The Dos and Don'ts of Stellar Rotation with TESS

Rotation is a complex function of mass, metallicity, binarity, and age in low-mass main sequence stars. Here, we show that we can measure rotation periods from lightcurves in the TESS SCVZ and use TESS lightcurves to identify other classes of stellar variability (e.g. pulsations). However, instrument systematics prevent the detection of rotation signals longer than the TESS orbital period of 13.7 days. We use these rotation periods, rotational velocities from the APOGEE spectroscopic survey, and radii inferred from Gaia to trace rotation as a function of evolution for stars around the Kraft Break (~1.25 solar masses). Additionally, comparing the distribution of detected stars in Kepler and TESS reveals key differences between stellar populations probed by these two missions, with TESS probing a significant population of young stars that were not present in the Kepler sample