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Thus, the MW and M31 halos show the strongest signal of environmental influence over their satellites of any known systems, and the LG is a compelling laboratory for studying environmental processes on galaxies.  Several such processes within a host halo can regulate the gas content, star formation, morphology, and eventual disruption of satellite galaxies, including gravitational tidal forces \citep[e.g.,][]{Dekel2003}, galaxy-galaxy tidal interactions \citep[e.g.,][]{FaroukiShapiro1981}, galaxy-galaxy mergers \citep[e.g.,][]{Deason2014a}, and ram-pressure stripping of extended gas \citep[e.g.,][]{Larson1980, McCarthy2008} or cold inter-stellar medium \citep[e.g.,][]{GunnGott1972, Tonnesen2009}, some of which may be assisted by stellar feedback within the satellite \citep[e.g.,][]{NicholsBlandHawthorn2011,BaheMcCarthy2015}.  %tidal shocking and resonant interactions with the host \citep[e.g.,][]{Mayer2001,DOnghia2010},   The key astrophysical challenge is understanding the relative importance of these processes, including which (if any) dominate, and how they vary across both satellite and host masses.  One strong constraint for understanding the relative effects of environmental processes is determining the timescale over which environmental quenching occurs, as previous works have explored at higher masses \citep[e.g.,][]{Balogh2000, Wetzel2013, Hirschmann2014, Wheeler2014}.