\begin{table}%t3
\caption{\label{tab_flux}Results of the H$_2$ S(1) line analysis.}
\par
%\centerline
{\begin{tabular}{lcccccccccccccccccc}
  \hline
  \hline \noalign{\smallskip}  
  Star   & $\lambda _{\rm obs}$\tablefootmark{(a)}& Integrated flux\tablefootmark{(b)} & 
  Intensity\tablefootmark{(b)}                & 
  \multicolumn{3}{c}{$N({\rm H}_2)$ upper limits\tablefootmark{(b)}}   & &  
  \multicolumn{3}{c}{H$_2$ mass upper limits\tablefootmark{(b, c)}}     
  \\
  HD     &  ($\mu$m)       & (\flux)                 & (erg~s$^{-1}$~cm$^{-2}$~sr$^{-1}$) &  \multicolumn{3}{c}{(cm$^{-2}$)}                  & &   \multicolumn{3}{c}{ ($M_{\rm Jup}$)} 
  \\
  \cline{5-7}  \cline{9-11}
         &                 &                         &                                      &    150~K  & 300~K & 1000~K                             & &     150 K &    300 K  &  1000 K \\
  \hline    
142527  & 17.0351          & $<1.0\times 10^{-14}$ & $<$2.5~$\times$~10$^{-3}$ & 9.4~$\times$~10$^{22}$ & 6.1~$\times$~10$^{21}$ & 1.4~$\times$~10$^{21}$ & & 1.9~$\times$~10$^{-1}$ & 1.2~$\times$~10$^{-2}$ & 3.3~$\times$~10$^{-3}$ \\ 
169142  & 17.0343          & $<$1.8~$\times$~10$^{-14}$ & $<$4.2~$\times$~10$^{-3}$ & 1.6~$\times$~10$^{23}$ & 1.0~$\times$~10$^{22}$ & 2.4~$\times$~10$^{21}$ & & 3.5~$\times$~10$^{-1}$ & 2.1~$\times$~10$^{-2}$ & 6.1~$\times$~10$^{-3}$ \\ 
150193A & 17.0349          & $<$2.1~$\times$~10$^{-14}$ & $<$5.0~$\times$~10$^{-3}$ & 1.9~$\times$~10$^{23}$ & 1.2~$\times$~10$^{22}$ & 2.8~$\times$~10$^{21}$ & & 4.5~$\times$~10$^{-1}$ & 2.7~$\times$~10$^{-2}$ & 7.7~$\times$~10$^{-3}$ \\
163296  & 17.0345          & $<$2.8~$\times$~10$^{-14}$ & $<$6.7~$\times$~10$^{-3}$ & 2.5~$\times$~10$^{23}$ & 1.6~$\times$~10$^{22}$ & 3.8~$\times$~10$^{21}$ & & 3.9~$\times$~10$^{-1}$ & 2.4~$\times$~10$^{-2}$ & 6.9~$\times$~10$^{-3}$ \\
100546  & 17.0363          & $<$1.4~$\times$~10$^{-13}$ & $<$3.3~$\times$~10$^{-2}$ & 1.2~$\times$~10$^{24}$ & 7.9~$\times$~10$^{22}$ & 1.9~$\times$~10$^{22}$ & & 1.4                  & 8.4~$\times$~10$^{-2}$ & 2.4~$\times$~10$^{-2}$ \\  
  \hline
\end{tabular}}
\tablefoot{\tablefoottext{a}{expected position of the line in the observed spectra by
  correcting the radial velocity of the star for the epoch of
  observation.}
\tablefoottext{b} {3$\sigma$ upper confidence limits.}
\tablefoottext{c} {masses of H$_2$ are calculated assuming the distances quoted
  in Table~\ref{param}.}}\vspace*{5mm}
\end{table}