  New mass estimates and cumulative mass profiles with Bayesian credible
regions (c.r.) for the Milky Way (MW) are found using the Galactic Mass
Estimator (GME) code and dwarf galaxy (DG) kinematic data from multiple
sources. GME takes a hierarchical Bayesian approach to simultaneously estimate
the true positions and velocities of the DGs, their velocity anisotropy, and
the model parameters for the Galaxy's total gravitational potential. In this
study, we incorporate meaningful prior information from past studies and
simulations. The prior distributions for the physical model are informed by the
results of Eadie & Juric (2019), which used globular clusters instead of DGs,
as well as by the subhalo distributions of the Ananke Gaia-like surveys from
Feedback In Realistic Environments-2 (Fire-2) cosmological simulations (see
Sanderson et al. 2020). Using DGs beyond 45 kpc, we report median and 95% c.r
estimates for $r_{200}$ = 212.8 (191.12,238.44) kpc, and for the total enclosed
mass $M_{200}$ = 1.19 (0.87,1.68)$\times10^{12}M_{\odot}$ (adopting
$\Delta_c=200$). Median mass estimates at specific radii are also reported
(e.g., $M(<50\text{ kpc})=0.52\times10^{12}M_{\odot}$ and $M(100\text{
kpc})=0.78\times10^{12}M_{\odot}$). Estimates are comparable to other recent
studies using GAIA DR2 and DGs, but notably different from the estimates of
Eadie & Juric (2019). We perform a sensitivity analysis to investigate whether
individual DGs and/or a more massive Large Magellanic Cloud (LMC) on the order
of $10^{11}M_{\odot}$ may be affecting our mass estimates. We find possible
supporting evidence for the idea that some DGs are affected by a massive LMC
and are not in equilibrium with the MW.
