  Using a new long X-ray observation of the cluster of galaxies Sersic 159-03
with XMM-Newton, we derive radial temperature and abundance profiles using
single- and multi-temperature models. The fits to the EPIC and RGS spectra
prefer multi-temperature models especially in the core. The radial profiles of
oxygen and iron measured with EPIC/RGS and the line profiles in RGS suggest
that there is a dip in the O/Fe ratio in the centre of the cluster compared to
its immediate surroundings. A possible explanation for the large scale
metallicity distribution is that SNIa and SNII products are released in the ICM
through ram-pressure stripping of in-falling galaxies. This causes a peaked
metallicity distribution. In addition, SNIa in the central cD galaxy enrich
mainly the centre of the cluster with iron. This excess of SNIa products is
consistent with the low O/Fe ratio we detect in the centre of the cluster. We
fit the abundances we obtain with yields from SNIa, SNII and Population-III
stars to derive the clusters chemical evolution. We find that the measured
abundance pattern does not require a Population-III star contribution. The
relative contribution of the number of SNIa with respect to the total number of
SNe which enrich the ICM is about 25-50%. Furthermore, we discuss the possible
presence of a non-thermal component in the EPIC spectra. A potential source of
this non-thermal emission can be inverse-Compton scattering between Cosmic
Microwave Background (CMB) photons and relativistic electrons, which are
accelerated in bow shocks associated with ram-pressure stripping of in-falling
galaxies.
