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Moreover, for dwarf galaxies, the same internal stellar feedback that regulates their low star-formation efficiency likely heats/drives significant cold gas to large radii on short timescales \citep[e.g.,][]{Muratov2015}, which would assist any such environmental stripping, making it even more efficient.  Thus, the rapid environmental quenching timescales for dwarf galaxies may arise from the non-linear interplay of both internal feedback and external stripping \citep[e.g.,][]{NicholsBlandHawthorn2011, BaheMcCarthy2015}.  Overall, satellites with $\mstar\sim10^9\msun$ (similar to the Magellanic Clouds) represent the transition between these effects, gas consumption and gas stripping,  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.