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(Abridged) We present an analysis of the X-ray spectrum of the Galacticshell-type supernova remnant (SNR) G347.3-0.5 (RX J1713.7-3946). By performinga joint spectral analysis of data from observations made of G347.3-0.5 usingthe ROSAT PSPC, the ASCA GIS and the RXTE PCA, we have fit the spectra ofparticular regions of this SNR (including the bright northwestern andsouthwestern rims, the northeastern rim and the interior diffuse emission) overthe approximate energy range of 0.5 through 30 keV. Based on the parameters ofthe best fit to the spectra using the SRCUT model, we estimate the maximumenergy of cosmic-ray electrons accelerated by the rims of G347.3-0.5 to be19-25 TeV, assuming a magnetic field strength of 10 microGauss. We present abroadband (radio to gamma-ray) photon energy flux-spectrum for the northwesternrim of the SNR, using a synchrotron-inverse Compton model with a variablemagnetic field strength to fit the spectrum. Our fit derived from this modelyields a maximum energy of only 8.8 TeV for the accelerated cosmic-rayelectrons and a magnetic field strength of 150 microGauss. However, our derivedratio of volumes for TeV emission and X-ray emission (approximately 1000) istoo large to be physically acceptable. We argue that neither non-thermalbremsstrahlung nor neutral pion decay can adequately describe the TeV emissionfrom this rim, and therefore the physical process responsible for this emissionis currently uncertain. Finally, we compare the gross properties of G347.3-0.5with other SNRs known to possess X-ray spectra dominated by non-thermalemission.Comment: 46 pages, 16 figures, accepted for publication in the Astrophysical  Journal (Volume 593, 10 August 2003 Issue

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RXTE,ROSAT, andASCAObservations of G347.3−0.5 (RX J1713.7−3946): Probing Cosmic‐Ray Acceleration by a Galactic Shell‐Type Supernova Remnant