\begin{table}%t2
\par
  \caption {\label{tab_sOri_GCS:nb_VLM_BD}Comparison of the numbers of low-mass stars
and brown dwarfs as a function of the distance
from the cluster centre (D), from~5 to 30~arcmin in radius.
}
%\centerline
 { \begin{tabular}{@{\hspace{0mm}}c  c c c  c c c@{\hspace{0mm}}}
 \hline\hline
 D  & Stars$^{a,b}$ & BD$^{c}$ &  R1$^{d}$ & Stars$^{a}$ & BD$^{c}$ &  R1$^{e}$   \\
    &             &     &  \%   &           &     &  \%   \\
 \hline
 5  &  24 (25) &   5  & 20.8 (10.2)  &  27 (25) &   3  & 11.1 (5.8)  \\
10  &  64 (43) &  24  & 37.5 (22.4)  &  77 (43) &  13  & 16.9 (10.8)  \\
15  &  93 (62) &  37  & 39.8 (23.9)  & 109 (62) &  24  & 22.0 (14.0)  \\
20  & 128 (81) &  51  & 39.8 (24.4)  & 147 (81) &  37  & 25.2 (16.2)  \\
25  & 163 (108) &  59  & 36.2 (21.8)  & 186 (108) &  42  & 22.6 (14.3)  \\
30  & 198 (120) &  73  & 36.9 (23.0)  & 223 (120) &  56  & 25.2 (16.4)  \\
 \hline
 \end{tabular}}
\par
 \smallskip
\par
$^{a}$ In this table, low-mass stars are defined as objects with masses 
between~0.5 and 0.08~$M_{\odot}$ (for the purpose of the indices).
$^{b}$ The numbers in brackets take into account the most massive members 
($J \leq 12$~mag; $M \geq 0.5$~$M_{\odot}$) of \sOri{} taken Mayrit catalogue 
\citep{caballero08c}, yielding the $R_{\rm SS}$ or R1~ratios defined by \citet{briceno02} 
and \citet{luhman03b}, respectively.
 $^{c}$  In this table, brown dwarfs are defined as objects with masses 
between~0.08 and 0.02~$M_{\odot}$ (for the purpose of the indices).
 $^{d}$  The results on the left-hand side assume a distance of 352~pc from {\it{Hipparcos}}.
 $^{e}$  The results on the right-hand side assume a distance of 440~pc \citep{brown94,sherry04}.
\end{table}