1 and 4 $R_{vir}$ of the host. We restrict the sample to the most massive ones, having pre-infall masses around $10^9 M_{\odot}$ and above. Among these we reject 60% that cannot be properly identified and replaced because they are either too elongated (axis ratio less than 0.65, possibly tidally disturbed by companions) or have a substantial fraction of their mass in subhalos. Four objects remain after this rejection procedure, with masses in the range $0.99-4 \times 10^9 M_{\odot}$. Note that at $z \sim 2$ this translates into satellites having masses in the range 80-300 times smaller than the host, which has a virial mass of $3.00 \times 10^{11} M_{\odot}$ and a virial radius of 55.6 kpc at the corresponding epoch (both relatively high since ErisDARK has a fast assembly history with no more major mergers after $z=3$, [@2014ApJ...784..161P]). We remark that the lower end of the satellite-to-host mass ratio is still in a regime in which dynamical friction is effective in eroding the orbital energy over many Gyrs ([@1999ApJ...525..720C]), while this is a negligible effect in published idealized simulations that assume satellites of similar mass but within a host having a fixed mass $\sim 10^{12} M_{\odot}$ ([@2013ApJ...764L..29K]). Finally, we observe 