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The supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) ispart of the class of remnants dominated by synchrotron emission in X-rays. Itis also one of the few shell-type SNRs observed at TeV energies allowing toinvestigate particle acceleration at SNRs shock.  Our goal is to compare spatial and spectral properties of the remnant in X-and gamma-rays to understand the nature of the TeV emission. This requires tostudy the remnant at the same spatial scale at both energies. To complement thenon-thermal spectrum of the remnant, we attempt to provide a reliable estimatefor the radio flux density. In radio, we revisited ATCA data and used HI andmid-infrared observations to disentangle the thermal from the non-thermalemission. In X-rays, we produced a new mosaic of the remnant and degraded thespatial resolution of the X-ray data to the resolution of the HESS instrumentto perform spatially resolved spectroscopy at the same spatial scale in X- andgamma-rays. Radial profiles were obtained to investigate the extension of theemission at both energies.  We found that part of the radio emission within the SNR contours is thermalin nature. Taking this into account, we provide new lower and upper limits forthe integrated synchrotron flux of the remnant at 1.4 GHz of 22 Jy and 26 Jyrespectively. In X-rays, we obtained the first full coverage of RX J1713.7-3946with XMM-Newton. The spatial variation of the photon index seen at small scalein X-rays is smeared out at HESS resolution. A non-linear correlation betweenthe X- and gamma-ray fluxes of the type Fx \propto Fg^2.41 is found.

A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946