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Dark matter-dominated cores have long been claimed for the well-studied localgroup dwarf galaxies. More recently, extended stellar halos have been uncoveredaround several of these dwarfs through deeper imaging and spectroscopy. Suchcore-halo structures are not a feature of conventional cold dark matter (CDM),based on collisionless particles where smooth, scale-free profiles arepredicted. In contrast, smooth and prominent dark matter cores are predictedfor Warm and Fuzzy/Wave Dark Matter (WDM/$\psi$DM) respectively. The questionarises to what extent the visible stellar profiles should reflect this darkmatter core structure. Here we compare cosmological hydrodynamical simulationsof CDM, WDM $\&$ $\psi$DM, aiming to predict the stellar profiles for thesethree DM scenarios. We show that cores surrounded by extended halos aredistinguishable for WDM and $\psi$DM, with the most prominent cores in the caseof $\psi$DM, where the stellar density is enhanced in the core due to thepresence of the relatively dense soliton. Our analysis demonstrates that suchbehavior does not appear in CDM, implying that the small-scale cut-off in thepower spectrum present for WDM and $\psi$DM provides a core-halo transition.Consequently, we estimate the mass of the $\psi$DM particle at this core-halotransition point. Furthermore, we observe the anticipated asymmetry for$\psi$DM due to the soliton's random walk, a distinctive characteristic notfound in the symmetric distributions of stars in Warm and CDM models.

Galaxy formation with Wave/Fuzzy Dark Matter: The core-halo structure