Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/37481
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dc.contributor.author | Aharonian, F. | - |
dc.contributor.author | Akhperjanian, A. | - |
dc.contributor.author | Aye, K. | - |
dc.contributor.author | Bazer-Bachi, A. | - |
dc.contributor.author | Beilicke, M. | - |
dc.contributor.author | Benbow, W. | - |
dc.contributor.author | Berge, D. | - |
dc.contributor.author | Berghaus, P. | - |
dc.contributor.author | Bernlohr, K. | - |
dc.contributor.author | Boisson, C. | - |
dc.contributor.author | Bolz, O. | - |
dc.contributor.author | Borgmeier, C. | - |
dc.contributor.author | Breitling, F. | - |
dc.contributor.author | Brown, A. | - |
dc.contributor.author | Bussons Gordo, J. | - |
dc.contributor.author | Chadwick, P. | - |
dc.contributor.author | Chounet, L. | - |
dc.contributor.author | Cornils, R. | - |
dc.contributor.author | Costamante, L. | - |
dc.contributor.author | Degrange, B. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2005 | - |
dc.identifier.citation | Astronomy and Astrophysics: a European journal, 2005; 437(1):135-139 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.issn | 1432-0746 | - |
dc.identifier.uri | http://hdl.handle.net/2440/37481 | - |
dc.description.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. | - |
dc.description.statementofresponsibility | F. Aharonian ... G. Rowell ... and S. J. Wagner, (et al) | - |
dc.language.iso | en | - |
dc.publisher | E D P Sciences | - |
dc.rights | © The European Southern Observatory 2005 | - |
dc.source.uri | http://dx.doi.org/10.1051/0004-6361:20042522 | - |
dc.title | Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1051/0004-6361:20042522 | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | - |
Appears in Collections: | Aurora harvest Physics publications |
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hdl_37481.pdf | Published version | 373.12 kB | Adobe PDF | View/Open |
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