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Stellar rotation is a complex function of mass, metallicity, and age and canbe altered by binarity. To understand the importance of these parameters inmain sequence stars, we have assembled a sample of observations that spans arange of these parameters using a combination of observations from TheTransiting Exoplanet Survey Satellite (TESS) and the Kepler Space Telescope. Wefind that while we can measure rotation periods and identify other classes ofstellar variability (e.g., pulsations) from TESS lightcurves, instrumentsystematics prevent the detection of rotation signals longer than the TESSorbital period of 13.7 days. Due to this detection limit, we also utilizerotation periods constrained using rotational velocities measured by the APOGEEspectroscopic survey and radii estimated using the Gaia mission for both TESSand Kepler stars. From these rotation periods, we 1) find we can trackrotational evolution along discrete mass tracks as a function of stellar age,2) find we are unable to recover trends between rotation and metallicity thatwere observed by previous studies, and 3) note that our sample reveals thatwide binary companions do not affect rotation, while close binary companionscause stars to exhibit more rapid rotation than single stars.

Rotation Distributions around the Kraft Break with TESS and Kepler: The Influences of Age, Metallicity, and Binarity