for differential rotation. However, for ten of them the second detected period spacing pattern corresponds to Rossby modes, for which we still need to develop a suitable computational tool to arrive at appropriate numerical values, as discussed in Section \[subsec:slowfast\]. For the remainder of this study, we assign the values of $f_{\rm rot}$ and $\Delta\Pi_l$ which we obtained from the prograde series to the retrograde series of the same star. Because formal mode identification of these retrograde pulsations is currently not possible, they are marked as “R” in Table \[tab:param\]. For two other stars we have both a zonal and prograde dipole series, while for a third we have prograde dipole and quadrupole modes. Finally, KIC9751996, the slowly rotating star we discussed in Sec.\[subsec:slowfast\], is the only target for which we have a series of rotationally split multiplets. For each of these last four stars, we were able to use the multiple detected period spacing patterns to refine the obtained $f_{\rm rot}$ and $\Delta\Pi_l$.

![\[fig:single\] Part of the frequency spectrum of KIC7365537. The light grey area shows the location of the pulsation modes which form the detected period spacing pattern of this star. The dashed line marks the value of 