Predicted images and spectra of gamma rays and X-rays from shell supernovaremnants

Hard X-ray and gamma-ray emission is expected from supernova remnants due t o synchrotron radiation, nonthermal bremsstrahlung, decay of neutral pions produced by cosmic ray protons and ions colliding with thermal gas, and inv erse-Compton emission from relativistic electrons upscattering cosmic micro wave background photons. The question of the maximum energy to which partic les can be accelerated by shocks is of great astrophysical interest, and th e identification of hard X-ray synchrotron radiation gives direct evidence for electrons of energies of order 100 TeV and higher. Bard X-rays can also be produced by bremsstrahlung from nonrelativistic but superthermal electr ons that form the low-energy end of the accelerated-particle spectrum. Dete ction of remnants in TeV gamma rays requires the presence of 100 TeV electr ons. Another discriminant is possible with spectra and images in hard X-ray s. The IBIS imager on INTEGRAL will be able to localize X-ray emission well enough to distinguish synchrotron and nonthermal radiation in the remnant of SN 1006 between 15 and 50 keV. I exhibit model images and spectra of syn chrotron radiation and nonthermal bremsstrahlung for a variety of model par ameters.