\begin{table}%t4
\caption {Derived stellar parameters (December 2004).
\label{tab:param} }
\small
%\centerline
 {\begin{tabular}{lcrcccrrccl}
\hline\hline
\noalign {\smallskip}
 ~~star & spectrum & H$\alpha^1$& $V$ & $B-V$ & $A_{\rm V}$ & 
$T$ (K) &B.C.$^2$& $M_{\rm bol}$ $^3$~ & log~$L/L_{\odot}$ & phase$^4$ \\
\noalign {\smallskip}
\hline
\noalign {\medskip}
GR290  &Oe (WN11)&$-$120~ &17.18 &$-$0.09 & 0.68&
  30~000~  &$-$3.2 & $-11.5~$ & 6.5~     &  min  \\
Var A  & F--G   &$-$35~ &18.60 & +0.88  &(0.7)&
   6~500~  &$-$0.3 & ~$-7.2^5$ & 4.8    &  min  \\
Var B  & Be     &$-$310~ &17.50 &$-$0.15 & 0.37&
            &$-$2.0 & $-9.7$ & 5.8~     &  min  \\
Var C  & B[e]   &$-$49~ &16.40 & +0.10  & 0.6 & 
            &$-$1.0 & ~$-10.0~$ & 5.9~     &  post max \\ 
\noalign {\smallskip}
\hline 
\end{tabular}}
\par
\smallskip
% 
\par
$^1$ Equivalent width of the H$\alpha$ emission line in \AA.~~ 
$^2$ Adopted bolometric correction. See A. N. Cox, Allen's  
Astrophysical Quantities (2000). ~~
$^3$~Assuming for M~33 $m-M = 24.8$ (\citealt{Kim02}). ~~
$^4$~Photometric phase. ~~ 
$^5$~Value referred to the optical spectral component (Fig.~\ref{fig:varased}). 
The star should be subject to a $\sim$3$^{\rm m}$ obscuration 
in the visual due to the presence of a dusty envelope that 
is responsible for the strong mid-infared emission found
by \citet{Hump87}. 
\par
\end{table}