deletions | additions       diff --git a/quenching_time.tex b/quenching_time.tex  index e14cb70..329d40c 100644  --- a/quenching_time.tex  +++ b/quenching_time.tex 
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We show their result for groups with $\mvir=10^{12-13}\msun$, which are most similar to MW/M31 masses.  Altogether, Figure~\ref{fig:quench_times} indicates a complex dependence of the environmental quenching timescale on satellite $\mstar$.  Our results suggest that Specifically,  the typical timescale for satellites in the MW/M31 halos increases with satellite $\mstar$, from $\lesssim1\gyr$ at $\mstar<10^7\msun$ to $\sim5\gyr$ at $\mstar\approx10^{8.5}\msun$. The results of \citet{Wheeler2014} indicate a continuation of this trend, though with a rapid increase ($\sim2\times$) of the timescale to $\approx9.5\gyr$, though interestingly they find no change from $\mstar\approx10^{8.5}$ to $10^{9.5}\msun$.  This rapid increase suggests some tension with our results, specifically, two satellites of M31, NGC 205 and M32 ($\mstar\approx10^{8.5}\msun$), which are quiescent, unless both satellites experienced unusually early infall, or M31 is particularly efficient at quenching its satellites, even compared with more massive hosts.  (\citeauthor{Wheeler2014}'s results are consistent with the star-forming LMC/SMC of the MW.)