  Andromeda (And) XXV has previously been reported as a dwarf spheroidal galaxy
(dSph) with little-to-no dark matter. However, the uncertainties on this result
were significant. In this study, we double the number of member stars and
re-derive the kinematics and mass of And XXV. We find that And XXV has a
systemic velocity of $\nu_\mathrm{r}=-107.7\pm1.0 \mathrm{~km s}^{-1}$ and a
velocity dispersion of $\sigma_\nu=4.5\pm1.0\mathrm{~km s}^{-1}$. With this
better constrained velocity dispersion, we derive a mass contained within the
half-light radius of $M(r<
r_\mathrm{h})=6.9^{+3.2}_{-2.8}\times10^6\mathrm{~M}_\odot$. This mass
corresponds to a mass-to-light ratio of
$\mathrm{[M/L]}_\mathrm{r_\mathrm{h}}=37^{+17}_{-15}\mathrm{~M}_\odot/\mathrm{L}_\odot$,
demonstrating, for the first time, that And XXV has an unambiguous dark matter
component. We also measure the metallicity of And XXV to be
$\mathrm{[Fe/H]}=-1.9\pm0.1$$\mathrm{~}$dex, which is in agreement with
previous results. Finally, we extend the analysis of And XXV to include mass
modelling using GravSphere. We find that And XXV has a low central dark matter
density, $\rho_\mathrm{DM}(150\mathrm{pc})=
2.7^{+1.8}_{-1.6}\times10^7\mathrm{~M}_\odot\mathrm{kpc}^{-3}$, making And XXV
a clear outlier when compared to other Local Group (LG) dSphs of the similar
stellar mass. In a companion paper, we will explore whether some combination of
dark matter cusp-core transformations and/or tides can explain And XXV's low
density.
