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Overall, satellites with $\mstar\sim10^9\msun$ (similar to the Magellanic Clouds) represent the transition between these effects, and no quenching mechanism (either internal or external) appears to operate efficiently near this mass \citep[see also][]{Weisz2015}.  Finally, we note that the above scenario may explain the curious, though qualitative, similarity of Figure~\ref{fig:quench_times} with the mass dependence of the underlying galaxy-halo $\mstar/\mvir$ relation, which is low at both high and low $\mstar$ and peaks at $\mstar\sim10^{10}\msun$ \citep[e.g.,][]{Behroozi2013c}.  In particular, at high $\mstar$, the same physical process(es) that lowers $\mstar/\mvir$ also lowers a galaxy's cold gas fraction, which in turn causes more massive satellites to quench more rapidly.  At low $\mstar$, the same shallower potential wells that allow internal feedback to lower $\mstar/\mvir$ also allows external stripping to occur more easily and quenching to occur more rapidly.  %This analysis represents a statistical approach, but in future work we will combine the measured SFHs with the orbtal phase-space coordinates of each satellites to pursue a similar but more rigorous analysis on a satellite-by-satellite basis.  While preparing this letter, we became aware of Fillingham et al.~2015 (submitted), who also used ELVIS to constrain the quenching timescales of satellites of the MW/M31.