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Andrew Wetzel edited 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 dependence
in 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}...