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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 $z < 9$).  ELVIS contains 48 dark-matter halos of masses similar to the MW or M31 ($\mvir=1.0-2.8\times10^{12}\msun$), with a medianvirial radius of  $\rvir \approx 300 \kpc$. Half of these halos are located in zoom-in regions that were selected to contain a pair of halos that resemble the masses, distance, and relative velocity of the MW-M31 pair, while the other half are single isolated halos matched in masses to the paired ones.  We use allELVIS  halos, given the lack of strong difference in satellite virial-infall times in the paired versus isolated halos \citep{Wetzel2015}. ELVIS identifies dark-matter (sub)halos using the six-dimensional halo finder \textsc{rockstar} \citep{Behroozi2013a} and constructs merger trees using the \textsc{consistent-trees} algorithm \citep{Behroozi2013b}.  For each halo that is not a subhalo, we assign a virial mass, $\mvir$, and radius, $\rvir$, using the evolution of the virial relation from \citet{BryanNorman1998}. 
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When a (sub)halo passes within $\rvir$ of a host halo, the (sub)halo becomes its ``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 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 %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 time distributions to satellites in a 1-dex bin of $\mstar$. As %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 oncomputing  satellite infall virial-infall  times.