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 13dfedb..d5ffbeb 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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\label{fig:quench_times}  Environmental quenching timescales of for  satellite galaxies across the observable range of stellar mass, $\mstar$ (top axis shows subhalo $\mpeak$ from abundance matching). 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  virial-infall times of satellites from the ELVIS simulations \citep{Wetzel2015} in 1-dex bins of $\mstar$. At $\mstar=10^{4-5}\msun$ (light blue), some satellite may have been quenched prior to infall via reionization, so interpret with care.  Error bars are derived come  from the 68\% uncertainty inthe  observed quiescent fractions in Figure~\ref{fig:quiescent_fraction}. Left panel uses time since first infall into the current MW/M31 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 proper motion 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 dwarfs of dwarf galaxies in  the MW/M31 halos were  quenched much more rapidly after infall than more massive satellites in (in  other hosts, hosts),  with the timescale being longest near Magellanic-Cloud-masses. Magellanic-Cloud masses.