A&A 437, 135-139 (2005)
DOI: 10.1051/0004-6361:20042522

Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations

F. Aharonian¹, A. G. Akhperjanian², K.-M. Aye³, A. R. Bazer-Bachi⁴, M. Beilicke⁵, W. Benbow¹, D. Berge¹, P. Berghaus⁶, K. Bernlöhr^{1, 7}, C. Boisson⁸, O. Bolz¹, C. Borgmeier⁷, F. Breitling⁷, A. M. Brown³, J. Bussons Gordo⁹, P. M. Chadwick³, L.-M. Chounet¹⁰, R. Cornils⁵, L. Costamante^{1, 11}, B. Degrange¹⁰, A. Djannati-Ataï⁶, L. O'C. Drury¹², G. Dubus¹⁰, T. Ergin⁷, P. Espigat⁶, F. Feinstein⁹, P. Fleury¹⁰, G. Fontaine¹⁰, S. Funk¹, Y. A. Gallant⁹, B. Giebels¹⁰, S. Gillessen¹, P. Goret¹³, C. Hadjichristidis³, M. Hauser¹⁴, G. Heinzelmann⁵, G. Henri¹⁵, G. Hermann¹, J. A. Hinton¹, W. Hofmann¹, M. Holleran¹⁶, D. Horns¹, O. C. de Jager¹⁶, I. Jung^{1, 14}, B. Khélifi¹, Nu. Komin⁷, A. Konopelko^{1, 7}, I. J. Latham³, R. Le Gallou³, A. Lemière⁶, M. Lemoine¹⁰, N. Leroy¹⁰, T. Lohse⁷, A. Marcowith⁴, C. Masterson^{1, 11}, T. J. L. McComb³, M. de Naurois¹⁷, S. J. Nolan³, A. Noutsos³, K. J. Orford³, J. L. Osborne³, M. Ouchrif^{17, 11}, M. Panter¹, G. Pelletier¹⁵, S. Pita⁶, G. Pühlhofer^{1, 14}, M. Punch⁶, B. C. Raubenheimer¹⁶, M. Raue⁵, J. Raux¹⁷, S. M. Rayner³, I. Redondo^{10, 11}, A. Reimer¹⁸, O. Reimer¹⁸, J. Ripken⁵, L. Rob¹⁹, L. Rolland¹⁷, G. P. Rowell¹, V. Sahakian², L. Saugé¹⁵, S. Schlenker⁷, R. Schlickeiser¹⁸, C. Schuster¹⁸, U. Schwanke⁷, M. Siewert¹⁸, H. Sol⁸, R. Steenkamp²⁰, C. Stegmann⁷, J.-P. Tavernet¹⁷, C. G. Théoret⁶, M. Tluczykont^{10, 11}, D. J. van der Walt¹⁶, G. Vasileiadis⁹, P. Vincent¹⁷, B. Visser¹⁶, H. J. Völk¹ and S. J. Wagner<sup>14

1</sup>  Max-Planck-Institut für Kernphysik,
    e-mail: [Conor.Masterson;Gavin.Rowell]@mpi-hd.mpg.de
²  Yerevan Physics Institute,
³  University of Durham,
⁴  Centre d'Étude Spatiale des Rayonnements,
⁵  Universität Hamburg, Institut für Experimentalphysik,
⁶  Physique Corpusculaire et Cosmologie, IN2P3/CNRS, Collège de France,
⁷  Institut für Physik, Humboldt-Universität zu Berlin,
⁸  LUTH, UMR 8102 du CNRS, Observatoire de Paris,
⁹  Groupe d'Astroparticules de Montpellier,
¹⁰  Laboratoire Leprince-Ringuet, École Polytechnique
¹¹  European Associated Laboratory for Gamma-Ray Astronomy, jointly supported by CNRS and MPG
¹²  Dublin Institute for Advanced Studies
¹³  Service d'Astrophysique, DAPNIA/DSM/CEA, CE Saclay,
¹⁴  Landessternwarte, Königstuhl,
¹⁵  Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier,
¹⁶  Unit for Space Physics, North-West University,
¹⁷  Laboratoire de Physique Nucléaire et de Hautes Énergies, IN2P3/CNRS, Universités Paris VI & VII,
¹⁸  Institut für Theoretische Physik, Ruhr-Universität Bochum,
¹⁹  Institute of Particle and Nuclear Physics, Charles University,
²⁰  University of Namibia,

(Received 11 December 2004 / Accepted 4 February 2005 )

Abstract
Observations of the shell-type supernova remnant SN1006 have been carried out with the HESS system of Cherenkov telescopes during 2003 (18.2 h with two operating telescopes) and 2004 (6.3 h with all four telescopes). No evidence for TeV -ray emission from any compact or extended region associated with the remnant is seen and resulting upper limits at the 99.9% confidence level are up to a factor 10 lower than previously-published fluxes from CANGAROO. For SN1006 at its current epoch of evolution we define limits for a number of important global parameters. Upper limits on the -ray luminosity (for E = 0.26 to 10 TeV, distance d = 2 kpc) of   10³³ erg s^-1, and the total energy in corresponding accelerated protons,   10⁵⁰ erg are estimated (for proton energies to 60 TeV and assuming the lowest value n=0.05 cm^-3 of the ambient target density discussed in literature). Extending this estimate to cover the range of proton energies observed in the cosmic ray spectrum up to the knee (we take here 1 GeV to 3 PeV, assuming a differential particle index -2) gives   10⁵⁰ erg. A lower limit on the post-shock magnetic field of G results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and -ray upper limits.

Key words: gamma rays: observations -- ISM: supernova remnants

SIMBAD Objects in preparation

© ESO 2005

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