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A sample of 46 nearby clusters observed with Chandra is analyzed to produceradial density, temperature, entropy and metallicity profiles, as well as othermorphological measurements. The entropy profiles are computed to larger radialextents than in previous Chandra cluster sample analyses. We find that the ironmass fraction measured in the inner 0.15 R500 shows a larger dispersion acrossthe sample of low-mass clusters, than it does for the sample of high-massclusters. We interpret this finding as the result of the mixing of more haloesin large clusters than in small clusters, which leads to an averaging of themetal content in the large clusters, and thus less dispersion of metallicityfor high-mass clusters. This interpretation lends support to the idea that thelow-entropy, metal-rich gas of merging haloes reaches clusters' centers, whichexplains observations of Core-Collapse Supernova products metallicity peaks,and which is seen in hydrodynamical simulations. The gas in these merginghaloes would have to reach the centers of clusters without mixing in the outerregions, in order to support our interpretation. On the other hand, metallicitydispersion does not change with mass in the outer regions of clusters,suggesting that most of the outer metals come from a source with a more uniformmetallicity level, such as during pre-enrichment. We also measure a correlationbetween the metal content in low-mass clusters and the degree to which theirIntra-Cluster Medium (ICM) is morphologically disturbed, as measured bycentroid shift. This suggests an alternative interpretation of the large widthof the metallicity distribution in low-mass clusters, whereby a metallicityboost in the center of low-mass clusters is induced as a transitional state,during mergers.

Are the Effects of Structure Formation Seen in the Central Metallicity of Galaxy Clusters?