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Stellar rotation periods measured in open clusters have proved to beextremely useful for studying stars' angular momentum content and rotationallydriven magnetic activity, which are both age- and mass-dependent processes.While period measurements have been obtained for hundreds of solar-mass membersof the Pleiades, period measurements exist for only a few low-mass ($<$0.5M$_{\odot}$) members of this key laboratory for stellar evolution theory. Tofill this gap, we report rotation periods for 132 low-mass Pleiades members(including nearly 100 with M $\leq$ 0.45 M$_{\odot}$), measured fromphotometric monitoring of the cluster conducted by the Palomar TransientFactory in late 2011 and early 2012. These periods extend the portrait ofstellar rotation at 125 Myr to the lowest-mass stars and re-establish thePleiades as a key benchmark for models of the transport and evolution ofstellar angular momentum. Combining our new rotation periods with preciseBVIJHK photometry reported by Stauffer et al. and Kamai et al., we investigateknown anomalies in the photometric properties of K and M Pleiades members. Weconfirm the correlation detected by Kamai et al. between a star's rotationperiod and position relative to the main sequence in the cluster'scolor-magnitude diagram. We find that rapid rotators have redder (V-K) colorsthan slower rotators at the same V, indicating that rapid and slow rotatorshave different binary frequencies and/or photospheric properties. We find nodifference in the photometric amplitudes of rapid and slow rotators, indicatingthat asymmetries in the longitudinal distribution of starspots do not scalegrossly with rotation rate.

astrophysical journal/the astrophysical journal

Why are rapidly rotating M dwarfs in the Pleiades so (infra)red? New  period measurements confirm rotation-dependent color offsets from the cluster  sequence