\begin{table}%t6
%\centering
\par
\caption {\label{tab:stack160}Stacking extragalactic number counts at 160~$\mu$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
$    3.11\pm    0.46$ &  6795. &  2163. &  2485. & GTO CDFS\\
$    4.71\pm    0.16$ &  9458. &  1236. &  2104. & COSMOS\\
$    6.74\pm    0.22$ & 13203. &  1627. &  2880. & COSMOS\\
$    9.65\pm    0.26$ & 18057. &  2307. &  3986. & COSMOS\\
$   12.95\pm    0.37$ & 19075. &  2388. &  4182. & COSMOS\\
$   19.82\pm    0.48$ & 22366. &  2944. &  4987. & SWIRE EN1\\
$   25.71\pm    0.81$ & 20798. &  2811. &  4682. & SWIRE EN1\\
$   33.74\pm    0.98$ & 16567. &  2671. &  4004. & SWIRE EN1\\
$   45.18\pm    2.08$ & 20089. &  4849. &  6049. & SWIRE EN1\\
\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{Stansberry2007}.}
\end{table}