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 473c769..13e8c04 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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Blue circles show satellites of the MW and M31, obtained by matching the observed quiescent fractions in Figure~\ref{fig:quiescent_fraction} to rank-ordered infall times of satellites from the ELVIS simulations \citep{Wetzel2015} in 1-dex bins of $\mstar$.  At $\mstar=10^{4-5}\msun$ (light blue), reionization may have quenched some satellites prior to infall.  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 $\mstar=10^{8.5}$, $10^{9.5}\msun$ 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 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.