\begin{table}%t1
\caption{\label{tab1}Summary of the best fit clustering parameters. Poissonian 
uncertainties (only) are quoted here to allow comparison between different 
galaxy samples within the same GOODS field (see text). When comparing
the results between the two fields, or when comparing the average
properties of GOODS sources with those of other fields, cosmic
variance uncertainties must also be included (see Table~\ref{tab2}).}
\small%\centerline
{
\begin{tabular}{lrcccccc}
\hline \hline\noalign{\smallskip}
Sample& $N^a$& $z$ range& $\bar z^b$& $\bar L_{\rm IR}^c$& $r_0$~~~~~~& $\gamma$& $r_0(\gamma=1.5)$\\
&&&&&[$h^{-1}$~Mpc]&&[$h^{-1}$~Mpc]\\
\hline
\multicolumn{7}{c}{GOODS-South}\\
$f_{24}>20~\mu$Jy&                     495& 0.1--1.4& 0.74& 4.58& $4.25 \pm 0.12$& $1.51 \pm 0.04$& $4.23 \pm 0.09$\\
$L_{\rm IR}>10^{10}~L_{\odot}$&              444& 0.1--1.4& 0.81& 5.51& $4.58 \pm 0.13$& $1.53 \pm 0.04$& $4.52 \pm 0.11$\\
$L_{\rm IR}>10^{11}~L_{\odot}$&              161& 0.1--1.4& 1.04& 20.6& $5.22 \pm 0.31$& $1.61 \pm 0.09$& $5.00 \pm 0.29$\\
$L_{\rm IR}\leq 10^{11}~L_{\odot}$&          334& 0.1--1.4& 0.67& 2.62& $4.09 \pm 0.15$& $1.54 \pm 0.05$& $4.03 \pm 0.14$\\
$L_{\rm IR}>10^{11}~L_{\odot}$&               63& 0.5--1.0& 0.73& 17.2& $6.21 \pm 0.55$& $1.56 \pm 0.14$& $6.12 \pm 0.51$\\
$10^{10}<L_{\rm IR}\leq 10^{11}~L_{\odot}$&  177& 0.5--1.0& 0.69& 2.83& $4.18 \pm 0.23$& $1.50 \pm 0.07$& $4.18 \pm 0.17$\\
\hline
\multicolumn{7}{c}{GOODS-North}\\
$f_{24}>20~\mu$Jy&                     811& 0.1--1.4& 0.76& 4.26& $3.81 \pm 0.08$& $1.52 \pm 0.03$& $3.77 \pm 0.06$\\
$L_{\rm IR}>10^{10}~L_{\odot}$&              734& 0.1--1.4& 0.80& 4.86& $4.03 \pm 0.09$& $1.52 \pm 0.03$& $3.99 \pm 0.07$\\
$L_{\rm IR}>10^{11}~L_{\odot}$&              218& 0.1--1.4& 0.95& 20.1& $5.05 \pm 0.27$& $1.55 \pm 0.07$& $4.92 \pm 0.21$\\
$L_{\rm IR}\leq 10^{11}~L_{\odot}$&          593& 0.1--1.4& 0.59& 2.78& $3.52 \pm 0.09$& $1.54 \pm 0.04$& $3.46 \pm 0.08$\\
$L_{\rm IR}>10^{11}~L_{\odot}$&              111& 0.5--1.0& 0.85& 18.6& $4.66 \pm 0.63$& $1.42 \pm 0.13$& $4.94 \pm 0.40$\\
$10^{10}<L_{\rm IR}\leq 10^{11}~L_{\odot}$&  320& 0.5--1.0& 0.75& 3.31& $3.42 \pm 0.11$& $1.67 \pm 0.06$& $3.14 \pm 0.10$\\
\hline
\multicolumn{7}{c}{Millennium$^d$}\\
$f_{24}>20~\mu$Jy& 49~043& 0.1--1.4& 0.83& 3.6& 2.82& 1.59& 2.52\\
$L_{\rm IR}>10^{10}~L_{\odot}$& 44~114& 0.1--1.4& 0.87& 4.1& 2.77& 1.58& 2.51\\
$L_{\rm IR}>10^{11}~L_{\odot}$& 6423& 0.1--1.4& 1.10& 13.2& 3.31& 1.64& 2.82\\
$L_{\rm IR}\leq 10^{11}~L_{\odot}$& 42~620& 0.1--1.4& 0.78& 3.0& 2.75& 1.54& 2.63\\
\hline
\end{tabular}}
\smallskip
$^a$Number of objects in each sample. 
$^b$Median redshift. 
$^c$Median IR~luminosity in units of $10^{10}~L_{\odot}$. 
$^d$Statistical errors on $r_0$ and $\gamma$ are below 0.01.
\end{table}