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Stellar rotation periods measured from single-age populations are criticalfor investigating how stellar angular momentum content evolves over time, howthat evolution depends on mass, and how rotation influences the stellar dynamoand the magnetically heated chromosphere and corona. We report rotation periodsfor 40 late-K to mid-M stars members of the nearby, rich, intermediate-age(~600 Myr) open cluster Praesepe. These rotation periods were derived from ~200observations taken by the Palomar Transient Factory of four cluster fields from2010 February to May. Our measurements indicate that Praesepe's mass-periodrelation transitions from a well-defined singular relation to a more scattereddistribution of both fast and slow rotators at ~0.6 Msun. The location of thistransition is broadly consistent with expectations based on observations ofyounger clusters and the assumption that stellar-spin down is the dominantmechanism influencing angular momentum evolution at 600 Myr. However, acomparison to data recently published for the Hyades, assumed to be coeval toPraesepe, indicates that the divergence from a singular mass-period relationoccurs at different characteristic masses, strengthening the finding thatPraesepe is the younger of the two clusters. We also use previously publishedrelations describing the evolution of rotation periods as a function of colorand mass to evolve the sample of Praesepe periods in time. Comparing theresulting predictions to periods measured in M35 and NGC 2516 (~150 Myr) andfor kinematically selected young and old field star populations suggests thatstellar spin-down may progress more slowly than described by these relations.

The Factory and The Beehive I. Rotation Periods For Low-Mass Stars in Praesepe