$17.53 \pm 0.12$ h ($3\sigma$; this includes also a synodic-sidereal difference uncertainty). This agrees with the mutual orbit period, within the error bar. Considering that all the observed secondary lightcurve minima coincide with or lie close to the mutual events —small differences may be due to a phase effect or secondary libration—, it is very likely that the secondary is in synchronous rotation. We therefore assume that $P_2$ is equal to the orbital period (see Table \[tablePropKW4\]).

$(A_1 B_1)^{1/2}/C_1$ is a ratio between the mean equatorial and the polar axes of the primary. $A_i/B_i$ is a ratio between the equatorial axes of the $i$-th component (equatorial elongation). $\rho_1 = \rho_2$ are the bulk densities of the two components, which we assumed to be the same in our modeling.

Most of the quantities were parameters of our model given in Section \[NumModel\] and we derived them from our observations.

The cross-section and volume equivalent diameters of the primary were derived using the shape model of the primary from Ostro et al. (2006). Assuming its rotational pole is the same as the mutual orbital pole (see below), we computed its rotationally averaged cross-section for each lightcurve session and presented the mean value 