but kinematic data are needed to substantiate that possibility. Conclusive evidence for association would require proper motions to constrain the orbital angular momentum direction, which, for true Magellanic satellites, must coincide with that of the Clouds. We use this result to predict radial velocities and proper motions for all new dwarfs. Our results are relatively insensitive to the assumption of first or second pericenter for the Clouds.'
author:
- |
    \
    \
    $^{1}$ Department of Physics and Astronomy, University of California Riverside, 900 University Ave., CA92507, US\
    $^{2}$ Senior CIfAR Fellow. Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada\
    $^{3}$ Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA\
    $^{4}$ Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK\
bibliography:
- 'master.bib'
title: Identifying true satellites of the Magellanic Clouds
---

galaxies: haloes - galaxies: formation - galaxies: evolution - galaxies: kinematics and dynamics.

Introduction {#sec:intro}
============

The Large and Small Magellanic Clouds (LMC and SMC, respectively) are a galaxy pair orbiting together in the halo of the Milky Way and provide a prime example of the nested hierarchy of structures expected in the $\Lambda$CDM galaxy formation 