All Tables

Table 1: All measured squared visibilities of the 2002 run, grouped per filter. PA is the position angle (counted from North to East) of the interferometric baseline projected onto the sky.
Table 2: The stellar parameters from Decin et al. (2003b) and references therein, and the limits of the grid in which we searched for an optimal fit to the interferometric data ( $\xi _{\rm {t}}$ is the microturbulent velocity).
Table 3: Uniform disk (UD) angular diameters derived by fitting Eq. (4) to the narrow-band data taken in respective filters or altogether. The third column gives the reduced chi-square of the fit (chi-square per degree of freedom), denoted $\chi ^{2}_{{\rm r}}$ .
Table 4: Angular diameter determinations with plane-parallel and spherical MARCS models. Only a very small improvement on the chi-square value can be achieved by increasing the extension of the atmosphere of the model (SPH model with $\log{g} = 1.0$ ), and such a low surface gravity cannot be reconciled with the spectral features.
Table 5: All measured squared visibilities of the 2001 run, grouped per filter.
Table 6: Best-fit parameters with formal errors for the binary model.
Table 7: Primary and companion stellar parameters for age-limits².