62 articles – 637 Notices  [english version]
 HAL : in2p3-00024436, version 1
 arXiv : astro-ph/0502239
 Astronomy and Astrophysics 437 (2005) 135-139
 Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations
 HESS Collaboration(s)
 (2005)
 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 $\gamma$-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 $\gamma$-ray luminosity (for E = 0.26 to 10 TeV, distance d = 2 kpc) of $L_\gamma < 1.7$ $\times$ 1033 erg s-1, and the total energy in corresponding accelerated protons, $W_{\rm p}<1.6$ $\times$ 1050 erg are estimated (for proton energies $E_{\rm p} \sim 1.5$ 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 $E_{\rm p} \sim$ 1 GeV to 3 PeV, assuming a differential particle index -2) gives $W_{\rm p}<6.3$ $\times$ 1050 erg. A lower limit on the post-shock magnetic field of $B>25~\mu$G results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and $\gamma$-ray upper limits.
 Thème(s) : Physique/Astrophysique/Cosmologie et astrophysique extra-galactiquePlanète et Univers/Astrophysique
 Mot(s)-clé(s) : gamma rays: observations – ISM: supernova remnants
 Lien vers le texte intégral : http://fr.arXiv.org/abs/astro-ph/0502239
 in2p3-00024436, version 1 http://hal.in2p3.fr/in2p3-00024436 oai:hal.in2p3.fr:in2p3-00024436 Contributeur : Dominique Girod <> Soumis le : Lundi 30 Octobre 2006, 20:42:32 Dernière modification le : Lundi 30 Octobre 2006, 20:58:33