over all sessions. Its 1$\sigma$ uncertainty was computed using the uncertainties of the dimensions of the primary from Ostro et al.

$D_{1,{\rm V}}$ was taken from Table 2 of Ostro et al.

$D_{2,{\rm V}}$ was derived using the shape model of the secondary by Ostro et al. (2006), rescaled to 130% of its original size to match mutual events’ depths from our data (see below). Its 1$\sigma$ uncertainty is a formal value taken from Table 2 of Ostro et al. (2006), but the real uncertainty may be higher because of uncertainties of the secondary radar shape model (Lance Benner, personal communication).

In the last part of Table \[tablePropKW4\], we summarize the parameters of the mutual orbit of the binary components. $a$ is the semimajor axis, $L_{\rm P}, B_{\rm P}$ are the ecliptic coordinates of the orbital pole in the equinox J2000, $L_0$ is the mean length of the secondary (i.e., the sum of angular distance from the ascending node and the length of the ascending node) for epoch JD 2455305.0, $e$ is the orbit eccentricity (only the upper limit was derived), and $\Delta M_d$ is the quadratic drift in mean anomaly. Since the orbital period $P_{\rm orb}$ is changing in 