  The hot intracluster medium (ICM) pervading galaxy clusters and groups is
rich in metals, which were synthesised by billions of supernovae and have
accumulated in cluster gravitational wells for several Gyrs. Since the products
of both Type Ia and core-collapse supernovae - expected to explode over
different time scales - are found in the ICM, constraining accurately the
chemical composition these hot atmospheres can provide invaluable information
on the history of the enrichment of large-scale structures. Recently, Hitomi
observations reported solar abundance ratios in the core of the Perseus
cluster, in tension with previous XMM-Newton measurements obtained for 44
cool-core clusters, groups, and massive ellipticals (the CHEERS sample). In
this work, we revisit the CHEERS results by using an updated version of the
spectral code used to fit the data (SPEXACT v3), the same as was used to obtain
the Hitomi measurements. Despite limitations in the spectral resolution, the
average Cr/Fe and Ni/Fe ratios are now found to be remarkably consistent with
unity and in excellent agreement with the Hitomi results. Our updated
measurements suggest that the solar composition of the ICM of Perseus is a very
common feature in nearby cool-core systems.
