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Thus, by this definition, the only star-forming, gas-rich satellites in the LG are: LMC ($\mstar=1.5\times10^9\msun$, $\mgas/\mstar\approx0.3$) and SMC ($\mstar=4.6\times10^8\msun$, $\mgas/\mstar\sim1$) around the MW, and LGS 3 ($\mstar=9.6\times10^5\msun$, $\mgas/\mstar\approx0.4$) and IC 10 ($\mstar=9\times10^7$, $\mgas/\mstar\approx0.6$) around M31.  %(While Sculptor has $\mgas / \mstar \approx 0.096$, we consider it quiescent based on its morphology and lack of recent star formation \citep{Weisz2014a}).  (Dan or Erik - can you say something about comparing these cuts with either SFR metrics or SFHs? Specifically, I am glossing over any ambiguous systems?)  In measuring the fraction of satellites that are quiescent, we group them into 1-dex bins of $\mstar$.  We do not attempt any correction for observational completeness as a function of $\mstar$, because we measure the \emph{relative fraction} that are quiescent in each $\mstar$ bin, which should be unbiased, absent significant differential completeness as a function of recent star formation.  We consider the latter unlikely because star-forming galaxies are generally brighter, but the quiescent fraction is near unity across our range in $\mstar$.  However, we do take into account the maximum observed distance of satellites at each $\mstar$ bin when we compute the virial-infall times using the simulations (see below).