deletions | additions       diff --git a/quenching_time.tex b/quenching_time.tex  index 329d40c..89b1f56 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 $\mstar$.  Specifically, the typical timescale for satellites in the MW/M31 halos increases withsatellite  $\mstar$, 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 that  this trend, mass dependence continues,  though with a rapid increase ($\sim2\times$)of the timescale  to $\approx9.5\gyr$, though interestingly they find and  no change from $\mstar\approx10^{8.5}$ to $10^{9.5}\msun$. This rapid increase suggests implies  some tension with our results, specifically, the  two satellites of M31, NGC 205 and M32 ($\mstar\approx10^{8.5}\msun$),which are quiescent,  unless either (1)  bothsatellites  experienced unusually early infall, infall $>9.5\gyr$ ago,  or (2)  M31 is particularly efficient at quenching quenches  its satellites, satellites particularly rapidly,  even compared with more the  massive hosts.  (\citeauthor{Wheeler2014}'s hosts in \citet{Wheeler2014}.  %(\citeauthor{Wheeler2014}'s  results are consistent with the star-forming LMC/SMC of the MW.) Finally,the results of  \citet{Wetzel2013} indicates indicate  that the quenching timescale rapidly \emph{decreases} by $\mstar=5\times10^9\msun$ at $\mstar>5\times10^9\msun$  and continues to decline with increasing $\mstar$. Thus, Overall,  the typical  environmental quenching timescales are shortest for the lowest-mass satellites, satellites  andthe timescale  is longer longest  for satellites near with $\mstar\sim10^9\msun$ (roughly  Magellanic-Cloud masses. mass).