Comparison between the simulated ICM mass-weighted iron abundance Z_Fe/Z_Fe,⊙ and the L13 prediction based on the stellar-to-gas fraction f_*/f_ICM as in Eq. (5) for the region within R₂₀₀. Left: relation between Z_Fe/Z_Fe,⊙ and f_*/f_ICM for the simulated clusters (black asterisks), compared to the L13 relation (blue solid line). Overplotted two best-fit relations (cyan solid and dot-dashed lines, as in the legend) to the simulation data. Right: iron abundance as a function of simulated gas masses. Two estimates of Z_Fe/Z_Fe,⊙ are compared: the mass-weighted value computed directly from the simulation (“true”; black asterisks) and the value predicted for each simulated cluster given its stellar-to-gas fraction (“L13”; grey triangles). We mark median values in five mass bins for both the true (dashed cyan line) and the L13 (solid blue line) estimate, as well as the respective scatter (shaded areas) between the 16th and the 84th percentile of the distributions.