J. Veh C. Venter 25 A. Viana P. Vincent 4 J. Vink 26 H. Völk F. Volpe M. Vorster T. Vuillaume S. Wagner P. Wagner R. Wagner M. Ward M. Weidinger Q. Weitzel R. White A. Wierzcholska P. Willmann 27 A. Wörnlein D. Wouters 1 R. Yang V. Zabalza D. Zaborov 2 M. Zacharias A. Zdziarski A. Zech 3 H.-S. Zechlin 
Abstract : G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV GeV) gamma-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E> 100 GeV) gamma-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F(E> 400 GeV) = (6.5 +- 1.1_stat +- 1.3_syst) x 10^-13 phcm^-2s^-1 corresponding to ~0.7% of that of the Crab Nebula and to a luminosity of ~10^34 erg s^-1 above the same energy threshold, and a steep photon index Gamma_VHE = 2.8 +- 0.27_stat +- 0.20_syst are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index Gamma_HE = 2.2 +- 0.04_stat^+0.13_-0.31_sys. The combined gamma-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff (PLC). In the former case, the photon break energy is found at E_br,gamma = 55^+70_-30 GeV, slightly higher than what is usually observed in the HE/VHE gamma-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at E_cut,gamma = 1.4^+1.6_-0.55 (respectively 0.35^+0.75_-0.21) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the gamma-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to n_HW_p ~ 5 x 10^51 ergcm^-3. (EDP Sciences)
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A. Abramowski, F. Aharonian, F. Ait Benkhali, A. Akhperjanian, E. Angüner, et al.. H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud. Astronomy and Astrophysics - A&A, EDP Sciences, 2015, 574, pp.A100. ⟨10.1051/0004-6361/201425070⟩. ⟨hal-02478856⟩

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