@VanReeth2015, gravity-mode period spacing patterns are heavily influenced by rotation. We therefore introduced the influence of rotation on the pulsation periods using the traditional approximation [@Eckart1960; @Lee1987; @Townsend2005]. In this framework the $\theta$-component of the rotation vector is ignored [@Lee1997] and it is assumed that the star is sufficiently slowly rotating, so the effects of the centrifugal force can be neglected. While this particular assumption may not always be applicable, gravity-modes and gravito-inertial modes are mostly sensitive to the stellar properties near the convective core, where the rotational deformation of the star remains limited. This is illustrated in Fig.\[fig:kernels\], which shows both the Brunt-Väisälä frequency $N$ and the rotational kernel $K_{nl}$ for the lowest- and highest-order mode of the stellar model discussed in Sec.\[subsec:synthdata\]. Both functions correlate with the sensitivity of the pulsations to the different regions in the star and peak near the convective core boundary. The rotational kernel $K_{nl}$ specifically indicates the sensitivity of the pulsations to the local stellar rotation profile. Thus, the rotational frequencies deduced from pulsational properties throughout this paper correspond with the near-core interior rotation rates.

@Ballot2011 showed that the traditional approximation continues to perform adequately if the spin parameter $|s| \leq 2$ [see 