Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{1268fig1.ps} \end{figure}$ Figure 1: Top: OGLE-TR-56 de-trended differential light curves. Open squares and filled circles show, respectively, the VLT and Magellan data. Bottom: VLT (squares) and Magellan (circles) light curves binned by a factor of 23 and 14 respectively. The blue light curve corresponds to OGLE-TR-56, and the black and grey triangles to reference stars. Models with and without the best fit secondary transit are shown as horizontal lines. At phase 0.65 (red squares), we indicate the final values and uncertainties on the fit eclipse depth as well as the out-of-eclipse flux.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1268fig2.eps} \end{figure}$ Figure 2: Normalized flux histograms for the portions of the combined VLT and Magellan data in-eclipse (dotted line) and out of eclipse (solid line). The bin width is 0.000363, coincident with the detected transit depth.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{1268fig3.ps} \end{figure}$ Figure 3: The top panel shows the derived model eclipse depth versus assumed central transit phase, with the plot approximately covering the eclipse duration. Phase 0.5 corresponds to a circular orbit. The central phase is not well constrained within approximately 0.01, with similar transit depths found over a phase range of 0.49 to 0.515, but the transit depth falls off rapidly for central phases outside that range. The best-fit value (black dot at phase 0.497) is indicated in the bottom contour plot, along with the value assuming a circular orbit (cross). The joint confidence contours of the best fit are also plotted in the bottom figure for the 68.3%, 95.5% and 99.7% levels.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1268fig4.eps} \end{figure}$ Figure 4: z'-band secondary eclipse depth of OGLE-TR-56b as a function of the reradiation factor $\it f$ for albedos $A_{\rm B}$ = 0, 0.15 and 0.3 (left-side), and as a function of the planet's temperature (right-side), in the case of reflected light (dashed line), or from thermal emission assuming the planet emits as a black-body (solid line). The (red) filled and open squares indicate the expected model depth of the transit with and without TiO/VO (Hubeny et al. 2003). Our measured depth is the black dot.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1268fig2.eps} \end{figure}$	Figure 2: Normalized flux histograms for the portions of the combined VLT and Magellan data in-eclipse (dotted line) and out of eclipse (solid line). The bin width is 0.000363, coincident with the detected transit depth.
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