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 7f69207..2e778c4 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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Environmental quenching timescales 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 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 reionization  may havebeen  quenched some satellites  prior to infall via reionization, so interpret with care. 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, including possible effects of group preprocessing.  Gray triangle shows lower limit for the LMC/SMC systemusing its infall time  from its measured orbital velocity 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 $\mvir=10^{12-13}$ in SDSS \citep{Wetzel2013}.  The satellitedwarf  galaxies in the MW/M31 haloswere  quenched much more rapidly after infall than more massive satellites (around other hosts), with the timescale being longest near Magellanic-Cloud masses.