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So, LMC mass scales represent the transition between these effects.  In other words, there appears to be no quenching mechanism (either internal or external) that operates efficiently for LMC/SMC-mass galaxies.  They are too small for stellar feedback or AGN, but too big (potential too deep) for reionization, gravitational stripping, or ram pressure to remove ISM, and they have too much ISM for strangulation to operate.  See also \citet{Weisz2015}.  This trend with $\mstar$ in Figure~\ref{fig:quench_times} resembles the trend with galaxy $\mstar/\mvir$ (Tollerud et al. 2011a Fig 11 (right panel, Behroozi et al.), which peaks at somewhat higher but similar mass because that's where all the star formation has just happened/is happening.  At the high-mass end, the same stellar feedback that sets the lowering $\mstar/\mvir$ relation with increasing mass also sets the lowering gas fraction with mass that causes more massive satellites to quench more rapidly.