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\subsection{Observed Quiescent Fractions}  Words. 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).