\begin{table}%t3
\caption{\label{tab:allphot}All photometric cluster member candidates of our survey.  Table~\ref{tab:allphot} is published in its entirety in the
      electronic edition of \textit{Astronomy \& Astrophysics}.  A
      fraction is shown here for guidance regarding its form and
      content.}
%\centerline
 {\small \begin{tabular}{ccccccccc}
\hline\hline
ID & $\alpha$ & $\delta$ & $I_{\rm c}^a$ & $J ^a$ & $K_{\rm s} ^a$ & $M^a$ & $T_{\rm eff}^a$ & $J_{\rm model}^a$ \\
& ($^{\rm h}$~$^{\rm m}$~$^{\rm s}$) & ($^\circ$~$'$~$''$) & [mag] & [mag] & [mag] & [$M_\odot$] & [K] & [mag] \\
      \hline
      001&08 40 53.61&+19 40 58.6 &19.19 &16.81 &15.61 &0.089&2665&17.00 \\
      002&08 41 08.8 &+19 43 27.5 &16.14 &14.95 &13.97 &0.219&3321&14.86 \\
      003&08 41 01.6 &+19 52 02.5 &16.67 &15.35 &14.38 &0.162&3189&15.48 \\
      004&08 41 12.17&+19 52 48.6 &18.43 &16.39 &15.46 &0.099&2805&16.72 \\
      005&08 41 08.5 &+19 54 02.0 &19.02 &16.58 &15.39 &0.088&2636&17.06 \\
      006&08 40 10.74&+19 40 49.8 &16.97 &15.47 &14.36 &0.132&3061&15.95 \\
      007&08 39 39.56&+19 47 54.3 &17.95 &16.10 &15.07 &0.104&2860&16.58 \\
      008&08 39 43.38&+19 48 45.7 &16.89 &15.56 &14.68 &0.161&3186&15.50 \\
      009&08 39 55.84&+19 53 14.3 &20.29 &17.50 &16.54 &0.081&2520&17.32 \\
      010&08 39 06.9 &+19 47 08.0 &16.51 &15.14 &14.20 &0.155&3166&15.57 \\
      \hline
    \end{tabular}}
\medskip
$^a$ The 1$\sigma$ uncertainty in the determination of magnitude, effective
temperature and mass are the following: $\Delta$mag~=~0.002~mag, $\Delta T_{\rm eff} = 140$~K and $\Delta M=0.1~M_\odot$ for stars ($M > 0.2~M_\odot$), $\Delta$mag~=~0.01~mag, $\Delta T_{\rm eff} = 230$~K and
$\Delta M = 0.05~M_\odot$ for very low-mass stars (0.072~$M_\odot< M < 0.2~M_\odot$), $\Delta$mag~=~0.04~mag, $\Delta$$T_{\rm eff} = 420$~K
and $\Delta M  = 0.02~M_\odot$ for BDs ($M<~0.072~M_\odot$). The magnitude $J_{\rm model}$ is the predicted magnitude based on photometric determination of $T_{\rm eff}$ and mass. 
\end{table}