\begin{table}%t1
\par
\caption{\label{tab:fits}Best fit models for the HLIRG's SED.}
\small%\centering
\par
\begin{tabular}{lllcccccccclc}
\hline\hline\noalign{\smallskip}
Source & $z$ & Type & CT\tablefootmark{a} & \multicolumn{7}{c}{Best Fit model\tablefootmark{b}} & $\log L_{\rm BOL}$\tablefootmark{c} & AGN / SB\tablefootmark{d} \\
\cline{5-11}\noalign{\smallskip}
       &   &      &        & \multicolumn{3}{c}{all data\tablefootmark{e}} & \multicolumn{3}{c}{no X-rays\tablefootmark{f}} & composite temp.\tablefootmark{g} & (erg s$^{-1}$) &  \\
       &   &      &        & \multicolumn{2}{c}{Model} & $\alpha$ & \multicolumn{2}{c}{Model} & $\alpha$ &                  &  &  \\       
\hline\noalign{\smallskip}
\multicolumn{11}{l}{Class A HLIRG} \\
\noalign{\smallskip}
\object{PG~1206+459}      & 1.158 & QSO   & N & AGN1-L & ... & 1   & AGN1 & ... & 1   & \textbf{AGN1-L}    & 48.4 &   1 / 0 \\
\object{PG~1247+267}      & 2.038 & QSO   & N & AGN1-L & ... & 1   & AGN1 & ... & 1   & \textbf{AGN1-L}    & 49.2 &   1 / 0 \\
\object{IRAS~F12509+3122} & 0.780 & QSO   & N & AGN1-L & SB1 & 0.3 & AGN1 & SB4 & 0.5 & \textbf{AGN1-L+SB1}& 47.7 & 0.3 / 0.7 \\
\object{IRAS~14026+4341}  & 0.323 & QSO   & N & ...    & SB2 & 0   & \textbf{AGN1} & \textbf{SB2} & 0.3 & SB2 & 46.7 & 0.3 / 0.7 \\
\object{IRAS~F14218+3845} & 1.21  & QSO   & N & AGN1   & SB1 & 0.4 & AGN1 & SB1 & 0.3 & \textbf{AGN1+SB1}  & 47.2 & 0.4 / 0.6 \\
\object{IRAS~16347+7037}  & 1.334 & QSO   & N & AGN1-L & ... & 1   & AGN1 & ... & 1   & \textbf{AGN1-L}    & 48.9 &   1 / 0 \\
\object{IRAS~18216+6418}  & 0.297 & QSO   & N & AGN1   & SB3 & 0.8 & AGN1 & SB3 & 0.8 & \textbf{AGN1+SB3}  & 47.4 & 0.8 / 0.2 \\
\noalign{\smallskip}
\multicolumn{11}{l}{Class B HLIRG} \\
\noalign{\smallskip}
\object{IRAS~F00235+1024} & 0.575 & NL-SB~& Y & ...    & SB3 & 0    & ...  & SB3 & 0   & \textbf{CP1} & 46.7 & $\sim$0.5 / $\sim$0.5 \\
\object{IRAS~07380-2342}  & 0.292 & SB~   & N & AGN4   & SB1 & 0.06 & AGN3 & SB1 & 0.3 & \textbf{CP1} & 47.0 & $\sim$0.5 / $\sim$0.5 \\
\object{IRAS~00182-7112}  & 0.327 & QSO 2 & Y & AGN3   & SB4 & 0.06 & AGN3 & SB3 & 0.3 & \textbf{CP1} & 46.6 & $\sim$0.5 / $\sim$0.5 \\
\object{IRAS~09104+4109}  & 0.442 & QSO 2 & Y & AGN4   & SB4 & 0.09 & AGN3 & SB1 & 0.8 & \textbf{CP2} & 47.3 & $\sim$0.7 / $\sim$0.3 \\
\object{IRAS~12514+1027}  & 0.32  & Sy2   & Y & AGN5   & SB4 & 0.06 & AGN3 & SB2 & 0.9 & \textbf{CP2} & 46.7 & $\sim$0.7 / $\sim$0.3 \\
\object{IRAS~F15307+3252} & 0.926 & QSO 2 & Y & AGN1   & SB3 & 0.03 & AGN3 & SB1 & 0.8 & \textbf{CP1} & 47.9 & $\sim$0.5 / $\sim$0.5 \\
\noalign{\smallskip}\hline 
\end{tabular}
\tablefoot{\tablefoottext{a}{Compton-thick candidates.} \\
 \tablefoottext{b}{The best fit adopted to estimate the bolometric luminosity and the AGN and SB~fraction
      is marked in bold fonts.} \\
 \tablefoottext{c}{Bolometric luminosity in CGS units.} \\
 \tablefoottext{d}{Fraction of the bolometric luminosity originated in AGN and SB. Calculated through
      the parameter $\alpha$ of the best-fit model.} \\
 \tablefoottext{e}{Best fit using our original set of templates.} \\
 \tablefoottext{f}{Best fit not using X-ray data.} \\
 \tablefoottext{g}{Best fit including the templates of composite sources.}}
\end{table}