deletions | additions       diff --git a/quenching_time.tex b/quenching_time.tex  index 6074bbf..2cacbf9 100644  --- a/quenching_time.tex  +++ b/quenching_time.tex 
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Similarly, the green curves in Figure~\ref{fig:quench_times} show the quenching timescales for more massive satellites from \citet{Wetzel2013}, who also used identical methodology, combining galaxy groups from SDSS \citep{Tinker2011, Wetzel2012} with satellite infall times (including group preprocessing) measured in mock group catalogs in their cosmological simulation.  We show their result for groups with $\mvir=10^{12-13}\msun$, which are most similar to MW/M31 masses.  Combining our results with these works suggests indicates  a complex dependence of environmental quenching timescales on satellite $\mstar$. Specifically, our Our  results alone suggest that the typical  quenching timescale for satellites  in the MW/M31 halos increases increase  with satellite mass, from $\lesssim1\gyr$ at $\mstar<10^7\msun$ to $\sim5\gyr$ at $\mstar\approx10^{8.5}\msun$. However, the The  results of \citet{Wheeler2014} imply indicate a continuation of this trend, though with  a doubling \emph{rapid} increase ($\sim2\times$)  of the timescale to $\approx9.5\gyr$ at just higher $\mstar$, $\approx9.5\gyr$,  though the interestingly they  find no dependencein their sample  from $\mstar\approx10^{8.5}$ to $10^{9.5}\msun$. This rapid increase  suggests some tension with the satellite NGC 205 and M32, two satellites  of M31 with $\mstar\approx10^{8.5}\msun$ that are quiescent, unless both satellites experienced unusually early infall (the results are consistent with  the MW/M31. star-forming LMC and SMC.)  Finally, the results of \citet{Wetzel2013}...