RMS residuals of the two best local minima obtained using the spherical shapes (with $\Delta M_d$ of $-0.65$ and $-1.3$ deg/yr$^2$) were 0.0307 and 0.0320 mag, respectively. The fits improved to 0.0251 and 0.0266 mag using the elipsoidal shapes. The fit is significanly poorer for the latter solution. The former solution provides a satisfactory fit to the data and it is accepted as real solution for the binary asteroid parameters.

For 2001 SL9, the RMS residuals of the five best local minima obtained using the spherical shapes (with $\Delta M_d$ of 2.8, 5.2, 7.6, 4.0 and 0.5 deg/yr$^2$) were 0.0238. 0.0238, 0.0245, 0.0246 and 0.0248 mag, respectively. The fits improved to 0.0236, 0.0236, 0.0243, 0.0245 and 0.0245 mag using the elipsoidal shapes; the marginal improvement is due to that the secondary of 2001 SL9 is not prominently elongated. The first two solutions provide satisfactory fit to the data; one of them is a real solution for the binary asteroid parameters, but we cannot resolve this ambiguity with the available data. The other three solutions with the higher RMS residuals provide significantly poorer fits to the data and they do not appear real. Figures \[additionalM0KW4\] and \[additionalM0SL9\] show the quadratic drift 