\pm 0.036$ h, semimajor axis $a = 2548 \pm 15$ m, eccentricity $e = 0.0004 \pm 0.0019$, pole direction in ecliptic coordinates: $L_{\rm P} = 325.8 \pm 3.5$ deg, $B_{\rm P} = -61.8 \pm 1.2$ deg (uncertainties correspond to $1 \sigma$).

To compare our results with the values from Ostro et al. (2006), we computed $(A_1 B_1)^{1/2}/C_1$ and $a/(A_1 B_1)^{1/2}$ using their DEEVE for the primary and their semimajor axis of the mutual orbit. The result is plotted as a solid point in Fig. \[66391\_20Ba\_a\_PrimA\_Rho\] with $1 \sigma$ error bars.

There is one significant discrepancy between our results and those by Ostro et al. (2006): We obtained a significantly larger secondary-to-primary size ratio. To compare their result with ours, we computed a mean (rotationally averaged) cross-section ratio from the component shapes by Ostro et al. (2006): $(D_{\rm 2,C}/D_{\rm 1,C})_{\rm radar} = 0.34 \pm 0.02$ ($1 \sigma$) at the same mean aspect as our observations (asterocentric latitude of the Phase Angle Bisector, $B_{\rm PAB} = 27$ deg). The value is significantly lower than our $D_{\rm 2,C}/D_{\rm 1,C} = 0.42 \pm 0.03$ ($3 \sigma$).

To look more into the discrepancy between the secondary-to-primary size ratios by Ostro et al. (2006) and by 