deletions | additions       diff --git a/quenching_time.tex b/quenching_time.tex  index c772daa..16dcb5f 100644  --- a/quenching_time.tex  +++ b/quenching_time.tex 
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Given that both remain star-forming, this places a lower limit to their quenching timescale (gray triangle), consistent with our statistical timescales.  Similarly, measurements of the 3-D orbital velocity and star-formation history for Leo I ($\mstar=5.5\times10^6\msun$) indicate that it fell into the MW halo $\approx2.3\gyr$ ago and quenched $\approx1\gyr$ ago (near its $\approx90\kpc$ pericentric passage), implying a quenching timescale of $\approx1.3\gyr$ \citep[][gray pentagon]{Sohn2013}, again consistent with our results.  The mass trend in Figure~\ref{fig:quench_times} is broadly consistent the star-formation-history-based results of \citep{Weisz2015} \citet{Weisz2015}  that more massive dwarf galaxies in the LG quenched more recently. Also, the overall timescale is broadly consistent with the related analysis of \citet{SlaterBell2014}, who deduced a quenching time since first \emph{pericenter} of $1-2\gyr$, which implies a quenching time since infall of $\sim3Gyr$, though they did not examine mass dependence in detail.  We also compare these timescales with previous studies of more massive satellites of other hosts.