deletions | additions       diff --git a/quenching_time.tex b/quenching_time.tex  index 64df6fa..9035b22 100644  --- a/quenching_time.tex  +++ b/quenching_time.tex 
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Thus, the left panel of Figure~\ref{fig:quench_times} uses time since infall into the MW/M31 halo, ignoring group preprocessing, while the right panel uses time since infall into \emph{any} host halo, including group preprocessing.  The latter necessarily results in longer quenching timescales, though it primarily shifts the upper 16\% of the distribution (error bars).  Both panels show shorter median quenching timescales for less massive satellites: $\sim5\gyr$ at $\mstar=10^{8-9}\msun$, $2-3\gyr$ at $\mstar=10^{7-8}\msun$, and $\lt1.5\gyr$ $<1.5\gyr$  at $\mstar<10^7\msun$, depending on the inclusion of group preprocessing. Moreover, the median timescale for two of the lowest $\mstar$ bins is $0\gyr$ because 100\% of satellites are quiescent there, which implies that quenching must be nearly instantaneous to eliminate all star-forming satellites.  %(modulo uncertainty from the limited number of observed satellites).