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We study the chemical evolution of galaxy clusters by measuring the iron massin the ICM after dissecting the abundance profiles into different components.We use Chandra archival observations of 186 morphologically regular clusters inthe redshift range [0.04, 1.07]. For each cluster we compute the iron abundanceand gas density profiles. We aim at identifying in the iron distribution acentral peak associated with the BCG, and an approximately constant plateauassociated with early enrichment. We are able to firmly identify the twocomponents in a significant fraction of the sample, simply relying on the fitof the abundance profile. We compute the iron mass included in the iron peakand plateau, and the gas mass-weighted iron abundance out to $r_{500}$. Whilethe iron plateau shows no evolution, we find marginal decrease with redshift inthe iron peak. We measure that the fraction of iron peak mass is typically afew percent (~1%) of the total iron mass within $r_{500}$. Therefore, since thetotal iron mass budget is dominated by the plateau, we find consistently thatthe global gas mass-weighted iron abundance does not evolve significantly. Weare also able to reproduce past claims of evolution in the global ironabundance, which turn out to be due to the use of cluster samples withdifferent selection methods combined to the use of emission-weighted instead ofgas mass-weighted abundance values. Finally, while the intrinsic scatter in theiron plateau mass is consistent with zero, the iron peak mass exhibits a largescatter, in line with the fact that the peak is produced after thevirialization of the halo and depends on the formation of the hosting cool coreand the associated feedback processes. We conclude that only aspatially-resolved approach can resolve the issue of the ICM iron evolution,reconciling the contradictory results obtained in the last ten years.

The Chemical Evolution of Galaxy Clusters: Dissecting the Iron Mass Budget of the Intracluster Medium