\begin{table}%t3
\caption{Physical parameters of the programme stars (values for \xcma{} from Morel et~al. \cite{morel}).} 
\label{tab:parameters}
\small%\centerline
 {
\begin{tabular}{lccc}
\hline
\hline
&&& \\[-8pt]
& \multicolumn{1}{c}{\xcma{}} & \multicolumn{1}{c}{\tsco{}} & \multicolumn{1}{c}{\tcar{}}            \\
\hline
Spectral type    & \multicolumn{1}{c}{B0.7 IV} & \multicolumn{1}{c}{B0.2 V} & \multicolumn{1}{c}{B0.2 V} \\
$T_{\rm eff}$ (K)        & 27~500  $\pm$  1000  & 31~500  $\pm$  1000 & 31~000  $\pm$  1000 \\
$\log g$ (cm s$^{-2}$)   & 3.75     $\pm$  0.15  & 4.05     $\pm$ 0.15 & 4.20     $\pm$  0.20 \\
$\xi$ (km~s$^{-1}$)      & 6        $\pm$  2     & 2       $\pm$  2    & 12      $\pm$  4    \\
$v \sin i$ (km~s$^{-1}$) & 10       $\pm$  2$^a$ & 8        $\pm$ 2    & 113      $\pm$  8    \\ 
\hline
\end{tabular}}
\medskip
$^a$ This value is an upper limit, as the spectral lines are significantly broadened 
by pulsations in this $\beta$~Cephei variable.
\end{table}