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\subsection{Inferred Environmental Quenching Timescales for Satellites}  Our goal is to translate the quiescent fractions in Figure~\ref{fig:quiescent_fraction} into the typical timescales over which satellites are quenched after first falling into a more massive host halo, and we follow the methodology of \citet{Wetzel2013}, used also in \citet{Wheeler2014}. \citet{Wetzel2013}.  First, motivated by the dearth of isolated dwarf galaxies that are quiescent (see above), our models assumes that all satellite dwarf galaxies were actively star-forming prior to first virial infall.  Because ultra-faint dwarfs at $\mstar<10^4\msun$ likely quenched at via cosmic reionization \citep[e.g.,][]{Weisz2014a,Brown2014}, we do not model that mass scale.