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Probing the gamma-ray emission from HESS J1834-087 using H.E.S.S. and Fermi LAT observations

A. Abramowski F. Aharonian F. Ait Benkhali A. G. Akhperjanian E. Angüner G. Anton M. Backes S. Balenderan Agnès Balzer A. Barnacka Y. Becherini J. Becker Tjus K. Bernlöhr E. Birsin E. Bissaldi J. Biteau 1 M. Böttcher C. Boisson 2 J. Bolmont 3 P. Bordas J. Brucker F. Brun P. Brun 4 T. Bulik S. Carrigan S. Casanova P. M. Chadwick R. Chalme-Calvet 3 R. C. G. Chaves A. Cheesebrough M. Chrétien 3 S. Colafrancesco G. Cologna J. Conrad C. Couturier 3 Y. Cui M. Dalton 5 M. K. Daniel I. D. Davids B. Degrange 1 C. Deil P. Dewilt H. J. Dickinson A. Djannati-Ataï 6 W. Domainko L. O'C. Drury G. Dubus K. Dutson J. Dyks M. Dyrda T. Edwards K. Egberts P. Eger P. Espigat 7 C. Farnier S. Fegan 1 F. Feinstein 8 M. V. Fernandes D. Fernandez 8 A. Fiasson 9 G. Fontaine 1 A. Förster M. Füßling M. Gajdus Y. A. Gallant 8 T. Garrigoux 3 G. Giavitto B. Giebels 1 J. F. Glicenstein M. -H. Grondin M. Grudzińska S. Häffner J. Hahn J. Harris G. Heinzelmann G. Henri G. Hermann O. Hervet 2 A. Hillert J. A. Hinton W. Hofmann P. Hofverberg M. Holler D. Horns A. Jacholkowska 3 C. Jahn M. Jamrozy M. Janiak F. Jankowsky I. Jung M. A. Kastendieck K. Katarzyński U. Katz S. Kaufmann B. Khélifi 7 Michel Kieffer 3 S. Klepser D. Klochkov W. Kluźniak T. Kneiske D. Kolitzus Nu. Komin 9 K. Kosack S. Krakau F. Krayzel 9 P. P. Krüger H. Laffon 5 G. Lamanna 9 J. Lefaucheur 7 A. Lemière 7 M. Lemoine-Goumard 5 J. -P. Lenain 3 T. Lohse A. Lopatin C. -C. Lu V. Marandon A. Marcowith 8 R. Marx G. Maurin 9 N. Maxted M. Mayer T. J. L. Mccomb J. Méhault 5 P. J. Meintjes U. Menzler M. Meyer R. Moderski M. Mohamed Emmanuel Moulin T. Murach C. L. Naumann 3 M. de Naurois 1 J. Niemiec S. J. Nolan L. Oakes H. Odaka S. Ohm E. de Oña Wilhelmi B. Opitz M. Ostrowski I. Oya M. Panter R. D. Parsons M. Paz Arribas N. W. Pekeur G. Pelletier J. Perez P. -O. Petrucci B. Peyaud S. Pita 7 H. Poon G. Pühlhofer M. Punch 7 A. Quirrenbach S. Raab M. Raue I. Reichardt 7 A. Reimer O. Reimer M. Renaud 8 R. de Los Reyes F. Rieger L. Rob C. Romoli S. Rosier-Lees 9 G. Rowell B. Rudak C. B. Rulten 2 V. Sahakian D. A. Sanchez 9 A. Santangelo R. Schlickeiser F. Schüssler A. Schulz U. Schwanke S. Schwarzburg S. Schwemmer H. Sol 2 G. Spengler F. Spies Ł. Stawarz R. Steenkamp C. Stegmann F. Stinzing K. Stycz I. Sushch J. -P. Tavernet 3 T. Tavernier 7 A. M. Taylor R. Terrier 7 M. Tluczykont C. Trichard 9 K. Valerius C. van Eldik B. van Soelen G. Vasileiadis 8 C. Venter A. Viana P. Vincent 3 H. J. Völk F. Volpe M. Vorster T. Vuillaume S. J. Wagner P. Wagner R. M. Wagner M. Ward M. Weidinger Q. Weitzel R. White A. Wierzcholska P. Willmann A. Wörnlein D. Wouters R. Yang V. Zabalza M. Zacharias A. A. Zdziarski A. Zech 2 H. -S. Zechlin Fermi-Lat Collaboration Fabio Acero J. M. Casandjian J. Cohen-Tanugi 8 F. Giordano Lucas Guillemot 10 J. Lande H. Pletsch Y. Uchiyama
Abstract : Previous observations with HESS have revealed the existence of an extended very-high-energy (VHE; E>100 GeV) gamma-ray source, HESS J1834-087, coincident with the SNR W41. The origin of the gamma-ray emission has been further investigated with HESS and the Fermi-LAT. The gamma-ray data provided by 61h (HESS) and 4 yrs (Fermi LAT) of observations cover over 5 decades in energy (1.8GeV - 30TeV). The morphology and spectrum of the TeV and GeV sources have been studied and multi-wavelength data have been used to investigate the origin of the observed emission. The TeV source can be modeled with a sum of two components: one point-like and one significantly extended (sig_TeV = 0.17{\deg}), both centered on SNR W41 and exhibiting spectra described by a power law of index 2.6. The GeV source detected with Fermi is extended (sig_GeV =0.15{\deg}) and morphologically matches the VHE emission. Its spectrum can be described by a power-law with index 2.15 and joins smoothly the one of the whole TeV source. A break appears in the spectra around 100 GeV. Two main scenarios are proposed to explain the emission: a pulsar wind nebula (PWN) or the interaction of SNR W41 with a molecular cloud. X-ray observations suggest the presence of a point-like source (pulsar candidate) near the center of the SNR and non-thermal X-ray diffuse emission which could arise from a potential PWN. The PWN scenario is supported by the match of of the TeV and GeV positions with the putative pulsar. However, the overall spectrum is reproduced by a 1-zone leptonic model only if an excess of low-energy electrons is injected by a high spin-down power pulsar. This low-energy component is not needed if the point-like TeV source is unrelated to the extended GeV and TeV sources. The interacting SNR scenario is supported by the spatial coincidence between the gamma-ray sources, the detection of OH maser lines and the hadronic modeling.
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A. Abramowski, F. Aharonian, F. Ait Benkhali, A. G. Akhperjanian, E. Angüner, et al.. Probing the gamma-ray emission from HESS J1834-087 using H.E.S.S. and Fermi LAT observations. Astronomy and Astrophysics - A&A, EDP Sciences, 2015, 574, pp.A27. ⟨10.1051/0004-6361/201322694⟩. ⟨in2p3-01025854⟩

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