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\subsection{Inferred Environmental Quenching Timescales}  The timescale from \citet{Wheeler2014} is based on combining the the galaxy catalog from \citet{Geha2013} \citet{Geha2012}  with satellite virial-infall times in the Millennium II simulation. In particular, \citet{Wheeler2014} used a subset of satellites from \citet{Geha2013} \citet{Geha2012}  at $8.25 < log(\mstar/\msun) < 8.75$ and $9.25 < log(\mstar/\msun) < 9.65$. The \citet{Geha2013} \citet{Geha2012}  sample includes all such satellites around hosts with $\mstar > 2.5 \times 10 ^ {10} \msun$, and as \citet{Wheeler2014} examined using mock catalogs in Millennium II, these satellites span a range of host halo masses $\mvir ~ 10 ^ {12.5 - 14} \msun$. Thus, this corresponds to significantly higher host halo masses than the MW/M31, or in the sample from \citet{Wetzel2013}, which spanned $\mvir = 10 ^ {12 - 13} \msun$.  \citet{Wheeler2014} defined the virial-infall time of a satellite as the first time that it became a satellite, so their definition include group preprocessing, with the caveat that if a satellite orbits beyond its host, as defined by the FoF group, becoming a backsplash/ejected satellite, and then falls back into a host again, they include only the latter infall time.