AHARONIAN, F.; AKHPERJANIAN, A.G.; BARRES DE ALMEIDA, U.; BAZER-BACHI, A.R.; BEHERA, B.; BEILICKE, M.; BENBOW, W.; BERGE, D.; BERNL¨OHR, K.; BOISSON, C.; BOLZ, O.; BORREL, V.; BRAUN, I.; BRION, E.; BRUCKER, J.; B¨UHLER, R.; BULIK, T.; B¨USCHING, I.; BOUTELIER, T.; CARRIGAN, S.; CHADWICK, P.M.; CHOUNET, L.-M.; CLAPSON, A.C.; COIGNET, G.; CORNILS, R.; COSTAMANTE, L.; DALTON, M.; DEGRANGE, B.; DICKINSON, H.J.; DJANNATI-ATAÏ, A.; DOMAINKO, W.; DRURY, L.O'C.; DUBOIS, F.; DUBUS, G.; DYKS, J.; EGBERTS, K.; EMMANOULOPOULOS, D.; ESPIGAT, P.; FARNIER, C.; FEINSTEIN, F.; FIASSON, A.; FÖRSTER, A.; FONTAINE, G.; FÜSSLING, M.; GALLANT, Y.A.; GIEBELS, B.; GLICENSTEIN, J.F.; GLÜCK, B.; GORET, P.; HADJICHRISTIDIS, C.; HAUSER, D.; HAUSER, M.; HEINZELMANN, G.; HENRI, G.; HERMANN, G.; HINTON, J.A.; HOFFMANN, A.; HOFMANN, W.; HOLLERAN, M.; HOPPE, S.; HORNS, D.; JACHOLKOWSKA, A.; DE JAGER, O.C.; JUNG, I.; KATARZYNSKI, K.; KENDZIORRA, E.; KERSCHHAGGL, M.; KHÉLIFI, B.; KEOGH, D.; KOMIN, Nu.; KOSACK, K.; LAMANNA, G.; LATHAM, I.J.; LEMOINE-GOUMARD, M.; LENAIN, J.-P.; LOHSE, T.; MARTIN, J.M.; MARTINEAU-HUYNH, O.; MARCOWITH, A.; MASTERSON, C.; MAURIN, D.; MCCOMB, T.J.L.; MODERSKI, R.; MOULIN, Emmanuel; NAUMANN-GODO, M.; DE NAUROIS, M.; NEDBAL, D.; NEKRASSOV, D.; NOLAN, S.J.; OHM, S.; OLIVE, J.-P.; DE ONA WILHELMI, E.; ORFORD, K.J.; OSBORNE, J.L.; OSTROWSKI, M.; PANTER, M.; PEDALETTI, G.; PELLETIER, G.; PETRUCCI, P.-O.; PITA, S.; PÜHLHOFER, G.; PUNCH, M.; QUIRRENBACH, A.; RAUBENHEIMER, B.C.; RAUE, M.; RAYNER, S.M.; RENAUD, M.; RIPKEN, J.; ROB, L.; ROSIER-LEES, S.; ROWELL, G.; RUDAK, B.; RUPPEL, J.; SAHAKIAN, V.; SANTANGELO, A.; SCHLICKEISER, R.; SCHÖCK, F.M.; SCHRÖDER, R.; SCHWANKE, U.; SCHWARZBURG, S.; SCHWEMMER, S.; SHALCHI, A.; SOL, H.; SPANGLER, D.; STAWARZ, &#321.; STEENKAMP, R.; STEGMANN, C.; SUPERINA, G.; TAM, P.H.; TAVERNET, J.-P.; TERRIER, R.; VAN ELDIK, C.; VASILEIADIS, G.; VENTER, C.; VIALLE, J.P.; VINCENT, P.; VIVIER, M.; VÖLK, H.J.; VOLPE, F.; WAGNER, S.J.; WARD, M.; ZDZIARSKI, A.A.; ZECH, A.

doi:10.1051/0004-6361:200809401

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AHARONIAN, F.

AKHPERJANIAN, A.G.

BARRES DE ALMEIDA, U.

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Astronomy and Astrophysics - A&A. 2008, vol. 488, p. 219-223

EDP Sciences

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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.< Réduire

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SN1604

G4.5+6.8)

gamma rays: observations

ISM: supernova remnants

ISM: individual objects: (Kepler's SNR

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