we also have to take into acccount rotational deformation. The centrifugal force leads to a lower effective gravity at the equator than at the pole. This influences the Brunt-Väisälä frequency, which affects the pulsations. In the case of KIC12066947, we could roughly estimate the deformation of the star, using equation A.6 from @Maeder2000. In this analysis we evaluated the observed spectroscopic parameter values and asymptotic spacing $\Delta\Pi_{l}$ using the models in our MESA grid and took the best matching model ($M = 1.5M_\odot$, $Z = 0.014$, $X_i=0.69$, $X_c = 0.452$, $\alpha_{\rm ov} = 0.01$) as a guess for the stellar structure. We found that $f_{\rm rot}/f_{\rm rot,crit} = 0.78$ and $R_{\rm pole}/R_{\rm eq} = 0.88$. A two-dimensional treatment of the rotation is clearly needed to quantify the impact of the rotation on the modes, which will allow us to improve our constraints on $f_{\rm rot}$ and $\Delta\Pi_l$.

![\[fig:kic12066947\_retro\] *Top:* The observed period spacing patterns (black dots and grey triangles) for the prograde (left) and retrograde (right) modes of KIC12066947. The black part of the pattern was used to determine $f_{rot}$ and $\Delta\Pi_{l}$, while the grey section was excluded. The white squares indicate the model fit, assuming we are dealing with 