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 c2aa096..67e9a26 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 satellite galaxies across the observable range of stellar mass, $\mstar$.  Top $\mstar$ (top  axis shows the subhalo's subhalo  $\mpeak$ from abundance matching. matching).  Blue circles show times for satellites of the MW and M31, obtained by matching the observed quiescent fractions in Figure~\ref{fig:quiescent_fraction} tothe  virial-infall times of satellites from the ELVIS simulations \citep{Wetzel2015} in 1-dex  bins of $\mstar$. Left panel shows uses  time since first infall into the current MW/M31 MW/M31-like  halos, while right panel shows uses  time since first infall into \emph{any} host halo,thus  including the (potential) possible  effects of group preprocessing. Some satellites at $\mstar<10^5\msun$ At $\mstar=10^{4-5}\msun$  (light blue) blue), some satellite  may have been quenched prior to infall via reionization, so interpret their quenching  timescale with care. Gray triangle shows lower limit for the Large and Small Magellanic Clouds LMC/SMC system  usingtheir  infall time from their its  measured proper motion \citep{Kallivayalil2013}. Red squares showthe  timescale inferred for satellites with $\mstar=10^{8.5}$, $10^{9.5}\msun$ in SDSS \citep{Wheeler2014}, and green curve shows timescales inferred for more massive satellites in groups of $\mvir=10^{12-13}$ in SDSS \citep{Wetzel2013}. The satellite dwarfs in of  the Local Group MW/M31  quenched much more rapidly after infall than more massive satellites, satellites in other hosts,  with theenvironmental quenching  timescale peaking being longest  near Magellanic-Cloud-mass satellites.