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The non-thermal supernova remnant RX J1713.7-3946 (G347.3-0.5) has recentlybeen shown to be a site of cosmic ray (CR) electron acceleration to TeVenergies (Muraishi et al. 2000). Here we present evidence that this remnant isalso accelerating CR nuclei. Such nuclei can interact with ambient interstellargas to produce high energy gamma-rays via the decay of neutral pions. Weassociate the unidentified EGRET GeV gamma- ray source 3EG J1714-3857 with amassive (~3*10 5 Mo) and dense (~500 nucleons cm -3) molecular cloudinteracting with RX J1713.7-3946. Direct evidence for such interaction isprovided by observations of the lowest two rotational transitions of CO in thecloud; as in other clear cases of interaction, the CO(J=2-1)/CO(J=1-0) ratio issignificantly enhanced. Since the cloud is of low radio and X-ray brightness,CR electrons cannot be responsible for the bulk of its GeV emission there. Apicture thus emerges where both electrons and nuclei are being accelerated bythe SNR: whereas the CR electrons dominate the local non-thermal radio, X-rayand TeV emission, the shock accelerated CR protons and ions (hadrons) arerevealed through their interactions in the adjacent massive cloud. Such ascenario had been anticipated by Aharonian, Drury and Volk (1994).Comment: 15 pages, 2 low-resolution figures, submitted to ApJL Aug 10, 2001;  this version includes referee's suggestion

Is the Supernova Remnant RX J1713.7−3946 a Hadronic Cosmic-Ray Accelerator?