\begin{table}%t1
%\centering
\par
\caption{\label{tab:comp}95\% completeness flux density and photometric noise for different depths at different wavelengths.}
\begin{tabular}{lrrrrrrrr}
\hline\hline\noalign{\smallskip}%\cline{2-9}
\multicolumn{1}{c}{} & \multicolumn{2}{c}{95\% completeness} & \multicolumn{2}{c}{Instrumental noise} & \multicolumn{2}{c}{Total photometric noise} & \multicolumn{2}{c}{Deduced confusion noise} \\
\cline{2-9}
\multicolumn{1}{c}{} & \multicolumn{2}{c}{mJy} &  \multicolumn{2}{c}{mJy} &  \multicolumn{2}{c}{mJy} &  \multicolumn{2}{c}{mJy}\\
\cline{2-9}
\multicolumn{1}{c}{} & Shallow & Deep & Shallow & Deep & Shallow & Deep & Shallow & Deep\\
\hline
250~$\mu$m & 203 & 97 &  37.7 & 11.1 & 47.3 & 24.9 & 28.6 & 22.3\\
350~$\mu$m & 161 & 83 & 31.6 & 9.3 & 35.8 & 20.3 & 16.8 & 18.0\\
500~$\mu$m & 131 & 76 &  20.4 & 6.0 & 26.4 & 17.6 & 16.7 & 16.5\\
\hline
\end{tabular}
\tablefoot{The instrumental noise is given by the noise map. The total photometric noise includes the instrumental and confusion noise and is determined by Monte-Carlo simulations. The confusion noise is computed with the formula $\sigma_{\rm conf} = \sqrt{\sigma_{\rm tot}^2-\sigma_{\rm instr}^2}$.}
\end{table}