deletions | additions       diff --git a/figures/qu.time_v_m.star_sat.first.t/caption.tex b/figures/qu.time_v_m.star_sat.first.t/caption.tex  index 13e8c04..97958de 100644  --- a/figures/qu.time_v_m.star_sat.first.t/caption.tex  +++ b/figures/qu.time_v_m.star_sat.first.t/caption.tex 
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Error bars come from the 68\% uncertainty in observed quiescent fractions in Figure~\ref{fig:quiescent_fraction}.  Left panel uses time since first infall into the current MW/M31-like halo, while right panel uses time since first infall into \emph{any} host halo, thereby including possible effects of group preprocessing.  Gray triangle shows lower limit for the LMC/SMC system from its measured orbit \citep{Kallivayalil2013}, and gray pentagon shows the quenching timescale for Leo I from its measured orbit and star-formation history \citep{Sohn2013}.  Red squares show times inferred for satellites with $\mstar=10^{8.5}$, $10^{9.5}\msun$ around hosts with $\mstar>2.5\times10^{10}\msun$  in SDSS \citep{Wheeler2014}, and green curve shows the same for more massive satellites in groups of $\mvir=10^{12-13}\msun$ in SDSS \citep{Wetzel2013}. The satellite galaxies satellites  in the MW/M31 halos quenchedmuch  more rapidly after infall than more massive satellites (around other hosts), with hosts).  Overall,  the quenching  timescale being increases with $\mstar$, is  longest near at $\mstar\sim10^9\msun$ (near  Magellanic-Cloud masses. masses), then decreases with further increasing $\mstar$.