inertial reference frame is included in the appendix in Fig.\[fig:sample\_inext\]. For the majority of the stars, we obtain similar values of $f_{\rm dom,corot}$ between 0.15 and 0.75$\rm
d^{-1}$. This can be linked to the convective flux blocking excitation mechanism. @Dupret2005 and @Bouabid2013 remarked that, in order for the mode excitation mechanism to be efficient, the thermal timescale $\tau_{th}$ at the bottom of the convective envelope has to be on the order of the pulsation periods in the corotating frame. From this information and the content of Fig.\[fig:sample\_ov\], we can then also derive that both the detected retrograde spacing series and single modes likely have azimuthal order $m = -1$, because only $|m|=1$ led to similar $f_{\rm dom,corot}$ values for the series of different stars. While these results are consistent, we note that the observed pulsation periods in the corotating frame are typically larger than the theoretical values computed by @Bouabid2013. For the retrograde Rossby modes this can be linked to the correspondingly low eigenvalues $\lambda$ of the Laplace tidal equation. However, the same discrepancy is observed for the prograde modes as well, though to a lesser degree. This discrepancy may point towards limitations of the current theory of mode excitation 