All Figures

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[width=8cm]{behr01tl.eps}... ...r01bl.eps} & \includegraphics[width=8cm]{behr01br.eps}\end{tabular} \end{figure}$ Figure 1: Phased light curves for all observations for three of the four minor planets of this study - see Fig. 3 for the last one. E is the epoch in UTC "onboard'' the asteroid corresponding to the origin of the phase plot. T is the adopted synodic period for folding the observations. The horizontal axis represents the time of the observations, corrected for light travel, since E, in units of T, modulo 1; the leftmost quarter is repeated at right. The vertical axis represents the magnitude, usually unfiltered, based on the R-band of the USNO-A2.0 star catalogue (Monet 1998), from which the V-magnitude from the ephemeris is subtracted - used photometric parameters are tabulated in Table 1. One can easily notice some changes in the profile of the mutual phenomenons during the months following the discoveries, due to the evolution of the Sun-Asteroid-Earth configuration.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm]{behr02xx.eps} \end{figure}$ Figure 2: This plots show the theoretical light curve of a binary system consisting of two equal sized prolate bodies ( $10\times 7\times 7$ km) separated by 50 km. The orbit is circular and seen edge-on. Top: the rotational light curve is the component due to the rotation of the prolate bodies, characterized by the amplitude $\Delta m$ . Middle: the eclipsing light curve is flat outside eclipses and exhibits V-shape features with an amplitude of $\Delta e$ (0.75 mag in case of total eclipses) and an eclipse duration $\Delta {\phi }$ . Bottom: the total light curve is the combination of the rotational and eclipsing light curves.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm]{behr03tx.eps}\\ [2mm] \par\incl... ...hr03mx.eps}\\ [2mm] \par\includegraphics[width=8.2cm]{behr03bx.eps} \end{figure}$ Figure 3: Phased light curves for (4492) Debussy. See explanations in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{behr04xx.eps} \end{figure}$ Figure 4: Polar plot of the intrinsic variations of the flux (linear scale) of the asteroid Berna during one rotation of the system - radial coordinate. The angular coordinate is the phase $\frac{t-E}{T}$ . The ellipsoid is the computed light curve from the observations out of the eclipses. The occultation feature shows strongly compared with a traditional light curve.
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In the text

$\begin{figure} \par\begin{tabular}{c} \includegraphics[width=7.2cm,clip]{behr05xx.eps} % \end{tabular} \end{figure}$ Figure 5: Geometry and symbol definitions used in the model described in Sect. 3.1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{behr06xx.eps} \end{figure}$ Figure 6: The completed distribution of the $4.5\times 10^2$ asteroids in our survey, as a function of their H absolute magnitude parameter. For most objects of this survey, 9<H<15roughly corresponding to diameters from 10 to 50 ${\rm km}$ . A few near Earth objects with H>17 and some big main belt asteroids with H<7 are also present.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm]{behr03tx.eps}\\ [2mm] \par\incl... ...hr03mx.eps}\\ [2mm] \par\includegraphics[width=8.2cm]{behr03bx.eps} \end{figure}$	Figure 3: Phased light curves for (4492) Debussy. See explanations in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.5cm]{behr04xx.eps} \end{figure}$	Figure 4: Polar plot of the intrinsic variations of the flux (linear scale) of the asteroid Berna during one rotation of the system - radial coordinate. The angular coordinate is the phase $\frac{t-E}{T}$ . The ellipsoid is the computed light curve from the observations out of the eclipses. The occultation feature shows strongly compared with a traditional light curve.
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$\begin{figure} \par\begin{tabular}{c} \includegraphics[width=7.2cm,clip]{behr05xx.eps} % \end{tabular} \end{figure}$	Figure 5: Geometry and symbol definitions used in the model described in Sect. 3.1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{behr06xx.eps} \end{figure}$	Figure 6: The completed distribution of the $4.5\times 10^2$ asteroids in our survey, as a function of their H absolute magnitude parameter. For most objects of this survey, 9<H<15roughly corresponding to diameters from 10 to 50 ${\rm km}$ . A few near Earth objects with H>17 and some big main belt asteroids with H<7 are also present.
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