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With the release of Gaia DR2, it is now possible to measure the propermotions (PMs) of the lowest mass, ultra-faint satellite galaxies in the MilkyWay's (MW) halo for the first time. Many of these faint satellites are positedto have been accreted as satellites of the Magellanic Clouds (MCs). Using their6-dimensional phase space information, we calculate the orbital histories of 13ultra-faint satellites and five classical dwarf spheroidals in a combinedMW+LMC+SMC potential to determine which galaxies are dynamically associatedwith the MCs. These 18 galaxies are separated into four classes: i.) long-termMagellanic satellites that have been bound to the MCs for at least the last twoconsecutive orbits around the MCs (Carina 2, Carina 3, Horologium 1, Hydrus 1);ii.) Magellanic satellites that were recently captured by the MCs $<$ 1 Gyr ago(Reticulum 2, Phoenix 2); iii.) MW satellites that have interacted with the MCs(Sculptor 1, Tucana 3, Segue 1); and iv.) MW satellites (Aquarius 2, CanesVenatici 2, Crater 2, Draco 1, Draco 2, Hydra 2, Carina, Fornax, Ursa Minor).Results are reported for a range of MW and LMC masses. Contrary to previouswork, we find no dynamical association between Carina, Fornax, and the MCs.Finally, we determine that the addition of the SMC's gravitational potentialaffects the longevity of satellites as members of the Magellanic system(long-term versus recently captured), but it does not change the total numberof Magellanic satellites.

The Orbital Histories of Magellanic Satellites Using Gaia DR2 Proper Motions