\begin{table}%t7
\caption{\label{montecarlo}Probability of missing a significant orbital $RV$ variation$^{{a}}$.}             
\par
%\centerline
 {          
\begin{tabular}{l c c c c c}   
\hline\hline                      
Star & $M_1$ & 2--10 & 10--365 & 365--3000 &2--3000\\
\hline                    
HD~46~056 & 20.8 & 0.02 & 0.17 & 0.77 & 0.24\\
HD~46~149 & 20.8 & 0.01 & 0.04 & 0.31 & 0.07\\
HD~46~150 & 34.4 & 0.01 & 0.03 & 0.21 & 0.05\\
HD~46~202 & 17.1 & 0.01 & 0.09 & 0.50 & 0.13\\
HD~46~223 & 46.9 & 0.01 & 0.03 & 0.22 & 0.05\\
HD~46~485 & 20.8 & 0.01 & 0.20 & 0.68 & 0.20 \\
HD~46~573 & 22.9 & 0.01 & 0.06 & 0.38 & 0.09\\
HD~46~966 & 18.8 & 0.01 & 0.06 & 0.34 & 0.08\\
HD~48~279 & 22.9 & 0.01 & 0.07 & 0.40 & 0.10\\
\hline
\end{tabular} }
\par
\smallskip
$^{{a}}$ Table \ref{montecarlo} lists the probability of missing a significant orbital {\it RV}~variation ($\Delta {\it RV} > 40$~km~s$^{-1}$ for the two rapid rotators and $\Delta RV > 20$~km~s$^{-1}$ for the other stars). $M_1$ represents the primary mass and is expressed in $M_{\odot}$. The last four columns are classified according to the orbital period of the system (in days).
\end{table}