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 0f3c29b..c2aa096 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 galaxiesversus stellar mass, $\mstar$,  across the observable range. range of stellar mass, $\mstar$.  Top axis shows thesatellite  subhalo's $\mpeak$ based on from  abundance matching. Blue circles show times for satellites of the Milky Way (MW) MW  and M31, obtained by matching the observed quiescent fractions in Figure~\ref{fig:quiescent_fraction} to the virial-infall times of satellites from the ELVIS simulations \citep{Wetzel2015} in bins of $\mstar$. Left panel shows time since first infall into the current MW/M31 halos, while right panel shows time since first infall into \emph{any} host halo, that is, thus  including the (potential) effects of group preprocessing. Satellites Some satellites  at $\mstar < 10 ^ 5 \msun$ $\mstar<10^5\msun$  (light blue) may have been quenched prior tovirial  infall via reionization, so interpret  their timescaleshould be interpreted  with care. Gray triangle shows lower limit for the Large and Small Magellanic Clouds using their virial-infall infall  time from their measured proper motion \citep{Kallivayalil2013}. Red squares show the timescale inferred for satellites with $\mstar = 10 ^ {8.5 - 9.5} \msun$ around MW-like hosts $\mstar=10^{8.5}$, $10^{9.5}\msun$  in SDSS \citep{Wheeler2014}, and green curve show shows  timescales inferred for more massive satellites in groups of $\mvir = 10 ^ {12 - 13}$ from $\mvir=10^{12-13}$ in  SDSS \citep{Wetzel2013}. The satellites satellite dwarfs  in the Local Group quenched much more rapidly after falling into the MW/M31 halo infall  than more massive satellites around other hosts. satellites, with the environmental quenching timescale peaking near Magellanic-Cloud-mass satellites.