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Supernova remnants exhibit shock fronts (shells) that can accelerate chargedparticles up to very high energies. In the past decade, measurements of ahandful of shell-type supernova remnants in very-high-energy gamma rays haveprovided unique insights into the acceleration process. Among those objects,RX$~$J1713.7-3946 (also known as G347.3-0.5) has the largest surfacebrightness, allowing us in the past to perform the most comprehensive study ofmorphology and spatially resolved spectra of any such very-high-energygamma-ray source. Here we present extensive new H.E.S.S. measurements ofRX$~$J1713.7-3946, almost doubling the observation time compared to ourprevious publication. Combined with new improved analysis tools, the previoussensitivity is more than doubled. The H.E.S.S. angular resolution of$0.048^\circ$ ($0.036^\circ$ above 2 TeV) is unprecedented in gamma-rayastronomy and probes physical scales of 0.8 (0.6) parsec at the remnant'slocation.  The new H.E.S.S. image of RX$~$J1713.7-3946 allows us to reveal clearmorphological differences between X-rays and gamma rays. In particular, for theouter edge of the brightest shell region, we find the first ever indication forparticles in the process of leaving the acceleration shock region. By studyingthe broadband energy spectrum, we furthermore extract properties of the parentparticle populations, providing new input to the discussion of the leptonic orhadronic nature of the gamma-ray emission mechanism.

astronomy and astrophysics

H.E.S.S. observations of RX J1713.7-3946 with improved angular and  spectral resolution; evidence for gamma-ray emission extending beyond the  X-ray emitting shell