HESS J1741−302: a hidden accelerator in the Galactic plane

H. Abdalla A. Abramowski F. Aharonian F.Ait Benkhali E.O. Angüner M. Arakawa C. Armand 1 M. Arrieta 2 M. Backes A. Balzer M. Barnard Y. Becherini J.Becker Tjus D. Berge S. Bernhard K. Bernlöhr R. Blackwell M. Böttcher C. Boisson 2 J. Bolmont 3 S. Bonnefoy P. Bordas J. Bregeon 4 F. Brun 5 P. Brun 6 M. Bryan M. Büchele T. Bulik M. Capasso S. Caroff 7 A. Carosi 1 S. Casanova M. Cerruti 3 N. Chakraborty R.C. G. Chaves 4 A. Chen J. Chevalier 1 S. Colafrancesco B. Condon 5 J. Conrad I.D. Davids J. Decock 6 C. Deil J. Devin 4 P. Dewilt L. Dirson A. Djannati-Ataï 8 A. Donath L.O'C. Drury J. Dyks T. Edwards K. Egberts G. Emery 3 J.P. Ernenwein 9 S. Eschbach C. Farnier S. Fegan 7 M.V. Fernandes A. Fiasson 1 G. Fontaine 7 S. Funk M. Füßling S. Gabici 8 Y.A. Gallant 4 T. Garrigoux F. Gaté 1 G. Giavitto D. Glawion J.F. Glicenstein 6 D. Gottschall M.H. Grondin 5 J. Hahn M. Haupt J. Hawkes G. Heinzelmann G. Henri 10 G. Hermann J.A. Hinton W. Hofmann C. Hoischen T.L. Holch M. Holler D. Horns A. Ivascenko H. Iwasaki A. Jacholkowska 3 M. Jamrozy D. Jankowsky F. Jankowsky M. Jingo L. Jouvin 8 I. Jung-Richardt M.A. Kastendieck K. Katarzyński M. Katsuragawa U. Katz D. Kerszberg 3 D. Khangulyan B. Khélifi 8 J. King S. Klepser D. Klochkov W. Kluźniak Nu. Komin K. Kosack 6 S. Krakau M. Kraus P.P. Krüger H. Laffon 5 G. Lamanna 1 J. Lau J. Lefaucheur 2 A. Lemière 8 M. Lemoine-Goumard 5 J.P. Lenain 3 E. Leser T. Lohse M. Lorentz 6 R. Liu R. López-Coto I. Lypova D. Malyshev V. Marandon A. Marcowith 4 C. Mariaud 7 R. Marx G. Maurin 1 N. Maxted M. Mayer P.J. Meintjes M. Meyer A.M. W. Mitchell R. Moderski M. Mohamed L. Mohrmann K. Morå E. Moulin 6 T. Murach S. Nakashima M. de Naurois 7 H. Ndiyavala F. Niederwanger J. Niemiec L. Oakes P. O'Brien H. Odaka S. Ohm M. Ostrowski I. Oya M. Padovani 4 M. Panter R.D. Parsons N.W. Pekeur G. Pelletier 10 C. Perennes 3 P.O. Petrucci 10 B. Peyaud 6 Q. Piel 1 S. Pita 8 V. Poireau 1 D.A. Prokhorov H. Prokoph G. Pühlhofer M. Punch 8 A. Quirrenbach S. Raab R. Rauth A. Reimer O. Reimer M. Renaud 4 R. de los Reyes F. Rieger L. Rinchiuso 6 C. Romoli G. Rowell B. Rudak C.B. Rulten 2 V. Sahakian S. Saito D.A. Sanchez 1 A. Santangelo M. Sasaki R. Schlickeiser F. Schüssler 6 A. Schulz U. Schwanke S. Schwemmer M. Seglar-Arroyo 6 A.S. Seyffert N. Shafi I. Shilon K. Shiningayamwe R. Simoni H. Sol 2 F. Spanier M. Spir-Jacob 8 Ł. Stawarz R. Steenkamp C. Stegmann C. Steppa I. Sushch T. Takahashi J.P. Tavernet 3 T. Tavernier 6 A.M. Taylor R. Terrier 8 L. Tibaldo D. Tiziani M. Tluczykont C. Trichard 9 M. Tsirou 4 N. Tsuji R. Tuffs Y. Uchiyama D.J. van der Walt C. van Eldik C. van Rensburg B. van Soelen G. Vasileiadis 4 J. Veh C. Venter A. Viana P. Vincent 3 J. Vink F. Voisin H.J. Völk T. Vuillaume 1 Z. Wadiasingh S.J. Wagner P. Wagner R.M. Wagner R. White A. Wierzcholska P. Willmann A. Wörnlein D. Wouters 6 R. Yang D. Zaborov 7 M. Zacharias R. Zanin A.A. Zdziarski A. Zech 2 F. Zefi 7 A. Ziegler J. Zorn N. Żywucka R. Enokiya Y. Fukui T. Hayakawa T. Okuda K. Torii H. Yamamoto
Abstract : The H.E.S.S. Collaboration has discovered a new very high energy (VHE, E > 0.1 TeV) γ-ray source, HESS J1741−302, located in the Galactic plane. Despite several attempts to constrain its nature, no plausible counterpart has been found so far at X-ray and MeV/GeV γ-ray energies, and the source remains unidentified. An analysis of 145-h of observations of HESS J1741−302 at VHEs has revealed a steady and relatively weak TeV source (~1% of the Crab Nebula flux), with a spectral index of Γ = 2.3 ± 0.2stat ± 0.2sys, extending to energies up to 10 TeV without any clear signature of a cut-off. In a hadronic scenario, such a spectrum implies an object with particle acceleration up to energies of several hundred TeV. Contrary to most H.E.S.S. unidentified sources, the angular size of HESS J1741−302 is compatible with the H.E.S.S. point spread function at VHEs, with an extension constrained to be below 0.068° at a 99% confidence level. The γ-ray emission detected by H.E.S.S. can be explained both within a hadronic scenario, due to collisions of protons with energies of hundreds of TeV with dense molecular clouds, and in a leptonic scenario, as a relic pulsar wind nebula, possibly powered by the middle-aged (20 kyr) pulsar PSR B1737−30. A binary scenario, related to the compact radio source 1LC 358.266+0.038 found to be spatially coincident with the best fit position of HESS J1741−302, is also envisaged.Key words: gamma rays: ISM / gamma rays: general / cosmic rays / ISM: clouds★★ Wallenberg Academy Fellow.
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H. Abdalla, A. Abramowski, F. Aharonian, F.Ait Benkhali, E.O. Angüner, et al.. HESS J1741−302: a hidden accelerator in the Galactic plane. Astron.Astrophys., 2018, 612, pp.A13. ⟨10.1051/0004-6361/201730581⟩. ⟨hal-01797468⟩

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