\begin{table}%t2
\caption{Parameters for the asymptotic formula Eq.~(\ref{eq:asymptotic2}).}
\label{tab:asymptotic2} 
%\centerline
{
\begin{tabular}{ccccccccccccccc}
\hline
\hline\noalign{\smallskip}
\multicolumn{3}{c}{Stellar parameters} & & & &
\multicolumn{4}{c}{\dotfill $\tilde{\l}=0$ \dotfill} &
\multicolumn{4}{c}{\dotfill $\tilde{\l}=1$ \dotfill} & \\
$\displaystyle \frac{M}{M_{\odot}}$ & 
$\eta$ &
$\alpha$ &
$\begin{array}{c} \displaystyle \Delta_{\tilde{n}} \\ (\mu{\rm Hz}) \end{array}$ & 
$\displaystyle \frac{\Omega_{{\rm fit}}}{\Delta_{\tilde{n}}}$  &
$\displaystyle \frac{\Omega_{{\rm real}}}{\Delta_{\tilde{n}}}$  &
$\displaystyle \frac{D_{\tilde{m}}}{\Delta_{\tilde{n}}}$ &
$\displaystyle \mu$ &
$\displaystyle \frac{\tilde{\alpha}}{\Delta_{\tilde{n}}}$ &
$\displaystyle \frac{D_{\tilde{m}}}{2 \mu \Delta_{\tilde{n}}}$ &
$\displaystyle \frac{D_{\tilde{m}}}{\Delta_{\tilde{n}}}$ &
$\displaystyle \mu$ &
$\displaystyle \frac{\tilde{\alpha}}{\Delta_{\tilde{n}}}$ &
$\displaystyle \frac{D_{\tilde{m}}}{2 \mu \Delta_{\tilde{n}}}$ &
$\displaystyle \frac{\left< \delta \omega^2 \right>^{1/2}}{\Delta_{\tilde{n}}}$ \\
\noalign{\smallskip}\hline
25 & 0.6 & 0.0 & 14.91 & 0.980 & 0.989       & 0.197 & 5.95 & 2.67 & 0.0166 & 0.234 & 5.11 & 3.41 & 0.0229 & 0.045 \\
25 & 0.6 & 0.2 & 15.01 & 0.962 & 0.953--0.993 & 0.221 & 6.04 & 2.50 & 0.0183 & 0.244 & 4.52 & 3.52 & 0.0270 & 0.052 \\
\hline
\end{tabular}}
\medskip
Values of the parameters from Eq.~(\ref{eq:asymptotic2}) used to fit
         the frequencies in Fig.~\ref{fig:frequency_spectrum}
         ({i.e.} the ranges on the quantum numbers are
         $15\leq\tilde{n}\leq 20$, $0\leq\tilde{\l}\leq1$ and $-10\leq m \leq
         10$). These values are similar to those in Table~\ref{tab:asymptotic}
         (see text for details).  The two values of
         $\Omega_{{\rm real}}$ for the differentially rotating model (second
         line) are the lower and upper bounds on the angular velocity, {i.e.}
         the equatorial and polar rotation rates, respectively. The parameter
         $\Omega_{{\rm fit}}$ is twice as close to $\Omega_{{\rm real}}$
         as in Table~\ref{tab:asymptotic} for the uniformly rotating model
         ($\alpha = 0$) due to the inclusion of higher azimuthal orders. 
\end{table}