{ "id": "0704.1703", "version": "v1", "published": "2007-04-13T15:30:50.000Z", "updated": "2007-04-13T15:30:50.000Z", "title": "Very High Energy Gamma Rays from Supernova Remnants and Constraints on the Galactic Interstellar Radiation Field", "authors": [ "T. A. Porter", "I. V. Moskalenko", "A. W. Strong" ], "comment": "To appear in the proceedings of the 1st GLAST Symposium", "journal": "AIPConf.Proc.921:411-412,2007", "doi": "10.1063/1.2757377", "categories": [ "astro-ph" ], "abstract": "The 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.", "revisions": [ { "version": "v1", "updated": "2007-04-13T15:30:50.000Z" } ], "analyses": { "subjects": [ "98.70.Rz", "98.38.Mz" ], "keywords": [ "high energy gamma rays", "supernova remnants", "large-scale galactic interstellar radiation field", "gamma-ray emission" ], "tags": [ "journal article" ], "publication": { "publisher": "AIP", "journal": "AIP Conf. Proc." }, "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable", "inspire": 748545, "adsabs": "2007AIPC..921..411P" } } }