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The catalog includes the distance of each dwarf from both the MW and M31, and we define ``satellites'' as those within $300 \kpc$ of either host, motivated by the sharp transition in star formation, gas, and morphological properties within this distance.  $300 \kpc$ also coincides with the median virial radius, $\rvir$, for our simulated MW/M31 halos (see below).  In addition to the data in \citet{McConnachie2012}, we also include the more recent measurements or upper limits of cold atomic gas mass from \citet{Spekkens2014}.  We do not include the recently discovered ultra-faint satellites of the MW from the Dark Energy Survey \citep{Koposov2015, DES2015}, though if they are all quiescent galaxies, their inclusion would not barely  change our results much. results.  The observed dwarf galaxies show a tight correlation between their morphology, star formation, and cold gas content, such that all (?) of the dwarf spheroidals have little-to-no detectable gas or ongoing star formation, and all (?) of the dwarf irregulars have a significant fraction of their baryonic mass in cold gas and ongoing star formation.  Thus, we define ``quiescent'' satellites as those that have $\mgas/\mstar<0.1$ or are classified as having spheroidal morphology if they have no cold gas constraints.