The intracluster medium (ICM)—the hot, X-ray-emitting gas filling galaxy clusters—exhibits complex metallicity gradients, with iron and other heavy elements showing spatial distributions that are difficult to reconcile with standard models of supernova enrichment and gas mixing. Observations reveal that metallicity often peaks near the cluster center and declines with radius, but the gradients are shallower and more uniform than expected if metals were simply injected by supernovae and AGN feedback within cluster galaxies (Leccardi & Molendi 2008; Mernier et al. 2017). Additionally, some clusters show remarkably uniform metallicity out to large radii (beyond 500 kpc), suggesting that enrichment occurred very early and was efficiently mixed, yet Lambda-CDM provides no mechanism to distribute metals so uniformly across such vast scales before the cluster assembled. The standard model struggles to explain both the timing of enrichment (metals appear too early and too widespread) and the homogeneity of the distribution, as hierarchical structure formation predicts clumpy, inhomogeneous metal injection from localized stellar populations.