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Several environmental 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 interactions \citep[e.g.,][]{FaroukiShapiro1981} and mergers \citep[e.g.,][]{Deason2014a}, ram-pressure stripping of extended gas \citep[e.g.,][]{Larson1980,McCarthy2008} or of cold inter-stellar medium \citep[e.g.,][]{GunnGott1972,Tonnesen2009}, some of which may be assisted by stellar feedback within the satellite \citep[e.g.,][]{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 might vary across both satellite and host mass scales.  One strong constraint for understanding their relative effects is in determining the timescale of environmental quenching, including its dependence on the mass of both the satellites and the host, as previous works have explored at higher masses \citep[e.g.,][]{Balogh2000,Wetzel2013,Hirschmann2014,Wheeler2014}.