All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{Ha281_f1.ps}\end{figure}$ Figure 1: Top: phase-folded light curve and best-fit transit curve for OGLE-TR-122. Bottom: radial velocity measurements and orbital solution.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{Ha281_f2.ps}\end{figure}$ Figure 2: Illustration of the different constraints on the primary of OGLE-TR-122 compared to stellar evolution models from Girardi et al. (2002) with Z=0.02 for ages 0, 1, 2, 3, 5, 10 and 15 Gyr (thin lines). Long-dashed lines show the contraints from V_T/R (related to the transit duration), short-dashed lines from $T_{\rm eff}$ , dash-and-dot lines from $\log g$ . Dotted lines shows the isoradius lines corresponding to pseudo-synchronised rotation. In each case the lines show the central value and $\pm$ 1-sigma interval.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{Ha281_f3.ps}\end{figure}$ Figure 3: Mass vs. radius for observed low-mass stars and giant planets and theoretical isochrones. Eclipsing binaries are shown as circles (OGLE-TR-122b in black), interferometric data as open triangles. Baraffe et al. (1998) isochrones for masses from $0.06~M_\odot$ to $1.4~M_\odot$ are plotted for 5 Gyr (solid) and 0.1 Gyr (dash-dotted). Dashed lines represent the Baraffe et al. (2003) CON models for masses for 0.5, 1 and 5 Gyr, from top to bottom.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{Ha281_f1.ps}\end{figure}$	Figure 1: Top: phase-folded light curve and best-fit transit curve for OGLE-TR-122. Bottom: radial velocity measurements and orbital solution.
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