Left panel: FWHM of Hα around 30 days after peak/discovery against the black hole mass of each respective TDE. The dashed red lines represent the expected keplerian velocity correlations for bound material at different radii (assuming a sun-like star). The solid green lines are the velocities for the outflowing material assuming R_p = R_t (pericenter and tidal radii respectively) for a sun-like star (1 R_*) or red giant (10 R_*) (Arcavi et al. 2014). No evidence for correlation is found between the line widths and the BH masses. Middle panel: FWHM of Hα against the L_opt/L_X of X-ray TDEs (taken from Wevers et al. 2019a) at the epochs for which we have spectra. The only TDE that exhibits strong X-ray emission during these epochs is ASASSN-14li and it is the one with the lowest FWHM. Right panel: FWHM of Hα around 30 days after peak/discovery (same FWHM as left panel) against the peak bolometric optical/UV luminosities of each TDE taken from Hinkle et al. (2020). The graph is color coded for Bowen N III TDEs (blue) and not Bowen (orange). Low FWHM TDEs (N III Bowen TDEs) seem to have low L_peak values.