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Half of the halos are part of a pair that resemble the masses, distance, and relative velocity of the MW-M31 pair, while the other half are single isolated halos.  Given the lack of systematic differences in satellite infall times for the paired versus isolated halos \citep{Wetzel2015}, we use all 48 to improve the statistics.  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}. \citep{Behroozi2013a}.  For each halo, we assign a virial mass, $\mvir$, and radius, $\rvir$, according to \citet{BryanNorman1998}.  A ``subhalo'' is a halo whose center is inside $\rvir$ of a more massive host halo, and a subhalo experiences ``first infall'' and becomes a ``satellite'' when it \emph{first} passes within $\rvir$.  For each subhalo, we compute the peak mass, $\mpeak$, that it ever reached, and 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}.