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Elucidating dark matter density profiles in the Galactic dwarf satellites isessential to understanding not only the quintessence of dark matter, but alsothe evolution of the satellites themselves. In this work, we present thecurrent constraints on dark matter densities in the Galactic ultra-faint dwarf(UFD) and diffuse galaxies. Applying our constructed non-spherical mass modelsto the currently available kinematic data of the 25 UFDs and 2 diffusesatellites, we find that whereas most of the galaxies have huge uncertaintieson the inferred dark matter density profiles, Eridanus~II, Segue~I, andWillman~1 favor cuspy central profiles even considering effects of a priorbias. We compare our results with the simulated subhalos on the plane betweenthe dark matter density at 150~pc and the pericenter distance. We find that themost observed satellites and the simulated subhalos are similarly distributedon this plane, except for Antlia~2, Crater~2, and Tucana~3, which are less thanone tenth of the density. Despite considerable tidal effects, the subhalosdetected by commonly-used subhalo finders have difficulty in explaining such ahuge deviation. We also estimate the dynamical mass-to-light ratios of thesatellites and confirm the ratio is linked to stellar mass and metallicity.Tucana~3 deviates largely from these relations, while it follows themass-metallicity relation. This indicates that Tucana~3 has a cored dark matterhalo, despite a significant uncertainty in its ratios.

Dark matter halo properties of the Galactic dwarf satellites:  implication for chemo-dynamical evolution of the satellites and a challenge  to $\Lambda$CDM