\begin{table}%t3
\caption{Statistics of the field-star decontamination, in magnitude bins, for representative cases.}\label{tab3}
%\renewcommand{\tabcolsep}{1.02mm}
\par
\small %\centerline
 {\begin{tabular}{cccccccccccccccccc}
\hline\hline
&\multicolumn{5}{c}{FSR~942 ($R<3\arcmin$)}&&\multicolumn{5}{c}{FSR~855 ($R<3\arcmin$)}
&&\multicolumn{5}{c}{FSR~801 ($R<3\arcmin$)}\\
\cline{2-6}\cline{8-12}\cline{14-18}
$\Delta\jj$&\no&\nc&\ns&\sFS&\fsU && \no&\nc&\ns&\sFS&\fsU&& \no&\nc&\ns&\sFS&\fsU\\
  (mag)    &(stars)&(stars)&&(stars)& && (stars)&(stars)&&(stars)& && (stars)&(stars)&&(stars)\\
\cline{1-18}
  7--8& -- & -- & -- & -- & --&&$1\pm1.0$ &1  &1.0&0.42&1.07&&--&--&--&--&--\\
  8--9& -- & -- & -- & -- & --&& --      &--&--&-- &-- &&--&--&--&--&--  \\
 9--10& -- & -- & -- & -- & --&&$1\pm1.0$ &1  &1.0&0.99&1.42&&--&--&--&--&--    \\
10--11&$3\pm1.7$ &3 &1.7&0.57&0.51 &&$5\pm2.2$ &1  &0.4&1.12&1.02&&--&--&--&--&-- \\
11--12&$4\pm2.0$ &4 &2.0&0.38&0.18 &&$4\pm2.0$ &2  &1.0&1.70&0.49&&$2\pm1.4$&1 &0.7&0.18&0.23 \\
12--13&$7\pm2.6$ &1 &0.4&0.50&0.12 &&$6\pm2.4$ &1  &0.4&3.09&0.43&&$4\pm2.0$&2 &1.0&0.30&0.20  \\
13--14&$24\pm4.9$&17&3.5&0.75&0.08 &&$20\pm4.5$&3  &0.7&2.47&0.19&&$4\pm2.0$&2 & 1.0&0.36&0.10 \\
14--15&$38\pm6.2$&21&3.4&1.61&0.09 &&$33\pm5.7$&6  &1.0&6.27&0.26&&$9\pm3.0$&3&1.0&0.72&0.11  \\
15--16&$63\pm7.9$&27&3.4&2.87&0.08 &&$56\pm7.5$&12 &1.6&5.31&0.11&&$25\pm5.0$&9&1.8&1.60&0.12  \\
16--17&$45\pm6.7$&21&3.1&4.91&0.14 &&$72\pm8.5$&29 &3.4&6.14&0.12&&$21\pm4.6$&8&1.7&1.78&0.09 \\
\cline{2-6}\cline{8-12}\cline{14-18}
All &$184\pm13.6$&94&6.8&3.2&0.03& &$198\pm14.1$&56&3.6&11.1&0.07 &&$65\pm8.1$&25&2.9&2.8&0.06\\
\hline
\end{tabular}}
\medskip
The table provides, for each magnitude bin ($\Delta\jj$), the number of observed stars
(\no) within the spatial region sampled in the CMDs shown in the top panels of Figs.~\ref{fig3}
and \ref{fig4}, the respective number of probable member stars (\nc) computed by the decontamination algorithm, the \ns\ parameter, the 1$\sigma$ Poisson fluctuation (\sFS) around the mean, with 
respect to the star counts measured in the 8~sectors of the comparison field, and the field-star
uniformity parameter (\fsU). The statistical significance of \nc\ is reflected in its ratio with
the 1$\sigma$ Poisson fluctuation of \no\ (\ns) and with \sFS. The bottom line corresponds to the
full magnitude range.
\end{table}