in $\gamma$Dor stars for moderate to fast rotators or may be caused by the limited applicability of the traditional approximation for these rotation rates. Further research on this topic is required.

In Fig.\[fig:spin\] we show the spin parameter $s$, as defined in Eq.(\[eq:3\]) and listed in the last column of Table \[tab:param\], as a function of the measured rotation frequency $f_{\rm rot}$. The spin parameter $s$ is a measure of the impact of rotation on the pulsation frequency and is inversely proportional to the pulsation frequency $f_{\rm co}$ in the corotating frame. Once again, the Rossby modes (marked with dark blue dots) have small values for the eigenvalue $\lambda$. In addition, despite the fact that both prograde sectoral modes and Rossby modes are less easily confined in a band around the equator, the effect is still significant for these high values of $s$ [@Townsend2003c]. This implies many of the stars in our sample are seen at moderate to high inclination angles. We further note that our observed values of $s$ are on average much larger than the values quoted in theoretical papers in the literature [e.g. @Townsend2003b; @Ballot2011].

Fig.\[fig:superinert\] offers a closer look at the three slowest rotating stars in 