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\section{Introduction}  The standard picture of the evolution of substructure in the Universe involves the collapse of dark matter into halos, which may host luminous galaxy. Such halos may exist within the bounds of larger halos; in these cases the galaxies they may host are thought of as satellite galaxies, and their evolution differs substantially from galaxies that are not satellites in ways not fully understood. The spatial and kinematic distributions of such galaxies can inform our ideas of how satellites and the systems in which they are found evolve. Substantial evidence exists that satellite galaxies are not isotropically distributed around their hosts \cite{Bailin_2008}, nor are their velocities isotropic \cite{Faltenbacher_2010}. This is also something seen in simulations \cite{Zentner_2005}. \cite{VDB99,Zentner_2005}.  Local group satellites are highly anisotropically distributed both around the Milky Way and M31. The disk-like arrangement of MW satellites was first pointed out by \citet{Lynden-Bell74}. Later studies argued further for the existence of a disk-like structure of Milky Way satellites, and noted that the arrangement of the satellites strongly favors the Northern Hemisphere. Around M31, dramatic evidence has been found for a disk of satellites, many of which exhibit coherent rotation along the line of sight\cite{Ibata_2013}. The M31 structure seems particularly difficult to square with our picture of galaxy evolution; \cite{Ibata_2014} argues that \cite{Ibata_2014} that alignments similar to the one found around M31 are essentially non-existant in numerical simulations.