Left panel: 2D correlation of the stellar distance vs. stellar metallicity. It is evident that metal-rich stars tend to be located closer to the galactic center. However, there is a notable offset for “WDM”_G3, suggesting a unique distribution pattern for this specific galaxy. The small subpanels provide a logarithmic scale representation for enhanced visualization. The vertical black line signifies the comoving limit, while the dashed line represents the ideal size of a core-halo structure. Right panel: 2D correlation of stellar age vs. metallicity. The negative Spearman correlation coefficient indicates that older stars are more likely to be metal-poor, while younger stars tend to be more metal-rich. This relationship holds across all DM models.