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The large-scale Galactic interstellar radiation field (ISRF) is the result ofstellar emission and dust re-processing of starlight. Where the energy densityof the ISRF is high (e.g., the Galactic Centre), the dominant gamma-rayemission in individual supernova remnants (SNRs), such as G0.9+0.1, may comefrom inverse Compton (IC) scattering of the ISRF. Several models of the ISRFexist. The most recent one, which has been calculated by us, predicts asignificantly higher ISRF than the well-used model of Mathis, Mezger, andPanagia. However,comparison with data is limited to local observations. Basedon our current estimate of the ISRF we predict the gamma-ray emission in theSNRs G0.9+0.1 and RXJ1713, and pair-production absorption features above 20 TeVin 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 toprovide upper bounds on the large-scale ISRF.

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