in the size-luminosity plane as ultra-faint dwarf galaxies (M$_{\rm V}$ between -2.0 and -7.8 and half-light radii, $r_h$, between $\sim 18$ and $\sim1000$ pc). It is not clear either which of these dwarfs, if any, have a Magellanic origin.

On that point, @Deason2015 cite a statistical argument based on abundance-matching models applied to massive subhalos in the ELVIS simulations [@Garrison-Kimmel2014] to suggest that $2$-$4$ of the $9$ then known DES candidates might have come into the Milky Way with the LMC. @Yozin2015, on the other hand, conclude, on the basis of orbit models, that the majority of the DES dwarfs could have been at least loosely associated with the Clouds. Yet another analysis suggests, using tailor-made numerical simulations, that only about half of the DES new dwarf galaxies are very likely to have been associated with the LMC in the past [@Jethwa2016] .

Here, we take a complementary and targeted approach, using an LMC analog subhalo identified in a fully cosmological simulation of a Milky Way-sized halo in $\Lambda$CDM. We track the positions and velocities of subhalo particles to constrain the likely location in phase space of systems with prior association with the Clouds. This is an extension of the 