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 d5ffbeb..05baf32 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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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 using its infall time from its measured orbital velocity \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 $\mvir=10^{12-13}$ in SDSS \citep{Wetzel2013}.  The satellite dwarf galaxies in the MW/M31 halos were quenched much more rapidly after infall than more massive satellites (in (around  other hosts), with the timescale being longest near Magellanic-Cloud masses.