Table 3: 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 (Hestroffer 1997). 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.
  Best-fit $\chi^2_r$ $\Delta V^2$
$\alpha $ $\theta_{\rm LD}$ (mas) (all data) (S1-S2)
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%

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