\begin{table}%t3
\caption{\label{ir}IR properties of the \mbox{X-ray} selected Compton-thick AGN.}
%\centerline
 {\small \begin{tabular}{lccccccccc}
\hline \hline
ID  & $z$ &  $3.6~\mu$m      & $4.5~\mu$m   & $5.8~\mu$m & 8.0~$\mu$m   & $24~\mu$m  & $R-[24]$  & $\log L_{\rm IR} $ & Comments  \\ 
(1)   & (2)&    (3) &  (4) &  (5) &   (6)       & (7)        & (8) & (9) &  (10)  \\
\hline
  35 & 2.203 &  -- & -- & -- & -- & -- & -- & $12.95^{\dagger} $ & sub-mm, oSFR     \\
  91 & 0.51 &  --   &   -- & --  & --  & --  & --   & --     &   \\  
  92 & 0.91 &  17.82 &  17.07 & 16.64 &  16.27 &  160.6 &  14.16  &  11.15 & irAGN\\ 
  107 & 0.59 & 18.54& 17.49&  16.47 & 15.45& 325.3 & 16.1  &  10.73 & irSFR\\ 
  121 & 0.520 &  --   &   -- & --  & --  & --  & --   & --     &   --   \\  
  127 & 1.014 &   --   &   -- & --  & --  & --  & --   &   --  &  \\  
  135 & 2.466 &  17.91 & 17.05 & 16.31& 15.97 & 376.4 & 13.88 & 11.6 & sub-mm, oSFR, irSFR \\
  171 & 1.993 &  17.86 & 17.09 & 15.92 & 14.38 &  801.1 7  & 13.60  & 12.96 & sub-mm, oAGN, irAGN\\ 
  190 & 2.005 & 16.60 & 15.64 & 14.53 & 13.33 & 1426.0 & 14.32 &  13.06 & sub-mm, oAGN, irAGN \\   
  191 & 0.276 & 16.08 & 15.81 & 15.55 &  14.77 &  --    &   --    & 10.96 & irSFR\\
\hline
\end{tabular}}
\medskip
The columns  are: (1)~Alexander ID~number; (2)~redshift;  three and two decimal numbers  refer to spectroscopic and photometric redshift respectively;  (3)~3.6~$\mu$m flux in  units   of $\mu$Jy;  (4)~4.5~$\mu$m flux in  units  of $\mu$Jy;  (5)~5.8~$\mu$m flux in  units of $\mu$Jy; (6)~8.0~$\mu$m flux in  units of $\mu$Jy; (7)~24~$\mu$m flux in  units of $\mu$Jy; (8)~$R-[24]$ colour (Vega); (9)~logarithm of the total IR~luminosity in units of $L_\odot$; (10)~comments: sub-mm denotes that the source is a sub-mm galaxy in the sample of Chapman et~al. (\cite{Chapman2005});  irAGN or  irSFR denotes whether the source has been classified as a star-forming galaxy or an AGN~according to the IR-SED fit; oAGN or oSFR denotes that the source  has been classified as an AGN or a starburst according to the optical spectrum of Chapman et~al. (\cite{Chapman2005}); $\dagger$: luminosity from Chapman et~al. (\cite{Chapman2005}).  
\end{table}