\begin{table}%t10
      \caption{Source counts without the corrections.}
         \label{tab10}
%\centerline
{
     \begin{tabular}{rrrrrrrrrr}
\hline  \hline
 \multicolumn{3}{c}{Cumulative counts $N_{\rm obs}$ (sr$^{-1}$)} & & 
   \multicolumn{6}{c}{
   Differential counts 
   $\Delta N_{\rm obs}/\Delta S_{\rm obs}$ (Jy$^{-1}$sr$^{-1}$)} \\
 \cline{1-3} \cline{5-10} 
 Flux & C\_90 & C\_160 & & \multicolumn{3}{c}{Flux bin} & 
 Eff. Flux & C\_90 & C\_160 \\
 $S_{\rm obs}$(mJy) &  &  & & su$^a$ & -- & sl$^a$ & 
 $S^{*}_{\rm obs}$(mJy)$^b$ & & \\
\hline
 400 & 3.63 $\times$ 10$^3$ (1.00) & 7.42 $\times$ 10$^3$ (0.71) & &   & -- & 400  &  & 
      &  \\
 283 & 1.09 $\times$ 10$^4$ (0.58) & 2.97 $\times$ 10$^4$ (0.35) & & 400 & -- & 283 & 328 & 
     6.20 $\times$ 10$^4$ (0.71) & 1.90 $\times$ 10$^5$ (0.41) \\
 200 & 4.73 $\times$ 10$^4$ (0.28) & 1.00 $\times$ 10$^5$ (0.19) & & 283 & -- & 200 & 232 & 
     4.39 $\times$ 10$^5$ (0.32) & 8.51 $\times$ 10$^5$ (0.23) \\
 141 & 1.67 $\times$ 10$^5$ (0.15) & 2.30 $\times$ 10$^5$ (0.13) & & 200 & -- & 141 & 164 & 
     2.05 $\times$ 10$^6$ (0.17) & 2.22 $\times$ 10$^6$ (0.17) \\
 100 & 5.38 $\times$ 10$^5$ (0.08) & 2.60 $\times$ 10$^5$ (0.12) & & 141 & -- & 100 & 116 &
     8.95 $\times$ 10$^6$ (0.10) & 7.16 $\times$ 10$^5$ (0.35) \\
  70 & 7.60 $\times$ 10$^5$ (0.07) & 2.67 $\times$ 10$^5$ (0.12) & & 100 & -- &  70 & 82  &
     7.57 $\times$ 10$^6$ (0.13) & 2.53 $\times$ 10$^5$ (0.71)  \\
\hline        
 \end{tabular}}
\medskip
$-$ Values in parentheses give errors relative to the 
preceding  values; thus, $abc$ ($xyz$) means $abc \pm abc*xyz$. \\
$^{a}$ su = $\sqrt{2}$ sl, where su and sl denote upper and 
     lower values in the respective flux bin. \\
$^{b}$ $S_{\rm obs}^{*}$, effective flux density defined as
     $S_{\rm obs}^{*} = \int_{sl}^{su}S({\rm d}N/{\rm d}S){\rm d}S / \int_{sl}^{su}({\rm d}N/{\rm d}S){\rm d}S$,
     where $N(S)$ is the cumulative source counts for $S$ or brighter. 
     $S_{\rm obs}^{*} = 1.16sl$ for $N \propto S^{-3}$, while 
     $S_{\rm obs}^{*} = 1.20sl$ for ${\rm d}N/{\rm d}S = {\rm constant}$. $S_{\rm obs}^{*} = 
     1.16sl$ is used in this work, because our counts can be approximated by
     $N \propto S^{-3.2}$ at C\_90 and $N \propto S^{-2.9}$ at C\_160. 
  \end{table}