  Dark matter-dominated cores have long been claimed for the well-studied local
group dwarf galaxies. More recently, extended stellar halos have been uncovered
around several of these dwarfs through deeper imaging and spectroscopy. Such
core-halo structures are not a feature of conventional cold dark matter (CDM),
based on collisionless particles where smooth, scale-free profiles are
predicted. In contrast, smooth and prominent dark matter cores are predicted
for Warm and Fuzzy/Wave Dark Matter (WDM/$\psi$DM) respectively. The question
arises to what extent the visible stellar profiles should reflect this dark
matter core structure. Here we compare cosmological hydrodynamical simulations
of CDM, WDM $\&$ $\psi$DM, aiming to predict the stellar profiles for these
three DM scenarios. We show that cores surrounded by extended halos are
distinguishable for WDM and $\psi$DM, with the most prominent cores in the case
of $\psi$DM, where the stellar density is enhanced in the core due to the
presence of the relatively dense soliton. Our analysis demonstrates that such
behavior does not appear in CDM, implying that the small-scale cut-off in the
power 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-halo
transition point. Furthermore, we observe the anticipated asymmetry for
$\psi$DM due to the soliton's random walk, a distinctive characteristic not
found in the symmetric distributions of stars in Warm and CDM models.
