$a$ (km) & $2.548 \pm 0.015$ & 1$\sigma$ & O06\
$(L_{\rm P}, B_{\rm P})$ (deg.) & $(329.6, -62.3) \pm (12 \times 4)^g$ & 3$\sigma$ & This work\
$P_{\rm orb}$ (h) & $17.45763 \pm 0.00004^h$ & 3$\sigma$ & This work\
$L_0$ (deg.) & $40 \pm 5^h$ & 3$\sigma$ & This work\
$e$ & $\le 0.006$ & 3$\sigma$ & O06\
$\Delta M_d$ (deg/yr$^2$) & $-0.65 \pm 0.16$ & 3$\sigma$ & This work\
$\dot{P}_{\rm orb}$ (h/yr) & $0.00013 \pm 0.00003 $ & 3$\sigma$ & This work\
$\dot{a}$ (cm/yr) & $1.2 \pm 0.3$ & 3$\sigma$ & This work\

References: O06 (Ostro et al., 2006)\
$^a$ The range of high solar phase angles covered by the observations did not allow to determine the $G$ parameter. We assumed the mean $G$ value for S-complex asteroids (Warner et al., 2009).\
$^b$ Derived from the primary shape model by O06 and for the average observed aspect. See text for details.\
$^c$ The formal best-fit value is 1.1.\
$^d$ This is a ratio of the cross-section equivalent diameters for the average observed aspect of 27 deg. See text for details.\
$^e$ Derived using the shape model of the secondary from O06 rescaled by 130%. See text for details.\
$^f$ 