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

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

doi:10.1051/0004-6361/201322694

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

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Pletsch, H.
Pulsar Observation and Data Analysis, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Citation

Abramowski, A., Aharonian, F., Benkhali, F. A., Akhperjanian, A. G., Angüner, E., Anton, G., et al. (2015). Probing the gamma-ray emission from HESS J1834-087 using H.E.S.S. and Fermi LAT observations. Astronomy and Astrophysics, 574: A27. doi:10.1051/0004-6361/201322694.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0025-BFBB-2

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.