\begin{table}%t5
%\centering
\caption {\label{tab:stack70}Stacking extragalactic number counts at 70~$\mu$m.}
%\centerline
 {\begin{tabular}{lrrrr}
\hline\hline
\noalign{\smallskip}
$\langle S\rangle$ & d$N/{\rm d}S.S^{2.5}$ & $\sigma_{\rm clus.}$ & $\sigma_{\rm clus.+calib.}$ & Field\\
\cline{1-4}
\noalign{\smallskip}
(in mJy) & \multicolumn{3}{c}{(in gal~Jy$^{1.5}$~sr$^{-1}$)} & \\
\hline
$    0.38\pm    0.05$ &   246. &    72. &    76. & FIDEL CDFS\\
$    0.64\pm    0.07$ &   517. &   109. &   122. & FIDEL CDFS\\
$    0.94\pm    0.03$ &   646. &    80. &   105. & COSMOS\\
$    1.48\pm    0.04$ &  1218. &   151. &   198. & COSMOS\\
$    2.14\pm    0.05$ &  1456. &   183. &   239. & COSMOS\\
$    3.27\pm    0.07$ &  1657. &   211. &   273. & COSMOS\\
\hline
\end{tabular}}
\tablefoot {$\sigma_{\rm clus.}$ is the uncertainty taking into account clustering (see Sect.~\ref{subsection:sectclus}). $\sigma_{\rm clus.+calib.}$ takes into account both clustering and calibration \citep{Gordon2007}.}
\end{table}