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Humboldt-Universität zu Berlin - Mathematisch-Naturwissen­schaft­liche Fakultät - Experimentelle Elementarteilchenphysik

The H Collaboration (2005)

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

aap, 437:135-139.

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 × 10^33 erg s^-1, and the total energy in corresponding accelerated protons, W^p<1.6 × 10^50 erg are estimated (for proton energies E^p ˜ 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^p ˜ 1 GeV to 3 PeV, assuming a differential particle index -2) gives W^p<6.3 × 10^50 erg. A lower limit on the post-shock magnetic field of B>25 muG results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and gamma-ray upper limits.

Provided by the SAO/NASA Astrophysics Data System