deletions | additions       diff --git a/quenching_time.tex b/quenching_time.tex  index 9a47302..3cab6eb 100644  --- a/quenching_time.tex  +++ b/quenching_time.tex 
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We now translate the quiescent fractions in Figure~\ref{fig:quiescent_fraction} into the typical timescales over which environmental processes quench satellites after they fall into a host halo, following the methodology of \citet{Wetzel2013}.  First, motivated by the dearth of \emph{isolated} galaxies with $\mstar<10^9\msun$ that are quiescent (see Introduction), our model assumes that all satellite dwarfs satellites with $\mstar(z=0)<10^9\msun$  were actively star-forming prior to first infall. However, because many galaxies with $\mstar(z=0)<10^4\msun$ may have been quenched at high redshift by cosmic reionization \citep[e.g.,][]{Weisz2014a,Brown2014}, we do not model those masses.  At $\mstar(z=0)=10^{4-5}\msun$, satellites' star-formation histories show a mix of complete quenching by $z\gtrsim3$ (e.g., Bootes I, Leo IV) and signs of star formation at $z\lesssim1$ (e.g., And XI, And XII, And XVI) \citep{Weisz2014a,Weisz2014c,Brown2014}, so quenching at these masses may arise from a mix of reionization and the host-halo environment.  %Leo T had recent star formation, suggesting that galaxies at least down to logM_star ~ 5 can form stars today if not for environment.