\begin{table}%t6
\caption{\label{compWW}Comparison of our results (NGBR) with the light-curves solutions of Wyithe \& Wilson (\cite{WW01, WW02}, WW01, WW02) and Graczyk (2003, dG03).}            
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%\centering
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\begin{tabular}{c c c c c c c c c c c}  
\hline\hline \noalign{\smallskip}
Object & Ref. & Model & $q$ & $R_{\rm P}/a$ & $R_{\rm S}/a$  & 
$i (\degr)$ & $e$ & $(L_{\rm S}/L_{\rm P})_{I}$ & $F_{e}$ & $l_{3,I}$\\  
\hline
4 117831 & NGBR & d  & $0.981\pm0.013$      & $0.261\pm0.008$ & $0.287\pm0.008$ & $78.2\pm0.4$ & $0	       $ & $1.175$ & $0.599$ & $0$\\  
	 & WW02 & sd & $0.157\pm0.054$      & $0.357\pm0.032$ & $0.209\pm0.021$ & $77.9\pm2.1$ & $0.049\pm0.019$ & $0.372$ & $0.853$ & $0$\\
4 163552 & NGBR & d  & $0.952\pm0.015$      & $0.339\pm0.011$ & $0.305\pm0.010$ & $80.9\pm0.2$ & $0	       $ & $0.798$ & $0.797$ & $0.119\pm0.006$ \\ 
	 & dG03 & d  & $0.98\pm0.09  $      & $0.338\pm0.006$ & $0.326\pm0.008$ & $85.4\pm0.9$ & $0	       $ & $0.951$ & $0.895$ & $0.263\pm0.007$\\ 
	 & WW02 & sd & $0.207\pm0.010$      & $0.383\pm0.004$ & $0.234\pm0.003$ & $82.8\pm0.7$ & $0.004\pm0.002$ & $0.397$ & $1.051$ & $0$\\  
4 175333 & NGBR & d  & $0.781\pm0.014$      & $0.237\pm0.008$ & $0.203\pm0.007$ & $80.4\pm0.5$ & $0.022\pm0.007$ & $0.582$ & $0.675$ & $0$\\ 
	 & WW01 & d  & 1.0		    & $0.253\pm0.009$ & $0.143\pm0.007$ & $85.0\pm1.5$ & $0.012\pm0.003$ & $	 $ & $1.080$ & $0$\\
5 016658 & NGBR & d  & $0.889\pm0.011$      & $0.320\pm0.011$ & $0.255\pm0.010$ & $80.3\pm0.2$ & $0	       $ & $0.609$ & $0.798$ & $0$\\ 
	 & WW01 & d  & 1.0		    & $0.345\pm0.007$ & $0.200\pm0.004$ & $85.7\pm1.3$ & $0.002\pm0.002$ & $	 $ & $1.175$ & $0$\\
5 038089 & NGBR & d  & $0.899\pm0.011$      & $0.273\pm0.004$ & $0.226\pm0.003$ & $77.1\pm0.2$ & $0	       $ & $0.693$ & $0.609$ & $0$\\  
	 & dG03 & d  & $1.12 \ ^{\rm a}$ & $0.246\pm0.009$ & $0.255\pm0.007$ & $76.8\pm1.9$ & $0	       $ & $1.053$ & $0.554$ & $0$\\
5 196565 & NGBR & d  & $0.803\pm0.007$      & $0.200\pm0.005$ & $0.150\pm0.005$ & $83.5\pm0.2$ & $0.138\pm0.006$ & $0.43 $ & $0.789$ & $0$\\
	 & WW01 & d  & 1.0		    & $0.204\pm0.006$ & $0.116\pm0.003$ & $88.7\pm2.5$ & $0.085\pm0.002$ & $	 $ & $1.282$ & $0$\\
5 266015 & NGBR & sd & $0.441\pm0.005$      & $0.332\pm0.005$ & $0.310\pm0.005$ & $78.5\pm0.1$ & $0	       $ & $0.494$ & $0.714$ & $0$\\ 
	 & WW02 & sd & $1.014\pm0.051$      & $0.183\pm0.003$ & $0.357\pm0.004$ & $80.8\pm0.4$ & $0.000\pm0.002$ & $2.564$ & $1.039$ & $0$\\
5 266131 & NGBR & d  & $0.864\pm0.013$      & $0.281\pm0.010$ & $0.242\pm0.009$ & $83.5\pm0.2$ & $0.042\pm0.001$ & $0.647$ & $0.847$ & $0$\\  
	 & WW01 & d  & 1.0		    & $0.332\pm0.008$ & $0.216\pm0.009$ & $85.1\pm1.5$ & $0.003\pm0.003$ & $	 $ & $1.071$ & $0$\\
5 283079 & NGBR & d  & $1.003\pm0.013$      & $0.243\pm0.007$ & $0.242\pm0.007$ & $87.7\pm0.3$ & $0	       $ & $0.987$ & $0.918$ & $0$\\
         & WW01 & d  & 1.0		    & $0.272\pm0.006$ & $0.233\pm0.007$ & $88.5\pm1.8$ & $0.001\pm0.001$ & $	 $ & $1.028$ & $0$\\
\hline		   
\end{tabular}
\tablefoot {The following parameters are listed: model of the system, mass ratio, relative radii, inclination, eccentricity, $I$~luminosity ratio, eclipse parameter (see Eq.~(2) in WW01) and third light (normalized to total flux at phase~0.25). \\
\tablefoottext{a}{From HHH03.}}\vspace*{-1.5mm}
\end{table}