Probing the gamma-ray emission from HESS J1834-087 using H.E.S.S. and Fermi LAT observations
Creators: name: Collaboration, The H. E. S. S.
name: :
name: Abramowski, A.
name: Aharonian, F.
name: Benkhali, F. Ait
name: Akhperjanian, A. G.
name: Angüner, E.
name: Anton, G.
name: Backes, M.
name: Balenderan, S.
name: Balzer, A.
name: Barnacka, A.
name: Becherini, Y.
name: Tjus, J. Becker
name: Bernlöhr, K.
name: Birsin, E.
name: Bissaldi, E.
name: Biteau, J.
name: Böttcher, M.
name: Boisson, C.
name: Bolmont, J.
name: Bordas, P.
name: Brucker, J.
name: Brun, F.
name: Brun, P.
name: Bulik, T.
name: Carrigan, S.
name: Casanova, S.
name: Chadwick, P. M.
name: Chalme-Calvet, R.
name: Chaves, R. C. G.
name: Cheesebrough, A.
name: Chrétien, M.
name: Colafrancesco, S.
name: Cologna, G.
name: Conrad, J.
name: Couturier, C.
name: Cui, Y.
name: Dalton, M.
name: Daniel, M. K.
name: Davids, I. D.
name: Degrange, B.
name: Deil, C.
name: deWilt, P.
name: Dickinson, H. J.
name: Djannati-Ataï, A.
name: Domainko, W.
name: Drury, L. O'C.
name: Dubus, G.
name: Dutson, K.
name: Dyks, J.
name: Dyrda, M.
name: Edwards, T.
name: Egberts, K.
name: Eger, P.
name: Espigat, P.
name: Farnier, C.
name: Fegan, S.
name: Feinstein, F.
name: Fernandes, M. V.
name: Fernandez, D.
name: Fiasson, A.
name: Fontaine, G.
name: Förster, A.
name: Füßling, M.
name: Gajdus, M.
name: Gallant, Y. A.
name: Garrigoux, T.
name: Giavitto, G.
name: Giebels, B.
name: Glicenstein, J. F.
name: Grondin, M. -H.
name: Grudzińska, M.
name: Häffner, S.
name: Hahn, J.
name: Harris, J.
name: Heinzelmann, G.
name: Henri, G.
name: Hermann, G.
name: Hervet, O.
name: Hillert, A.
name: Hinton, J. A.
name: Hofmann, W.
name: Hofverberg, P.
name: Holler, M.
name: Horns, D.
name: Jacholkowska, A.
name: Jahn, C.
name: Jamrozy, M.
name: Janiak, M.
name: Jankowsky, F.
name: Jung, I.
name: Kastendieck, M. A.
name: Katarzyński, K.
name: Katz, U.
name: Kaufmann, S.
name: Khélifi, B.
name: Kieffer, M.
name: Klepser, S.
name: Klochkov, D.
name: Kluźniak, W.
name: Kneiske, T.
name: Kolitzus, D.
name: Komin, Nu.
name: Kosack, K.
name: Krakau, S.
name: Krayzel, F.
name: Krüger, P. P.
name: Laffon, H.
name: Lamanna, G.
name: Lefaucheur, J.
name: Lemière, A.
name: Lemoine-Goumard, M.
name: Lenain, J. -P.
name: Lohse, T.
name: Lopatin, A.
name: Lu, C. -C.
name: Marandon, V.
name: Marcowith, A.
name: Marx, R.
name: Maurin, G.
name: Maxted, N.
name: Mayer, M.
name: McComb, T. J. L.
name: Méhault, J.
name: Meintjes, P. J.
name: Menzler, U.
name: Meyer, M.
name: Moderski, R.
name: Mohamed, M.
name: Moulin, E.
name: Murach, T.
name: Naumann, C. L.
name: de Naurois, M.
name: Niemiec, J.
name: Nolan, S. J.
name: Oakes, L.
name: Odaka, H.
name: Ohm, S.
name: Wilhelmi, E. de Oña
name: Opitz, B.
name: Ostrowski, M.
name: Oya, I.
name: Panter, M.
name: Parsons, R. D.
name: Arribas, M. Paz
name: Pekeur, N. W.
name: Pelletier, G.
name: Perez, J.
name: Petrucci, P. -O.
name: Peyaud, B.
name: Pita, S.
name: Poon, H.
name: Pühlhofer, G.
name: Punch, M.
name: Quirrenbach, A.
name: Raab, S.
name: Raue, M.
name: Reichardt, I.
name: Reimer, A.
name: Reimer, O.
name: Renaud, M.
name: Reyes, R. de los
name: Rieger, F.
name: Rob, L.
name: Romoli, C.
name: Rosier-Lees, S.
name: Rowell, G.
name: Rudak, B.
name: Rulten, C. B.
name: Sahakian, V.
name: Sanchez, D. A.
name: Santangelo, A.
name: Schlickeiser, R.
name: Schüssler, F.
name: Schulz, A.
name: Schwanke, U.
name: Schwarzburg, S.
name: Schwemmer, S.
name: Sol, H.
name: Spengler, G.
name: Spies, F.
name: Stawarz, Ł.
name: Steenkamp, R.
name: Stegmann, C.
name: Stinzing, F.
name: Stycz, K.
name: Sushch, I.
name: Tavernet, J. -P.
name: Tavernier, T.
name: Taylor, A. M.
name: Terrier, R.
name: Tluczykont, M.
name: Trichard, C.
name: Valerius, K.
name: van Eldik, C.
name: van Soelen, B.
name: Vasileiadis, G.
name: Venter, C.
name: Viana, A.
name: Vincent, P.
name: Völk, H. J.
name: Volpe, F.
name: Vorster, M.
name: Vuillaume, T.
name: Wagner, S. J.
name: Wagner, P.
name: Wagner, R. M.
name: Ward, M.
name: Weidinger, M.
name: Weitzel, Q.
name: White, R.
name: Wierzcholska, A.
name: Willmann, P.
name: Wörnlein, A.
name: Wouters, D.
name: Yang, R.
name: Zabalza, V.
name: Zacharias, M.
name: Zdziarski, A. A.
name: Zech, A.
name: Zechlin, H. -S.
name: Collaboration, Fermi-LAT
name: Acero, F.
name: Casandjian, J. M.
name: Cohen-Tanugi, J.
name: Giordano, F.
name: Guillemot, L.
name: Lande, J.
name: Pletsch, H.
name: Uchiyama, Y.
Publisher: name: arXiv
Year: 2014
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Previous observations with HESS have revealed the existence of an extended very-high-energy (VHE; E&gt;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°), 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°) 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.
description: 12 pages, 8 figures, Accepted for publication in Astronomy &amp; Astrophysics