Very High Energy Gamma Rays from Supernova Remnants and Constraints on the Galactic Interstellar Radiation Field

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dc.creatorPorter, T. A.
dc.creatorMoskalenko, I. V.
dc.creatorStrong, A. W.
dc.date2007-04-13
dc.date.accessioned2026-07-07T10:59:33Z
dc.date.available2026-07-07T10:59:33Z
dc.descriptionThe large-scale Galactic interstellar radiation field (ISRF) is the result of stellar emission and dust re-processing of starlight. Where the energy density of the ISRF is high (e.g., the Galactic Centre), the dominant gamma-ray emission in individual supernova remnants (SNRs), such as G0.9+0.1, may come from inverse Compton (IC) scattering of the ISRF. Several models of the ISRF exist. The most recent one, which has been calculated by us, predicts a significantly higher ISRF than the well-used model of Mathis, Mezger, and Panagia. However,comparison with data is limited to local observations. Based on our current estimate of the ISRF we predict the gamma-ray emission in the SNRs G0.9+0.1 and RXJ1713, and pair-production absorption features above 20 TeV in the spectra of G0.9+0.1, J1713-381, and J1634-472. We discuss how GLAST, along with current and future very high energy instruments, may be able to provide upper bounds on the large-scale ISRF.
dc.descriptionTo appear in the proceedings of the 1st GLAST Symposium
dc.identifierhttps://arxiv.org/abs/0704.1703
dc.identifierhttp://arxiv.org/abs/0704.1703
dc.identifierAIPConf.Proc.921:411-412,2007
dc.identifierdoi:10.1063/1.2757377
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/187439
dc.subjectAstrophysics
dc.titleVery High Energy Gamma Rays from Supernova Remnants and Constraints on the Galactic Interstellar Radiation Field
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