@Ballot2011 Fig.2], with $$s = \frac{2f_{\rm rot}}{f_{co}}, \label{eq:3}$$ where $f_{\rm rot}$ ($=\Omega/2\pi$) and $f_{co}$ are the stellar rotation frequency and the pulsation frequency in the corotating frame respectively. Thanks to the assumptions made in the traditional approximation, the computational requirements for the effects of rotation are dramatically reduced. In this work, we used the traditional approximation module from the 1D pulsation code GYRE v4.3 [@Townsend2013], and follow the approach described by @Ballot2011 and @Bouabid2013. These authors show that, within the traditional approximation, an asymptotic pulsation period series can be rewritten for a rotating star as $$P_{nlm,co} = \frac{\Pi_0}{\sqrt{\lambda_{l,m,s}}}(n + \alpha_{g}),
\label{eq:4}$$ where $P_{nlm,co}$ is the pulsation period of radial order $n$, spherical degree $l$ and azimuthal order $m$ in the corotating frame. In this paper, we adopt the convention that $m >
0$ corresponds with prograde modes and $m < 0$ with retrograde modes, respectively. In this equation, $\lambda_{l,m,s}$ is the eigenvalue of the Laplace tidal equation depending on $l$, $m$, and the spin parameter $s$, while the phase term $\alpha_{g}$ depends on the internal stellar properties at the boundaries of the pulsation mode cavity and can be taken to be 0.5 for stars with a convective core and a 