\begin{table}%t8
      \caption{\label{table.ctts}Intermediate- and low-mass X-ray stars in $\sigma$~Orionis with
      colours $J-K_{\rm s} >$ 1.15~mag\tablefootmark{a}.}   
       %%\centerline
\par
{\small
         \begin{tabular}{lcc c ccccc}
            \hline
            \hline
            \noalign{\smallskip}
No.	& Name			& Alternative		& $J-K_{\rm s}$	& Sp.	& $pEW$(Li {\sc i})       & $pEW$(H$\alpha$)	& SED	& Phot. 	\\
	&			& name   		& [mag]		& type	& [m\AA]	        & [\AA]			& class	& variable	\\
            \noalign{\smallskip}
            \hline
            \noalign{\smallskip}
29	& Mayrit~92149~AB	& [W96] rJ053847--0237	& $1.24\pm0.06$	& M1.0:	& $481\pm8$	        & $-20.9\pm1.2$	& II	& no		\\ % M1.0:, [Li I (Sa08), Halpha, II, X], Wo96,Fr06,He07
36	& Mayrit~203283		& [W96] rJ053831--0235	& $1.16\pm0.04$	& M0.0:	& $479\pm6$	        & $-10.2\pm0.9$	& II	& no		\\ % M0.0:, [Li I (Sa08), Halpha, II, X], Wo96,ZO02a,Fr06,He07
45	& Mayrit~609206		& V505 Ori		& $2.01\pm0.04$	& K7.0	& $431\pm11$	        & $-25.1\pm0.7$	& II	& yes		\\ % K7.0, [Li I (Sa08), Halpha, Em, mIR, X], HM53,Wi89,ZO02a,OvL04
61	& Mayrit~30241		& [HHM2007] 687		& $1.28\pm0.05$	& ...	& ...			& ...			& II	& no		\\ % [X, Ks excess], Ca07b 
72	& Mayrit~521199		& TX Ori		& $1.46\pm0.04$	& K4	& ...			& --16.6		& II	& yes		\\ % K4 [Halpha, Ca II, mIR, X, Si], HM53,HR72,OvL04,He07
75	& Mayrit~622103		& BG Ori		& $1.30\pm0.04$	& M0.5:	& $480\pm7$	        &   $-40\pm3$		& II	& yes		\\ % M0.5:, [Li I (Sa08), Halpha, II, X], HM53,Ca06,Fr06,He07 
79	& Mayrit~203260		& Haro 5--11		& $1.19\pm0.04$	& M2.0:	& $342\pm2$	        &  $-198\pm12$		& II	& no		\\ % M2.0:, [Li I (Sa08), Halpha, II], Wi89,WB04,Ca06,He07 
80	& Mayrit~497054		& V509 Ori		& $1.26\pm0.03$	& M0.5:	& $263\pm4$	        & $-25.8\pm0.8$	& II	& yes		\\ % M0.5:, [Li I (Sa08), Halpha, II, X]. Wi89,Ca06,Fr06,He07
            \hline
         \end{tabular}}
\tablefoot{\tablefoottext{a}{Spectral types and Li~{\sc i} and H$\alpha$ pseudo-equivalent
widths are from Zapatero Osorio et~al. (2002) and Sacco et~al. (2008).
The colon after the spectral type denotes a estimation based on photometry.}}
   \end{table}