All Figures

$\begin{figure} \par\includegraphics[width=9cm]{9238_fig1.ps} \end{figure}$ Figure 1: Top: Mercator/MENOPE photometry for the transit of HD 17156b. The best fitting theoretical transit curve is superimposed in red. Bottom: residuals of the fit ( $\rm rms=1.6e{-}3$ ).
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9238_fig2.ps} \end{figure}$ Figure 2: Model fitted using FullTransit on the photometric ( top) and RV ( bottom) data. Bottom left: red triangles = Keck, blue circles = Subaru. Bottom right: zoom on the transit phase. Top: blue triangles = Mercator photometry, green circles = ``Almenara'' photometry.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9238_fig3.ps} \end{figure}$ Figure 3: Mass radius diagram for the known transiting planets with an error bar on the mass and radius smaller than 10% (except GJ 436b). While most of them ( open circles) have a density comparable to or lower than the one of Jupiter, the three massive planets HD 17156b, HD 147506b and XO-3b are much denser, as predicted by theory, while CoRoT-Exo-2b appears to be ``anomalously'' large. The 1-sigma error bars are represented only for the 4 massive planets for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{9238_fig1.ps} \end{figure}$	Figure 1: Top: Mercator/MENOPE photometry for the transit of HD 17156b. The best fitting theoretical transit curve is superimposed in red. Bottom: residuals of the fit ( $\rm rms=1.6e{-}3$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{9238_fig2.ps} \end{figure}$	Figure 2: Model fitted using FullTransit on the photometric ( top) and RV ( bottom) data. Bottom left: red triangles = Keck, blue circles = Subaru. Bottom right: zoom on the transit phase. Top: blue triangles = Mercator photometry, green circles = ``Almenara'' photometry.
Open with DEXTER