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We aim to study the spatial distribution of the physical and chemicalproperties of the X-ray emitting plasma of the supernova remnant G272.2-3.2, inorder to get important constraints on its ionization stage, on the progenitorsupernova explosion, and the age of the remnant. We report combined XMM-Newtonand Chandra images, median photon energy map, silicon and sulfur equivalentwidth maps, and a spatially resolved spectral analysis for a set of regions ofthe remnant. Complementary radio and H{\alpha} observations, available in theliterature, are also used to study the multi-wavelength connection of alldetected emissions. The X-ray morphology of the remnant displays an overallstructure with an almost circular appearance, a centrally brightened hardregion, with a peculiar elongated hard structure oriented along thenorthwest-southeast direction of the central part. The X-ray spectral study ofthe regions shows distinct K{\alpha} emission-line features of metal elements,confirming the thermal origin of the emission. The X-ray spectra are wellrepresented by an absorbed VNEI thermal plasma model, which produces elevatedabundances of Si, S, and Fe in the circular central region, typical of ejectamaterial. The values of abundances found in the central region of the SNR favora Type Ia progenitor for this remnant. The outer region shows abundances belowthe solar value, as expected if the emission arises from the shocked ISM. Therelatively low ionization timescales suggests non-equilibrium ionization. Weidentify the location of the contact discontinuity. Its distance to the outershock is higher than expected for expansion in a uniform media, what suggeststhat the remnant spent most of its time in a more dense medium.

XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region