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https://hdl.handle.net/2440/37481
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Type: | Journal article |
Title: | Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations |
Author: | Aharonian, F. Akhperjanian, A. Aye, K. Bazer-Bachi, A. Beilicke, M. Benbow, W. Berge, D. Berghaus, P. Bernlohr, K. Boisson, C. Bolz, O. Borgmeier, C. Breitling, F. Brown, A. Bussons Gordo, J. Chadwick, P. Chounet, L. Cornils, R. Costamante, L. Degrange, B. et al. |
Citation: | Astronomy and Astrophysics: a European journal, 2005; 437(1):135-139 |
Publisher: | E D P Sciences |
Issue Date: | 2005 |
ISSN: | 0004-6361 1432-0746 |
Statement of Responsibility: | F. Aharonian ... G. Rowell ... and S. J. Wagner, (et al) |
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 γ-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 γ-ray luminosity (for E = 0.26 to 10 TeV, distance d = 2 kpc) of L γ < 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 μG results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and γ-ray upper limits. © ESO 2005. |
Rights: | © The European Southern Observatory 2005 |
DOI: | 10.1051/0004-6361:20042522 |
Published version: | http://dx.doi.org/10.1051/0004-6361:20042522 |
Appears in Collections: | Aurora harvest Physics publications |
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