deletions | additions       diff --git a/abstract.tex b/abstract.tex  index 3a1f033..750cf41 100644  --- a/abstract.tex  +++ b/abstract.tex 
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In the Local Group, almost nearly  all of the  satellite dwarf galaxies ($\mstar < 10 ^ 9 \msun$)  that are within $300 \kpc$ (approximately  the virial radius radius)  of the Milky Way (MW) and M31 exhibit Andromeda (M31) have quiescent star formation and little-to-no cold gas.  This is in  strong contrast to more isolated dwarf galaxies at larger distances, which are almost all actively star-forming and gas-rich.  This near dichotomy implies that  environmental influence. processes within the halos of the MW and M31 \emph{rapidly} removed gas and quenched star formation in such satellites after infall.  We examine combine  the environmental quenching timescales observed quiescent fractions  of satellites of the MW/M31  with $\mstar=10^{4-10} \msun$ using the virial-infall times of satellites in  the ELVIS suite of cosmologicalzoom-in dissipationless  simulations of48  MW/M31-like halos.  Many satellites experienced ``group preprocessing'' halos to infer statistically the timescales over which satellite dwarf galaxies are environmentally quenched.  The quenching timescales at $\mstar<10^8\msun$ are short: $< 2 - 3 \gyr$, depending on whether environmental preprocessing  in another host halo before falling into lower-mass groups is important.  We compare with  the MW/M31 halos.  More... timescales for more massive satellites from the literature, which suggests that environmental quenching timescales are longest ($\approx 9.5 \gyr$) for satellites at $\mstar \approx 10 ^ 9 \msun$ and decrease to $< 5 \gyr$ at $\mstar > 5 \times 10 ^ 9 \msun$.