rot}$. However, several qualitative arguments can be made in favour of Rossby modes as a correct identification. From the upward slope and the small average period spacing of the observed pattern, we derive that these modes are retrograde in the corotating frame with $|f_{co}| < f_{rot}$, which is completely in line with the theoretical expectations. Furthermore, the observed spin parameter values are larger for the retrograde than for the prograde modes, e.g., the values of the dominant modes of both series are $15.8\,\pm0.4$ and $7.7\,\pm0.1$, respectively. This indicates that in the corotating frame the pulsation frequencies of the retrograde modes are smaller than those of the prograde modes, which in turn can be explained by the small values of the eigenvalues $\lambda$. Finally, @Townsend2003c also notes that, compared to the retrograde gravito-inertial modes, Rossby modes are less equatorially confined as the stellar rotation rate increases. As a result, the latter can be expected to be less influenced by the geometrical cancellation effects, though the effect is still present. For KIC12066947, we find that the dominant prograde and Rossby modes are confined within equatorial bands with a width of 77.2 and 53.5 respectively.

For a fast rotating star such as KIC12066947, 