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Aims: Using XMM-Newton data, we have aimed to study the nuclear outflow ofthe nearby starburst galaxy NGC 253 in X-rays with respect to its morphologyand to spectral variations along the outflow. Methods: We analysed XMM-NewtonRGS spectra, RGS brightness profiles in cross-dispersion direction, narrow bandRGS and EPIC images and EPIC PN brightness profiles of the nuclear region andof the outflow of NGC 253. Results: We detect a diversity of emission linesalong the outflow of NGC 253. This includes the He-like ions of Si, Mg, Ne andO and their corresponding ions in the next higher ionisation state.Additionally transitions from Fe XVII and Fe XVIII are prominent. The derivedtemperatures from line ratios along the outflow range from 0.21+/-0.01 to0.79+/-0.06 keV and the ratio of Fe XVII lines indicates a predominantlycollisionally ionised plasma. Additionally we see indications of a recombiningor underionized plasma in the Fe XVII line ratio. Derived electron densitiesare 0.106+/-0.018 cm^-3 for the nuclear region and 0.025+/-0.003 cm^-3 for theoutflow region closest to the centre. The RGS image in the O VIII line energyclearly shows the morphology of an outflow extending out to ~750 pc along thesouth-east minor axis, while the north-west part of the outflow is not seen inO VIII due to the heavy absorption by the galactic disc. This is the first timethat the hot wind fluid has been detected directly. The limb brightening seenin Chandra and XMM-Newton EPIC observations is only seen in the energy rangecontaining the Fe XVII lines (550-750 eV). In all other energy ranges between400 and 2000 eV no clear evidence of limb brightening could be detected.Comment: 14 pages, 7 figures, 3 tables, accepted for publication on A&A, v2:  typos corrected, electron densities and table with emission line flux added,  discussion improve

High-resolution X-ray spectroscopy and imaging of the nuclear outflow of the starburst galaxy NGC 253