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H.E.S.S. upper limits for Kepler's supernova remnant

F. Aharonian A.G. Akhperjanian U. Barres de Almeida A.R. Bazer-Bachi 1 B. Behera M. Beilicke W. Benbow D. Berge K. Bernl¨ohr C. Boisson 2 O. Bolz V. Borrel 1 I. Braun E. Brion 3 J. Brucker R. B¨uhler T. Bulik I. B¨usching T. Boutelier 4 S. Carrigan P.M. Chadwick L.-M. Chounet 5 A.C. Clapson G. Coignet 6 R. Cornils L. Costamante M. Dalton B. Degrange 5 H.J. Dickinson A. Djannati-Ataï 7 W. Domainko L.O'C. Drury F. Dubois 6 G. Dubus 4 J. Dyks K. Egberts D. Emmanoulopoulos P. Espigat 8 C. Farnier 9 F. Feinstein 9 A. Fiasson 9 A. Förster G. Fontaine 5 M. Füßling Y.A. Gallant 9 B. Giebels 5 J.F. Glicenstein 3 B. Glück P. Goret 3 C. Hadjichristidis D. Hauser M. Hauser G. Heinzelmann G. Henri 4 G. Hermann J.A. Hinton A. Hoffmann W. Hofmann M. Holleran S. Hoppe D. Horns A. Jacholkowska 9 O.C. de Jager I. Jung K. Katarzynski E. Kendziorra M. Kerschhaggl B. Khélifi 5 D. Keogh Nu. Komin 9 K. Kosack G. Lamanna 6 I.J. Latham M. Lemoine-Goumard 5, 10 J.-P. Lenain 2 T. Lohse J.M. Martin 2 O. Martineau-Huynh 11 A. Marcowith 9 C. Masterson D. Maurin 11 T.J.L. Mccomb R. Moderski Emmanuel Moulin 3 M. Naumann-Godo 5 M. de Naurois 11 D. Nedbal D. Nekrassov S.J. Nolan S. Ohm J.-P. Olive 1 E. de Ona Wilhelmi 8 K.J. Orford J.L. Osborne M. Ostrowski M. Panter G. Pedaletti G. Pelletier 4 P.-O. Petrucci 4 S. Pita 8 G. Pühlhofer M. Punch 8 A. Quirrenbach B.C. Raubenheimer M. Raue S.M. Rayner M. Renaud J. Ripken L. Rob S. Rosier-Lees 6 G. Rowell B. Rudak J. Ruppel V. Sahakian A. Santangelo R. Schlickeiser F.M. Schöck R. Schröder U. Schwanke S. Schwarzburg S. Schwemmer A. Shalchi H. Sol 2 D. Spangler Ł. Stawarz R. Steenkamp C. Stegmann G. Superina 5 P.H. Tam J.-P. Tavernet 11 R. Terrier 8 C. van Eldik G. Vasileiadis 9 C. Venter J.P. Vialle 6 P. Vincent 11 M. Vivier 3 H.J. Völk F. Volpe 5 S.J. Wagner M. Ward A.A. Zdziarski A. Zech 2
Abstract : Observations of Kepler's supernova remnant (G4.5+6.8) with the H.E.S.S. telescope array in 2004 and 2005 with a total live time of 13 h are presented. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays. No evidence for a very high energy (VHE: >100 GeV) gamma-ray signal from the direction of the remnant is found. An upper limit (99% confidence level) on the energy flux in the range 230 GeV - 12.8 TeV of 8.6 x 10^{-13} erg cm^{-2} s^{-1} is obtained. In the context of an existing theoretical model for the remnant, the lack of a detectable gamma-ray flux implies a distance of at least 6.4 kpc. A corresponding upper limit for the density of the ambient matter of 0.7 cm^{-3} is derived. With this distance limit, and assuming a spectral index Gamma = 2, the total energy in accelerated protons is limited to E_p < 8.6 x 10^{49} erg. In the synchrotron/inverse Compton framework, extrapolating the power law measured by RXTE between 10 and 20 keV down in energy, the predicted gamma-ray flux from inverse Compton scattering is below the measured upper limit for magnetic field values greater than 52 muG.
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F. Aharonian, A.G. Akhperjanian, U. Barres de Almeida, A.R. Bazer-Bachi, B. Behera, et al.. H.E.S.S. upper limits for Kepler's supernova remnant. Astronomy and Astrophysics - A&A, EDP Sciences, 2008, 488, pp.219-223. ⟨10.1051/0004-6361:200809401⟩. ⟨in2p3-00289653⟩