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\subsection{Simulations}  To measure the virial-infall infall  times of satellites in a cosmological context, we use ELVIS (Exploring the Local Volume in Simulations), a suite of cosmological zoom-in $N$-body simulations that are targeted to modeling the LG \citep{GarrisonKimmel2014}. ELVIS was run using \textsc{GADGET-3} and \textsc{GADGET-2} \citep{Springel2005e}, with initial conditions generated using \textsc{MUSIC} \citep{HahnAbel2011}, all with $\Lambda$CDM cosmology based on WMAP7 \citep{Larson2011}: $\sigma_8=0.801$, $\omegamatter=0.266$, $\omegalambda=0.734$, $n_s=0.963$ and $h=0.71$.  Within the zoom-in regions, the particle mass is $1.9\times10^5\msun$ and the Plummer-equivalent force softening is $140\pc$ (comoving at $z>9$, physical at $z<9$). 
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A ``subhalo'' is a halo whose center is inside $\rvir$ of a (more massive) host halo, and when a (sub)halo passes within $\rvir$, it becomes a ``satellite'' and experiences ``virial infall''.  For each (sub)halo, we compute the peak mass, $\mpeak$, that it reached along the history of its primary progenitor.  In order to match subhalos to observed satellites, we assign $\mstar$ to subhalos based on their $\mpeak$ using the relation from abundance matching in \citet{GarrisonKimmel2014}, which reproduces the observed mass function at $\mstar<10^9\msun$ in the LG if one accounts for observational incompleteness \citep{Tollerud2008, Hargis2014}.  %While the relation between $\mstar$ and subhalo $\mpeak$ for dwarf galaxies remains highly uncertain, likely with significant scatter, in this work the relation is important \emph{only} in assigning virial-infall infall  time distributions to satellites in a 1-dex bin of $\mstar$. %As \citet{Wetzel2015} showed, satellite infall times generally change by $<10-20\%$ over $\sim 1$ dex in $\mstar$.  See \citet{GarrisonKimmel2014} for more details on ELVIS, and \citet{Wetzel2015} for more details on satellite virial-infall infall  times.