\begin{table}%t18
%\centering
\par
\caption{Photometric solutions for WZ Oph from the WD code
adopting linear limb darkening coefficients by van Hamme (\cite{vh93});
see Table~\ref{tab:wzoph_ebop_vh}. Gravity darkening exponents of 0.33 and bolometric albedo
coefficients of 0.5 were adopted, as appropriate for convective envelopes.
$T_{{\rm eff},p}$ was assumed to be 6165~K.}\label{tab:wzoph_wd_vh}
\small 
\begin{tabular}{lrrrr} \hline
\hline  &     $y$    &       $b$  &       $v$  &   $u$\\                   
\hline
$i$ ~ (\degr)       &  89.11     &   89.11    &   89.08    &  89.14\\   
                     & $\pm$1    &  $\pm$1   &  $\pm$2   & $\pm$3\\                 
\par
$\Omega_{\rm p}$           &  11.454    &   11.510   &   11.554   &  11.444\\  
                     &  $\pm$11   &   $\pm$15  &   $\pm$14  &  $\pm$32\\                
\par
$\Omega_{\rm s}$           &  11.334    &   11.299   &   11.310   &  11.276\\  
                     &  $\pm$12   &   $\pm$14  &   $\pm$17  &  $\pm$30\\                
\par
$r_{\rm p}$                &  0.0957    &   0.0952   &   0.0948   &  0.0958\\                 
\par
$r_{\rm s}$                &  0.0963    &   0.0967   &   0.0966   &  0.0969\\                 
\par
$k$                  &  1.007     &   1.016    &   1.019    &  1.012\\                  
\par
$r_{\rm p} + r_{\rm s}$          &  0.1920    &   0.1919   &   0.1914   &  0.1927\\                 
\par
$T_{{\rm eff},s}$    &  6149      &   6141     &   6141     &  6121\\
                     &$\pm$2     & $\pm$2    &$\pm$$  3$    &$\pm$5\\
\par
$L_{\rm s}/L_{\rm p}$            &  1.0023    &    1.0126  &   1.0180   &  0.9936 \\
\par
$\sigma$ ~ (mag)   &  0.0053    &    0.0057  &   0.0065   &  0.0104\\
\hline
\end{tabular}            
\end{table}