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Observations of low-mass satellite galaxies in the nearby Universe pointtowards a strong dichotomy in their star-forming properties relative to systemswith similar mass in the field. Specifically, satellite galaxies arepreferentially gas poor and no longer forming stars, while their fieldcounterparts are largely gas rich and actively forming stars. Much of therecent work to understand this dichotomy has been statistical in nature,determining not just that environmental processes are most likely responsiblefor quenching these low-mass systems but also that they must operate veryquickly after infall onto the host system, with quenching timescales $\lesssim2~ {\rm Gyr}$ at ${M}_{\star} \lesssim 10^{8}~{\rm M}_{\odot}$. This workutilizes the newly-available $Gaia$ DR2 proper motion measurements along withthe Phat ELVIS suite of high-resolution, cosmological, zoom-in simulations tostudy low-mass satellite quenching around the Milky Way on an object-by-objectbasis. We derive constraints on the infall times for $37$ of the known low-masssatellite galaxies of the Milky Way, finding that $\gtrsim~70\%$ of the`classical' satellites of the Milky Way are consistent with the very shortquenching timescales inferred from the total population in previous works. Theremaining classical Milky Way satellites have quenching timescales noticeablylonger, with $\tau_{\rm quench} \sim 6 - 8~{\rm Gyr}$, highlighting howdetailed orbital modeling is likely necessary to understand the specifics ofenvironmental quenching for individual satellite galaxies. Additionally, wefind that the $6$ ultra-faint dwarf galaxies with publicly available$HST$-based star-formation histories are all consistent with having their starformation shut down prior to infall onto the Milky Way -- which, combined withtheir very early quenching times, strongly favors quenching driven byreionization.

Characterizing the Infall Times and Quenching Timescales of Milky Way Satellites with $Gaia$ Proper Motions