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Stellar rotation periods are valuable both for constraining models of angularmomentum loss and for under- standing how magnetic features impact inferencesof exoplanet parameters. Building on our previous work in the northernhemisphere, we have used long-term, ground-based photometric monitoring fromthe MEarth Observatory to measure 234 rotation periods for nearby, southernhemisphere M dwarfs. Notable examples include the exoplanet hosts GJ 1132, LHS1140, and Proxima Centauri. We find excellent agreement between our data and K2photometry for the overlapping subset. Amongst the sample of stars with thehighest quality datasets, we recover periods in 66%; as the length of thedataset increases, our recovery rate approaches 100%. The longest rotationperiods we detect are around 140 days, which we suggest represent the periodsthat are reached when M dwarfs are as old as the local thick disk (about 9Gyr).

New rotation period measurements for M dwarfs in the southern hemisphere: an abundance of slowly rotating, fully convective stars