  While many M dwarfs are known to have strong magnetic fields and high levels
of magnetic activity, we are still unsure about the properties of their
starspots and the origin of their magnetic dynamos. Both starspots and
chromospheric heating are generated by the surface magnetic field; they produce
photometric variability and Halpha emission, respectively. Connecting
brightness variations to magnetic activity therefore provides a means to
examine M dwarf magnetism. We survey 30 M dwarfs previously identified as fast
rotating stars (Prot < 10 days). We present time-series optical photometry from
the Transiting Exoplanet Survey Satellite (TESS) and contemporaneous optical
spectra obtained using the Ohio State Multi-Object Spectrograph (OSMOS) on the
2.4m Hiltner telescope at MDM Observatory in Arizona. We measure rotation
periods and photometric amplitudes from TESS light curves using Gaussian
Processes. From the OSMOS spectra, we calculate the equivalent width of Halpha,
and LHalpha/Lbol. We find a weak positive correlation between Halpha luminosity
and the semi-amplitude, Rvar p=0.005_{-0.005}^{+0.075}. We also observe
short-term variability (between 20-45 minutes) in Halpha equivalent widths and
possible enhancement from flares consistent to recent literature.
