  Stellar rotation is a complex function of mass, metallicity, and age and can
be altered by binarity. To understand the importance of these parameters in
main sequence stars, we have assembled a sample of observations that spans a
range of these parameters using a combination of observations from The
Transiting Exoplanet Survey Satellite (TESS) and the Kepler Space Telescope. We
find that while we can measure rotation periods and identify other classes of
stellar variability (e.g., pulsations) from TESS lightcurves, instrument
systematics prevent the detection of rotation signals longer than the TESS
orbital period of 13.7 days. Due to this detection limit, we also utilize
rotation periods constrained using rotational velocities measured by the APOGEE
spectroscopic survey and radii estimated using the Gaia mission for both TESS
and Kepler stars. From these rotation periods, we 1) find we can track
rotational evolution along discrete mass tracks as a function of stellar age,
2) find we are unable to recover trends between rotation and metallicity that
were observed by previous studies, and 3) note that our sample reveals that
wide binary companions do not affect rotation, while close binary companions
cause stars to exhibit more rapid rotation than single stars.
