\begin{table}%t3
  %\centering
\par
  \caption{\label{table3}Dependence of the network emission on the magnetic flux: exponents of the power-law fits calculated   for the images at 4\arcsec\ and 12\arcsec\ resolution, averaged over 3.5~h and 0.5~h}
    \begin{tabular}{ccccc}
            \hline\hline
            NW flux & \multicolumn{2}{c}{4\arcsec\ resolution} & \multicolumn{2}{c}{12\arcsec\ resolution} \\
             & 3.5~h & 0.5~h & 3.5~h & 0.5~h \\
            \hline
            $|B| - I_{\rm CaII~ K}$ & 0.6 & 0.43 & 0.54 & 0.47   \\
            $|B| - I_{\rm 1600 ~\AA}$ & 0.49 & 0.53 & 0.66 & 0.44  \\
          %   \noalign{\smallskip}
          %  $|B| - I\rm{3.5 mm}$ &  & & 1.75 & 1.55 \\
            \hline
    \end{tabular} 
\end{table}