\begin{table}%t13
%\centering
\par
\caption{Photometric solutions for VZ~Hya from the WD code
adopting linear limb darkening coefficients by van Hamme (\cite{vh93});
see Table~\ref{tab:vzhya_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 6650~K.}\label{tab:vzhya_wd_vh}
\small
\begin{tabular}{lrrrr} \hline
\hline                     &     $y$    &       $b$  &       $v$  &   $u$\\                   
\hline            
$i$ ~ (\degr)       &  88.90     &   88.92    &   88.95    &  88.98\\           
                     & $\pm$2    &  $\pm$1   &  $\pm$2   & $\pm$2\\                 
\par
$\Omega_{\rm p}$           &   9.649    &    9.666   &    9.639   &   9.668\\  
                     &  $\pm$8   &   $\pm$7  &   $\pm$8  &  $\pm$11\\                
\par
$\Omega_{\rm s}$           &  10.349    &   10.329   &   10.355   &  10.343\\  
                     &  $\pm$8   &   $\pm$7  &   $\pm $$8$  &  $\pm$11\\                
\par
$r_{\rm p}$                &  0.1144    &   0.1142   &   0.1146   &  0.1142\\                 
\par
$r_{\rm s}$                &  0.0969    &   0.0971   &   0.0968   &  0.0969\\                 
\par
$k$                  &  0.847     &   0.850    &   0.845    &  0.849\\                  
\par
$r_{\rm p} + r_{\rm s}$          &  0.2113    &   0.2113   &   0.2114   &  0.2111\\                 
\par
$T_{{\rm eff},s}$    &  6272      &   6252     &   6229     &  6182\\
                     &$\pm$2     & $\pm$1    &$\pm$$  2$    &$\pm$3\\
\par
$L_{\rm s}/L_{\rm p}$            &  0.5686    &    0.5464  &   0.5125   &  0.5347 \\
\par
$\sigma$ ~ (mag.)   &  0.0046    &    0.0039  &   0.0043   &  0.0068\\
\hline
\end{tabular}
\end{table}