observed period spacing patterns for both the detected prograde and retrograde series, as well as the spacings predicted by the most suitable model in the grid, by assuming the values for $f_{rot}$ and $\Delta\Pi_{l}$ obtained by modelling the prograde series. For the calculation of the period series in the case of Rossby modes, $\Pi_0$ was derived from $\Delta\Pi_{l}$ using Eq.(\[eq:1\]), and this value was subsequently filled into Eq.(\[eq:4\]). The appropriate eigenvalues $\lambda$ were computed using the asymptotic approximation derived by @Townsend2003c, i.e. Eq.(37) in that study. This equation is valid when $\lambda \neq m^2$, as is the case here. The expected values of $\lambda$ for Rossby modes are three to four orders of magnitude smaller than for retrograde gravito-inertial modes, which allowed us to identify the observed pulsations. However, as @Townsend2003c pointed out, the asymptotic approximation does not converge well to the numerical solution in the case of such modes. The possibility to compute Rossby modes has currently not yet been included in the publicly available version of GYRE. As a consequence, we could not do a reliable quantitative analysis of the retrograde series at this point and limited ourselves to the analysis of the prograde series to derive $f_{\rm 