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 2e778c4..d090f0c 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, including possible effects of group preprocessing.  Gray triangle shows lower limit for the LMC/SMC system from its measured orbit \citep{Kallivayalil2013}.  Red squares show times inferred for satellites with $\mstar=10^{8.5}$, $10^{9.5}\msun$ in SDSS \citep{Wheeler2014}, and green curve shows the same for more massive satellites in groups of $\mvir=10^{12-13}$ $\mvir=10^{12-13}\msun$  in SDSS \citep{Wetzel2013}. The satellite galaxies in the MW/M31 halos quenched much more rapidly after infall than more massive satellites (around other hosts), with the timescale being longest near Magellanic-Cloud masses.