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Fig. 8.

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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. This pattern holds across all DM models, with a slight offset observed for ψDM. The small panels offer a logarithmic scale representation of the figure, providing additional insights. The vertical black line indicates 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 Spearman correlation is negative, indicating that metal-poor stars are generally older than their metal-rich counterparts (Emami et al. 2022). Notably, “WDM” and ψDM exhibit a similar stellar history, while CDM displays a more discrete profile. These visualizations offer valuable insights into the relationships between stellar properties, including distance, metallicity, and age, within the context of different DM models.

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