All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{2441f1a.ps}\hspace*{2mm} \includegraphics[angle=-90,width=8.4cm,clip]{2441f1b.ps} \end{figure}$ Figure 1: Least square fits of the projected separation ( left) and of the position angle ( right) of the GG Tau A binary. The data are taken from Table 3. Analysis similar to that of R96.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=8cm]{2441f2a}\hfil \includegraphics[angle=-90,origin=br,width=8.8cm]{2441f2b} }\end{figure}$ Figure 2: Variations of the fitted orbital elements (a,e) of the central binary as a function of the observational parameters. The left plot is a greyscale map of the eccentricity e for d=140 pc, as a function of ${\rm d}p/{\rm d}t$ and ${\rm d}\psi /{\rm d}t$ . The point quoted "R96'' is the R96 value, the "McC02'' point corresponds to MC02 (with its error box, 1 $\sigma$ ), and the "B03'' point corresponds to this work. The right plot shows the zone in (a,e) space corresponding to the error box (1 $\sigma$ ) around the "B03'' point, for three different values of d. The grey shaded area is the total error box in (a,e) space if we let all parameters vary within their error boxes. The two points superimposed (B03, McC02) have the same meaning as in the left plot, and hold for d=140 pc.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{2441f3} \end{figure}$ Figure 3: Approximate radius of the inner edge of the circumbinary disk as computed with HJS integrations, in units of the semi-major axis a of the binary, for various values of e, and $\mu =M_2/(M_1+M_2)=0.467$ corresponding to GG Tau A, taken from White et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{2441f4.eps} \end{figure}$ Figure 4: Comparison of the error boxes for the orbit of GG Tau A in (a,e) space deduced from astrometry (dark grey) and circumbinary disk dynamics (light grey). The conventions for this plot are the same as for the right plot of Fig. 2, except that the distance d has been fixed here to 140 pc for clarity. The box outlined in black is the error box for a and e we derive from the fit of the astrometric data if we let ${\rm d}p/{\rm d}t$ and ${\rm d}\psi /{\rm d}t$ vary within their error bars ( $1 \sigma$ coming from the astrometric data). The dark grey surrounding zone is the one we derive if we take into account the uncertainties on all the other parameters. The light grey band is the compatibility zone with the observed location of the inner edge of the disk. It is computed assuming that the location of the inner edge is known with $\pm$ 5 AU accuracy, but also taking a $\sim$ $2\%$ uncertainty on the theoretical edge locations shown in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{F5A.eps} \end{figure}$ Figure 5: Same as Fig. 4, but now the error bars on ${\rm d}p/{\rm d}t$ , ${\rm d}\psi /{\rm d}t$ , and on the location of the observed inner edge of the circumbinary disk have been increased by a factor of 3. There is now an intersection zone between the two boxes (outlined in white).
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{F6A.eps} \end{figure}$ Figure 6: Same as Fig. 5 ( $3 \sigma$ errors on astrometric data), but now the errors on the measurement of the inclination $\lambda$ ( left plot) and of the position angle $\phi$ ( right plot) of the circumbinary disk are enlarged by a factor of 3 with respect to the values of GDS99, setting them to $\pm$ $3\hbox {$^\circ $ }$ and $\pm$ $6\hbox {$^\circ $ }$ respectively. This shows that the astrometric errors are the dominant ones.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=0.7\columnwidth]{2441fA1} }\end{figure}$ Figure A.1: Projection of the circumbinary disk (grey ring) and of the GG Tau A binary (black spheres) onto the plane of the sky, showing the definition of the vectors ( $\vec{I},\vec{J}$ ), the position angles $\psi$ and $\phi$ , and the projected separation p. The disk itself is inclined by oriented angle $\lambda$ with respect to the plane of the sky.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{2441f1a.ps}\hspace*{2mm} \includegraphics[angle=-90,width=8.4cm,clip]{2441f1b.ps} \end{figure}$	Figure 1: Least square fits of the projected separation ( left) and of the position angle ( right) of the GG Tau A binary. The data are taken from Table 3. Analysis similar to that of R96.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{2441f3} \end{figure}$	Figure 3: Approximate radius of the inner edge of the circumbinary disk as computed with HJS integrations, in units of the semi-major axis a of the binary, for various values of e, and $\mu =M_2/(M_1+M_2)=0.467$ corresponding to GG Tau A, taken from White et al. (1999).
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$\begin{figure} \par\includegraphics[width=8.8cm]{F5A.eps} \end{figure}$	Figure 5: Same as Fig. 4, but now the error bars on ${\rm d}p/{\rm d}t$ , ${\rm d}\psi /{\rm d}t$ , and on the location of the observed inner edge of the circumbinary disk have been increased by a factor of 3. There is now an intersection zone between the two boxes (outlined in white).
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