  Our nearest large cosmological neighbour, the Andromeda galaxy (M31), is a
dynamical system, and an accurate measurement of its total mass is central to
our understanding of its assembly history, the life-cycles of its satellite
galaxies, and its role in shaping the Local Group environment. Here, we apply a
novel approach to determine the dynamical mass of M31 using high velocity
Planetary Nebulae (PNe), establishing a hierarchical Bayesian model united with
a scheme to capture potential outliers and marginalize over tracers unknown
distances. With this, we derive the escape velocity run of M31 as a function of
galacto-centric distance, with both parametric and non-parametric approaches.
We determine the escape velocity of M31 to be $470\pm{40}$ km s$^{-1}$ at a
galacto-centric distance of 15 kpc, and also, derive the total potential of
M31, estimating the virial mass and radius of the galaxy to be
$0.8\pm{0.1}\times10^{12}\,M_\odot$ and $240\pm{10}$ kpc, respectively. Our M31
mass is on the low-side of the measured range, this supports the lower expected
mass of the M31-Milky Way system from the timing and momentum arguments,
satisfying the HI constraint on circular velocity between $10\lesssim
R/\textrm{kpc}<35$, and agreeing with the stellar mass Tully-Fisher relation.
To place these results in a broader context, we compare them to the key
predictions of the $\Lambda{\rm CDM}$ cosmological paradigm, including the
stellar-mass-halo-mass and the dark matter halo concentration-virial mass
correlation, and finding it to be an outlier to this relation.
