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We explore the quenching of low-mass galaxies (10^4 < Mstar < 10^8 Msun) as afunction of lookback time using the star formation histories (SFHs) of 38 LocalGroup dwarf galaxies. The SFHs were derived from analyzing color-magnitudediagrams of resolved stellar populations in archival Hubble SpaceTelescope/Wide Field Planetary Camera 2 imaging. We find: (1) Lower massgalaxies quench earlier than higher mass galaxies; (2) Inside of virial radiusthere is no correlation between a satellite's current proximity to a massivehost and its quenching epoch; (3) There are hints of systematic differences inquenching times of M31 and Milky Way (MW) satellites, although the samplesample size and uncertainties in the SFHs of M31 dwarfs prohibit definitiveconclusions. Combined with literature results, we qualitatively consider theredshift evolution (z=0-1) of the quenched galaxy fraction over ~7 dex instellar mass (10^4 < Mstar < 10^11.5 Msun). The quenched fraction of allgalaxies generally increases toward the present, with both the lowest andhighest mass systems exhibiting the largest quenched fractions at allredshifts. In contrast, galaxies between Mstar ~ 10^8-10^10 Msun have thelowest quenched fractions. We suggest that such intermediate-mass galaxies arethe least efficient at quenching. Finally, we compare our quenching times withpredictions for infall times of low-mass galaxies associated with the MW. Wefind that some of the lowest-mass satellites (e.g., CVn II, Leo IV) may havebeen quenched before infall while higher mass satellites (e.g., Leo I, Fornax)typically quench ~1-4 Gyr after infall.

The Star Formation Histories of Local Group Dwarf Galaxies III. Characterizing Quenching in Low-Mass Galaxies