analysis previously presented in S11, who concluded that [*none*]{} of the $26$ Milky Way satellites known at the time were convincingly associated with the Clouds. The main goal of the present work is to assess the likelihood of association with the Clouds of the recently-discovered dwarfs, as well as to predict the radial velocities and proper motions required for that association to be true.

In § \[sec:sims\] we describe our numerical set up, in § \[sec:results\] we present the main results, including the expected sky distribution of the companion dwarfs, their radial velocities, probability of association with the LMC, as well as their 3D orbits. We conclude with a brief summary of our main conclusions in § \[sec:conc\].

![image](figs/aitoff_r_image_alldwarfs_des2_v3_snp0403){width="0.86\linewidth"}\

Numerical Simulations {#sec:sims}
=====================

We use the Aquarius Project [@Springel2008a], a suite of zoomed-in cosmological simulations that follow the formation of of $6$ Milky Way-sized halos with virial[^1] masses in the range $0.8$-$1.8\; \times 10^{12} M_\odot$. These halos were selected from a large scale simulation of a cosmologically representative volume [the Millennium-II Simulation, see @BoylanKolchin2009]. We focus in this paper on the properties of an “LMC analog” system (hereafter identified as LMCa, for short) which was identified and presented in S11.

