functions correlate with the sensitivity of the gravity-mode pulsations to the different regions inside the star.](kernels.pdf){width="88mm"}

Methodology {#sec:method}
===========

As we have discussed in the previous section, the influence of rotation on the pulsation frequencies depends on the values of both $l$ and $m$, while the asymptotic spacing $\Delta\Pi_l$ is dependent of the value of $l$ (Eq.\[eq:1\]). It is therefore necessary to have a pulsation mode identification if we wish to constrain the rotation profile of the observed star properly.

To derive a reliable estimate of the rotation rate of a $\gamma$Dor star with one or more observed period spacing patterns, we consider all the possible combinations of $l$ and $m$-values for the mode identification of the GYRE pulsation frequencies computed for the MESA models in our grid. For each combination of (l,m), we compute the asymptotic spacing value $\Delta\Pi_l$, as expressed in Eq.(\[eq:1\]) and subsequently correct it in the framework of the traditional approximation according to Eq.(\[eq:5\]). This is illustrated graphically in Fig.\[fig:method\]. Because the application of a rotational frequency shift does not introduce dips into the period spacing patterns, we do not need to take them into account at this point. A uniform period spacing series is sufficient 