\begin{table}%t3
%\scriptsize{
%\begin{center}
\par
\caption{\Ha\ equivalent widths, T Tauri classification, 
spectral types, effective temperatures and distances of the
stars studied as found in the literature and used to calculate the 
stellar luminosities and \IR\ excesses.} 
\label{results}
\par
\begin{tabular}{lcccccccccccccccc}
\par
\hline
\hline\noalign{\smallskip}
%W$_{\lambda}$(\Ha)
\par
Star & {\it EW}(\Ha) &   TTS &  Ref. &  Sp. T. &  Ref. &  $T$  &    \Av & Ref. &  $d$ &
 Ref. &  \Lstar &  $\lambda$$_{\rm IR}$$^{a}$ & \Le  & \multicolumn{2}{c} {\IRe$^{b}$} & co.$^{c}$\\
\par
      & [\AA]  &  &  &  &  & [K]  & & & [pc] & & [\Lsun] & [$\mu$m] & [\Lsun]& o & l & \\\noalign{\smallskip}
\par
\hline
\par
     T Cha &    --   &    w &          1 &         G8 &          1 &       5445 &       1.27 &          C &        140 &          2 &
      1.71 &    3.5 & 0.63 &     0.36 & 0.13  & n  \\
\par
     Sz 68 &   2--7 &    w &          3 &         K2 &       3/4  &       4955 &       1.09 &          C &        150 &          3 &
      4.59 &    3.5 & 1.60  &    0.35 & 0.30  &  y \\
\par
    RU Lup & 216.4 &    c &         5 &      K7-M0 &         6 &       3963 &       0.20 &         6 &        127 &         7 &
      1.27 &    3.5 &  0.68 &     0.53 & 0.48  & n    \\
\par
    EX Lup &   43.3 &    c &         5 &       M0.5 &         5 &       3802 &       ?     &         18  &        125 &         5 &
      0.47 &    3.5 &  0.17 &     0.35 &  --   & n   \\
\par
    Sz 124 &  ~ 1.6 &    w &         5 &         M0 &         5 &       3917 &       0.22 &          C &        125 &         5 &
      0.21 &   3.5 & 0.17   &   0.81 &   --   &  y \\
\par
     ROX 2 & ~ 2.8 &    w &         8 &         M0 &         8 &       3917 &       3.32 &          C &        170 &         8 &
      1.01 &    12.0& 2.23   &   2.20 & 0.91  & y \\
\par
   DoAr 24 &  20.0 &    c &         8 &         K5 &         8 &       4395 &       3.15 &          C &        170 &         8 &
      1.58 &    4.8 & 3.42    &  2.17 & 0.05  &  n \\
\par
  DoAr 24E & ~  5.0 &    w &         8 &         K0 &         8 &       5236 &       5.84 &          C &        170 &         8 &
      8.50 &    3.5 &  3.97   &  0.47 & 0.08  &  y \\
\par
     SR 12 & ~  3.6 &    w &          9 &       M2.5 &         10 &       3428 &       0.46 &          C &        170 &         8 &
      0.91 &    12.0&  2.41   &  2.65 & 1.71$^{s}$ &    y \\
\par
    ROX 31 & ~   3.3 &    w &         8 &         K7 &         8 &       4000 &       4.20 &          C &        170 &         8 &
      0.48 &    4.8 & 0.55    &  1.15 &  0.33  &  y \\
\par
  Wa Oph/4 &  ~ 0.6 &    w &          11 &         K4 &         11 &       4581 &       2.40 &          C &        150 &         11 &
      1.00 &    4.8 &  0.11   &  0.11 &  0.04 &  y \\
\par
  Wa Oph/6 &   35.0 &    c &          11 &         K7 &          12 &       4000 &       1.24 &          C &        150 &          11 &
      0.67 &    4.8 & 0.64   &   0.96 & 0.23  &  n \\
\par
    IX Oph & ~  1.3 &    w &          9 &          G &         13 &       5902 &       2.29 &          C &        125 &         14 &
      2.80 &    3.5 & 0.06   &   0.02 & --  &  n \\
\par
 V1725 Oph &  ~ 6.5 &    w &          15 &       M0.5 &          15 &       3802 &       1.08 &          15 &        225 &          15 &
      0.63 &    4.8 &  0.86  &   1.37 & --  &  n?\\
\par
CoKu Ser G1 & ~ 3.3 &   w &          9 &         K7 &          9 &       4000 &       3.48 &          9 &        350 &         16 &
      0.60 &    4.8 & 2.21   &   3.70 & 2.24  & y  \\
\par
CoKu Ser G7 &~  5.5 &   w &          9 &         M0 &          9 &       3917 &       3.72 &          9 &        350 &         16 &
      0.82 &    4.8 & 20.09   &  24.52 & 0.65  & n? \\
\par
  V536 Aql &   51.8 &    c &        9/3 &         K7 &          3 &       4000 &       1.43 &          C &        200 &          3 &
      0.72 &    4.8 & 1.79   &   2.48 & 0.47  & y \\
\par
   MacC H3 &  11.4 &    c &          9 &         K2 &          4 &       4955 &       0.53 &          C &        845 &         17 &
      1.83 &    7.7 & 3.03   &   1.66 & 0.85  & n \\
\par
\hline
\par
\end{tabular} 
\par
%\end{center}
\par
Notes to Table:
"C'' in the extinction's
reference column indicates we have calculated it for this paper from the
photometry and the spectral type. Otherwise the reference is given. 
\newline
$^a$ Wavelength (in\mum) from where the \IR\ luminosity excess was calculated (to infinite wavelength);
\newline
$^b$ \IRe~=~($L_{\rm IR}$~-~$L_{\rm bb}$)~/~\Lstar; (o) are the excesses calculated over 
the continuous line representing the star,
seen in each graph (Figs.\ \ref{SED1} to\ \ref{SED6}); (l) are the lower limits
obtained for the excesses. 
"s'' indicates the \IR\ excess is over the luminosity of the binary system.  
Details on how each \IR\ excess for individual stars was obtained, 
can be found in Sect. 3;
\newline
$^c$\ If the star is believed to have a companion nearby (y) or not (n),
 according to the literature. "n?'' no companion has been reported but we believe there could be one.
\newline
{
\textit{References:} (1)~\cite{Alcala93}, (2)~\cite{Siebenmorgen00}, (3)~\cite{Geoffray01},
 (4)~Herbig-Bell Catalogue (HBC), (5)~\cite{Appenzeller83},
(6)~\cite{Stempels02}, (7)~\cite{Favata98}, (8)~\cite{Bouvier92}, (9)~\cite{Cohen79},
 (10)~\cite{Rydgren76}, (11)~\cite{Walter86},
(12)~\cite{Chavarria00}, (13)~\cite{Covino92}, (14)~\cite{Reipurth96}, (15)~\cite{Reipurth86},
 (16)~\cite{Brown00}, (17)~\cite{DeZeeuw99}, (18)~\cite{Herbig01}.
}
\end{table}