\begin{table}%t3
%\centering
\par
\caption{\label{tab_PM}Gaussian fit parameters.}
%\tiny
\renewcommand{\tabcolsep}{0.65mm}
\par
\begin{tabular}{lccccc}
\hline\hline
Cluster&$\overline{\mu_\alpha~\cos(\delta)}$&$\sigma_\alpha$&$\overline{\mu_\delta}$&
$\sigma_\delta$&$\sigma_{\rm v}$\\
       &(\kms)&(\kms)&(\kms)&(\kms)&(\kms)\\
\hline
Cr~197&$-22.2\pm4.1$&$10.2\pm3.7$&$-8.1\pm4.0$&$14.4\pm4.3$&$22\pm5$\\
\par
Cr~197&$-48.5\pm5.0$&$6.6\pm3.6$&$+30.6\pm2.1$&$9.9\pm1.8$&$15\pm3$\\
\par
vdB~92&$-18.0\pm1.6$&$11.1\pm1.3$&$+14.5\pm2.1$&$13.1\pm1.7$&$21\pm2$\\
\par
\hline
\end{tabular}
\tablefoot{$\sigma_\alpha$ and $\sigma_\delta$ are the velocity dispersions in
right ascension and declination, respectively. Assuming spherical symmetry, 
we define $\sigma_{\rm v}^2=\frac{3}{2}(\sigma_\alpha^2+\sigma_\delta^2)$.}
%\vspace*{1.5mm}
\end{table}