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000193081 0881_ $$aarXiv:1407.0862
000193081 088__ $$2arXiv$$aarXiv:1407.0862
000193081 1001_ $$0P:(DE-HGF)0$$aH.E.S.S. Collaboration$$b0$$eCollaboration author
000193081 245__ $$aProbing the Gamma-Ray Emission from HESS J1834-087 using H.E.S.S. and Fermi LAT Observations
000193081 260__ $$aLes Ulis$$bEDP Sciences$$c2015
000193081 3367_ $$2DRIVER$$aarticle
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000193081 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1480951633_709
000193081 3367_ $$2BibTeX$$aARTICLE
000193081 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000193081 3367_ $$00$$2EndNote$$aJournal Article
000193081 500__ $$aOA
000193081 520__ $$aPrevious 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.
000193081 536__ $$0G:(DE-HGF)POF3-613$$a613 - Matter and Radiation from the Universe (POF3-613)$$cPOF3-613$$fPOF III$$x0
000193081 536__ $$0G:(EU-Grant)259391$$aP-WIND - New light on the gamma-ray sky: unveiling cosmic-ray accelerators in the Milky Way and their relation to pulsar wind nebulae (259391)$$c259391$$fERC-2010-StG_20091028$$x1
000193081 588__ $$aDataset connected to CrossRef, bib-pubdb1.desy.de
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000193081 7001_ $$aFermi-LAT Collaboration$$b221$$eCollaboration author
000193081 7001_ $$aAcero, F.$$b222
000193081 7001_ $$aCasandjian, J. M.$$b223
000193081 7001_ $$aCohen-Tanugi, J.$$b224
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000193081 773__ $$0PERI:(DE-600)1458466-9$$a10.1051/0004-6361/201322694$$gVol. 574, p. A27 -$$n10$$pA27$$tAstronomy and astrophysics$$v574$$x0004-6361$$y2015
000193081 7870_ $$0PUBDB-2014-04510$$aThe H. E. S. S. Collaboration et.al.$$d2014$$iIsParent$$rarXiv:1407.0862$$tProbing the gamma-ray emission from HESS J1834-087 using H.E.S.S. and Fermi LAT observations
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