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Astronomy and Astrophysics 437 (2005) 135-139
Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations
F. Aharonian, A. G. Akhperjanian, K.-M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus1, K. Bernlöhr, C. Boisson, O. Bolz, C. Borgmeier, F. Breitling, A. M. Brown, J. Bussons Gordo2, P. M. Chadwick, L.-M. Chounet3, R. Cornils, L. Costamante, B. Degrange3, A. Djannati-Ataï1, L. O'C. Drury, G. Dubus3, T. Ergin, P. Espigat1, F. Feinstein2, P. Fleury3, G. Fontaine3, S. Funk, Y. A. Gallant2, B. Giebels3, S. Gillessen, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, O. C. De Jager, I. Jung, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière1, M. Lemoine3, N. Leroy3, T. Lohse, A. Marcowith, C. Masterson, T. J. L. Mccomb, M. De Naurois4, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif4, M. Panter, G. Pelletier, S. Pita1, G. Pühlhofer, M. Punch1, B. C. Raubenheimer, M. Raue, J. Raux4, S. M. Rayner, I. Redondo3, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland4, G. P. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet4, C.G. Théoret1, M. Tluczykont3, D. J. Van Der Walt, G. Vasileiadis2, P. Vincent4, B. Visser, H. J. Völk, S. J. Wagner
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.
1 :  APC - UMR 7164 - AstroParticule et Cosmologie
2 :  LPTA - Laboratoire de Physique Théorique et Astroparticules
3 :  LLR - Laboratoire Leprince-Ringuet
4 :  LPNHE - Laboratoire de Physique Nucléaire et de Hautes Énergies
Physique/Astrophysique/Cosmologie et astrophysique extra-galactique

Planète et Univers/Astrophysique
gamma rays: observations – ISM: supernova remnants
Lien vers le texte intégral : 
http://fr.arXiv.org/abs/astro-ph/0502239