Spectroscopic rotation velocities of the single stars in our sample, as a function of the derived near-core rotation rate, assuming uniform rotation as the statistically favoured model. The symbol and colour indicate the derived pulsation mode identification. Contrary to the other stars in this figure, the stars with Yanai modes (with (k, m)=(−1, −1)) have not been successfully modelled. For these stars, the plotted rotation frequency is a lower limit, assuming the proposed mode identification is correct. The arrows indicate how the graph changes when f_rot is higher. This figure is an update of Fig. 14 by Van Reeth et al. (2016).