explain our methodology to derive the rotation frequency (Section \[sec:method\]). The method is illustrated with applications on synthetic data (Section \[subsec:synthdata\]), a slowly rotating star with rotational splitting, KIC9751996, and a fast rotator with a prograde and a retrograde period spacing series, KIC12066947 (Section \[subsec:slowfast\]). We then analyse the sample as a whole (Section \[subsec:sample\]), before moving on to the discussion and plans for future in-depth modelling of individual targets (Section \[sec:conclusions\]).

Grid of stellar models and pulsation frequencies {#sec:grid}
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We first computed a rough grid of theoretical stellar models to gain further insight into the internal structure and properties of $\gamma$Dor stars. To allow for a complete understanding, the models were purposely kept relatively simple. We did not include any rotational effects into the equilibrium models, allowing us to assume spherical symmetry and compute 1-dimensional models with the 1D MESA stellar evolution code [v7385; @Paxton2011; @Paxton2013; @Paxton2015]. The convection was treated using the mixing length theory with $\alpha_{\rm MLT} = 1.8$ and the Ledoux criterion with $\alpha_{\rm sc} = 0.01$. A single diffusive mixing coefficient was defined in the radiative region and fixed at a value of $1\,cm^2s^{-1}$. We used the solar metallicity values given by @Asplund2009 and 