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The high XMM-Newton throughput allows a detailed investigation of thespatial, spectral and variability properties of the extended and point sourceemission of the starburst galaxy NGC 253 simultaneously. We characterize thebrightest sources by their hardness ratios, detect a bright X-ray transient,and show the spectrum and light curve of the brightest point source, mostlikely a black-hole X-ray binary. The unresolved emission of two disk regionscan be modeled by two thin thermal plasma components of 0.13 and 0.4 keV plusresidual harder emission, with the lower temperature component originating fromabove the disk, the nuclear spectrum by a three temperature plasma (~0.6, 0.9,and 6 keV) with the higher temperatures increasingly absorbed. The hightemperature component most likely originates from the starburst nucleus. Nonon-thermal component, that would point at a significant contribution from anactive nucleus (AGN), is needed. Assuming that type IIa supernova remnants(SNRs) are mostly responsible for the E>4 keV emission, the detection with EPICof the 6.7 keV line allows us to estimate a supernova rate within the nuclearstarburst of 0.2 yr^-1. RGS spectra and EPIC images reveal that thelimb-brightening of the plume is mostly seen in higher ionization emissionlines, while in the lower ionization lines, and below 0.5 keV, the plume ismore homogeneously structured. (abridged)

XMM-Newton observations of NGC 253: Resolving the emission components in the disk and nuclear area