\begin{table}%t3
\caption{Influence of the limb-darkening parameter~$\alpha$ on the best-fit diameter and the
associated reduced~$\chi^2$ using the whole data set, assuming a~brightness distribution $I (\mu) =
\mu^{\alpha}$ with $\mu = \cos \theta$ the cosine of the azimuth of a~surface element of the star
\citep{Hestroffer97}. The visibility deficit measured at short baselines~(S1--S2) with respect to
the best-fit model is given in the last column, showing a~weak dependence on the limb-darkening
model.} \label{tab:ld} 
%\centering
\small
\begin{tabular}{cccc}
\hline \hline 
\noalign{\smallskip}
           & Best-fit                & $\chi^2_r$ & $\Delta V^2$
\\              $\alpha$ & $\theta_{\rm LD}$ (mas) & (all data) & (S1--S2)
\\ \hline          0.0   & $3.217 \pm 0.013$       &    3.36    & 1.88\%
\\                 0.1   & $3.264 \pm 0.013$       &    3.14    & 1.83\%
\\                 0.2   & $3.310 \pm 0.012$       &    2.96    & 1.78\%
\\                 0.3   & $3.356 \pm 0.012$       &    2.82    & 1.73\%
\\                 0.4   & $3.402 \pm 0.011$       &    2.71    & 1.67\%
\\                 0.5   & $3.447 \pm 0.011$       &    2.64    & 1.62\%
\\                 0.6   & $3.491 \pm 0.011$       &    2.61    & 1.58\%
\\                 0.7   & $3.536 \pm 0.012$       &    2.60    & 1.53\%
\\                 0.8   & $3.579 \pm 0.012$       &    2.62    & 1.49\%
\\                 0.9   & $3.623 \pm 0.012$       &    2.66    & 1.44\%
\\ \hline
\end{tabular}
\end{table}