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