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The supernova remnant (SNR) W51C is a Galactic object located in a stronglyinhomogeneous interstellar medium with signs of an interaction of the SNR blastwave with dense molecular gas. Diffuse X-ray emission from the interior of theSNR can reveal element abundances in the different emission regions and shedlight on the type of supernova (SN) explosion and its progenitor. The hardX-ray emission helps to identify possible candidates for a pulsar formed in theSN explosion and for its pulsar wind nebula (PWN). We have analysed X-ray dataobtained with XMM-Newton. Spectral analyses in selected regions were performed.Ejecta emission in the bright western part of the SNR, located next to acomplex of dense molecular gas, was confirmed. The Ne and Mg abundances suggesta massive progenitor with a mass of > 20 M_sun. Two extended regions emittinghard X-rays were identified (corresponding to the known sources [KLS2002] HX3west and CXO J192318.5+140305 discovered with ASCA and Chandra, respectively),each of which has an additional point source inside and shows a power-lawspectrum with Gamma ~ 1.8. Based on their X-ray emission, both sources can beclassified as PWN candidates.

XMM-Newton observation of the Galactic supernova remnant W51C (G49.1-0.1)