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We present the analysis of an XMM-Newton observation of the M17 nebula. TheX-ray point source population consists of massive O-type stars and a populationof probable low-mass pre-main sequence stars. CEN1a,b and OI352, the X-raybrightest O-type stars in M17, display hard spectra (kT of 3.8 and 2.6 keV)consistent with a colliding wind origin in binary/multiple systems. We showthat the strong interstellar reddening towards the O-type stars of M17 yieldshuge uncertainties on their Lx/Lbol values. The low-mass pre-main sequencestars exhibit hard spectra resulting from a combination of high plasmatemperatures and very large interstellar absorption. We find evidence forconsiderable long term (months to years) variability of these sources. M17 isone of the few star formation complexes in our Galaxy producing diffuse X-rayemission. We analyze the spectrum of this emission and compare it with previousstudies. Finally, we discuss the Optical Monitor UV data obtainedsimultaneously with the X-ray images. We find very little correspondencebetween the UV and X-ray sources, indicating that the majority of the UVsources are foreground stars, whilst the bulk of the X-ray sources are deeplyembedded in the M17 complex.

An XMM-Newton view of the M17 nebula