All Figures

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{0348fig1.ps}\end{figure}$ Figure 1: ADONIS images of the eclipsing PMS binary RX J0529.4+0041A (upper-right star) and its companion in the J, H, and K bands. North is down, East to the left. The three upper images show the eclipsing system at maximum brightness, whereas the lower ones are close to the primary minimum. In the upper and lower middle frames the apertures used for measuring each component and the corresponding sky are also drawn.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0348fig2.ps}\end{figure}$ Figure 2: Example of the bisector method used to determine the time of a minimum. The vertical solid line represents the bisector for primary eclipse data in the H band, whereas the dashed line shows the bisector on a ten times expanded scale.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0348fig3.ps} \end{figure}$ Figure 3: Observed minus calculated times of minima for the eclipsing system RX J0529.4+0041A. Primary and secondary minima are represented with filled and open circles respectively. The orbital period appears to be constant within the errors.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0348fig4.ps}\end{figure}$ Figure 4: $\it JHK$ light-curve solution of RX J0529.4+0041A with 2 spots on the primary component, at 0 $^{\circ }$ , -25 $^{\circ }$ , and 180 $^{\circ }$ , 42 $^{\circ }$ , of 20 $^{\circ }$ and 14 $^{\circ }$ radius, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0348fig5.ps}\end{figure}$ Figure 5: Normalized $\it UBVRI$ light-curves in proximity of the primary minimum as obtained from measurements on OIG images, inclusive of the "third light'' (light triangles), and after correction for the "third-light'' contribution (black squares), using the corresponding measurements for component B given in Table 2, as outlined in the Appendix. The corrected data match fairly well the synthetic light-curves (solid curves) calculated from solution of the J, H, and K bands only.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0348fig6.ps}\end{figure}$ Figure 6: Best-fit, simultaneous solution of the differential B, V, J, H, and K light-curves of RX J0529.4+0041A with respect to the visual companion, used as a comparison star. B and V differential magnitudes have been corrected for the third light contribution, following the method exposed in the Appendix. Light symbols represent the photoelectric data obtained at Serra La Nave (Covino et al. 2000), black dots indicate the CCD data from TNG.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0348fig7.ps}\end{figure}$ Figure 7: $\chi$ -square maps for different pairs of light-curve parameters, adopting for the primary component the $T_{\rm eff}$ of 5200 K.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0348fig8a.ps}\vspace*{3mm} \includegraphics[width=8.8cm,clip]{0348fig8b.ps}\end{figure}$ Figure 8: Upper panel: spectral energy distribution (SED) of RX J0529.4+0041 A, as deduced from observed $\it UBV(RI)_{\rm C} JHK$ fluxes (dots), compared with calculated ones (triangles), obtained from a combination of two synthetic Next-Generation spectra with effective temperatures of 5200 K and 4200 K (continuous thin lines). Lower panel: comparison between observed (dots) and computed (squares) SED of RX J0529.4+0041 B, superimposed on the synthetic Next-Generation spectrum (thin continuous line) for $T_{\rm eff}=4400$ K.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0348fig9.ps}\end{figure}$ Figure 9: Comparison on the HR diagramme of the positions of the eclipsing components of RX J0529.4+0041A (black diamonds) with different sets of PMS evolutionary tracks and isochrones from different authors. The position of the third component, RX J0529.4+0041B, is marked by the triangle. Tracks corresponding to different masses (solid lines) are labelled in solar units and isochrones (dashed lines) at different ages are marked in Myrs. Additionally, the positions of the components of the eclipsing system V1174 Ori (Stassun et al. 2004; small, open diamonds) and of the spectro-astrometric binary NTT 045251+3016 (Steffen et al. 2001; $\times$ symbols) are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0348fig2.ps}\end{figure}$	Figure 2: Example of the bisector method used to determine the time of a minimum. The vertical solid line represents the bisector for primary eclipse data in the H band, whereas the dashed line shows the bisector on a ten times expanded scale.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0348fig3.ps} \end{figure}$	Figure 3: Observed minus calculated times of minima for the eclipsing system RX J0529.4+0041A. Primary and secondary minima are represented with filled and open circles respectively. The orbital period appears to be constant within the errors.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0348fig4.ps}\end{figure}$	Figure 4: $\it JHK$ light-curve solution of RX J0529.4+0041A with 2 spots on the primary component, at 0 $^{\circ }$ , -25 $^{\circ }$ , and 180 $^{\circ }$ , 42 $^{\circ }$ , of 20 $^{\circ }$ and 14 $^{\circ }$ radius, respectively.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0348fig7.ps}\end{figure}$	Figure 7: $\chi$ -square maps for different pairs of light-curve parameters, adopting for the primary component the $T_{\rm eff}$ of 5200 K.
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