dc.contributor.advisor | Aharonian, F. | |
dc.contributor.author | Büsching, I. | |
dc.contributor.author | De Jager, O.C. | |
dc.contributor.author | Holleran, M. | |
dc.contributor.author | Raubenheimer, B.C. | |
dc.contributor.author | Venter, C. | |
dc.contributor.author | H.E.S.S. Collaboration | |
dc.date.accessioned | 2010-01-18T08:56:18Z | |
dc.date.available | 2010-01-18T08:56:18Z | |
dc.date.issued | 2008 | |
dc.identifier.citation | Aharonian, F. et al. 2008. HESS upper limits for Kepler's supernova remnant. Astronomy & astrophysics, 488(1):219-223. [http://www.aanda.org/] | en |
dc.identifier.issn | 0004-6361 | |
dc.identifier.issn | 1432-0746 (Online) | |
dc.identifier.uri | http://hdl.handle.net/10394/2747 | |
dc.identifier.uri | https://doi.org/10.1051/0004-6361:200809401 | |
dc.identifier.uri | http://www.aanda.org/articles/aa/pdf/2008/34/aa09401-08.pdf | |
dc.description.abstract | Aims. Observations of Kepler's supernova remnant (G4.5+6.8) with the HESS telescope array in 2004 and 2005 with a total live time of 13 h are presented. Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays. Results. No evidence for a very high energy (VHE: >100 GeV) gamma-ray signal from the direction of the remnant is found. An upper limit (99% confidence level) on the energy flux in the range $230~{\rm GeV}{-}12.8~{\rm TeV}$ of 8.6 $\times$ $10^{-13}~{\rm erg}~{\rm cm}^{-2}~{\rm s}^{-1}$ is obtained. Conclusions. In the context of an existing theoretical model for the remnant, the lack of a detectable gamma-ray flux implies a distance of at least $6.4~{\rm kpc}$. A corresponding upper limit for the density of the ambient matter of $0.7~{\rm cm}^{-3}$ is derived. With this distance limit, and assuming a spectral index $\Gamma = 2$, the total energy in accelerated protons is limited to $E_{\rm p} < 8.6$ $\times$ $10^{49}~{\rm erg}$. In the synchrotron/inverse Compton framework, extrapolating the power law measured by RXTE between 10 and $20~{\rm keV}$ down in energy, the predicted gamma-ray flux from inverse Compton scattering is below the measured upper limit for magnetic field values greater than $52~\mu {\rm G}$ | |
dc.language.iso | en | en |
dc.publisher | EDP sciences | en |
dc.subject | gamma rays: observations | |
dc.subject | ISM: supernova remnants | |
dc.subject | ISM: individual objects: Kepler's SNR, SN1604, G4.5+6.8 | |
dc.title | HESS upper limits for Kepler's supernova remnant | en |
dc.type | Article | en |
dc.contributor.researchID | 10859748 - Holleran, Mathew | |
dc.contributor.researchID | 12006653 - Venter, Christo | |
dc.contributor.researchID | 13235176 - Büsching, Ingo | |
dc.contributor.researchID | 10065857 - De Jager, Ocker Cornelis | |
dc.contributor.researchID | 10179240 - Raubenheimer, Barend Christoffel | |