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As the Milky Way and its satellite system become more entrenched in nearfield cosmology efforts, the need for an accurate mass estimate of the MilkyWay's dark matter halo is increasingly critical. With the second and earlythird data releases of stellar proper motions from {\it Gaia}, several groupscalculated full $6$D phase-space information for the population of Milky Waysatellite galaxies. Utilizing these data in comparison to subhalo propertiesdrawn from the Phat ELVIS simulations, we constrain the Milky Way dark matterhalo mass to be $\sim 1-1.2\times10^{12}~\msun$. We find that the kinematics ofsubhalos drawn from more- or less-massive hosts (i.e. $>1.2\times10^{12}~\msun$or $<10^{12}~\msun$) are inconsistent, at the $3\sigma$ confidence level, withthe observed velocities of the Milky Way satellites. The preferred host halomass for the Milky Way is largely insensitive to the exclusion of systemsassociated with the Large Magellanic Cloud, changes in galaxy formationthresholds, and variations in observational completeness. As more Milky Waysatellites are discovered, their velocities (radial, tangential, and total)plus Galactocentric distances will provide further insight into the mass of theMilky Way dark matter halo.

Sizing from the Smallest Scales: The Mass of the Milky Way