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The shell-type supernova remnant (SNR) RCW 86, possibly associated with thehistorical supernova SN 185, with its relatively large size (about 40' indiameter) and the presence of non-thermal X-rays is a promising target forgamma-ray observations. The high sensitivity, good angular resolution of a fewarc minutes and the large field of view of the High Energy Stereoscopic System(H.E.S.S.) make it ideally suited for the study of the gamma-ray morphology ofsuch extended sources. H.E.S.S. observations have indeed led to the discoveryof the SNR RCW 86 in very high energy (VHE; E > 100 GeV) gamma-rays. With 31hours of observation time, the source is detected with a statisticalsignificance of 8.5 sigma and is significantly more extended than the H.E.S.S.point spread function. Morphological studies have been performed and show thatthe gamma-ray flux does not correlate perfectly with the X-ray emission. Theflux from the remnant is ~10% of the flux from the Crab nebula, with a similarphoton index of about 2.5. Possible origins of the very high energy gamma-rayemission, via either Inverse Compton scattering by electrons or the decay ofneutral pions produced by proton interactions, are discussed on the basis ofspectral features obtained both in the X-ray and gamma-ray regimes.

Discovery of gamma-ray emission from the shell-type supernova remnant RCW 86 with H.E.S.S