All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{2771f1.ps}\end{figure}$ Figure 1: Example of cross-correlation functions from our programme: for an unrotating star ( left), for a rotating star synchronised with the eclipsing companion ( middle) and for a triple-lined spectroscopic binary ( right). In the last case, the third component is the wide depression between the two deeper dips.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2771f2.ps}\end{figure}$ Figure 2: Rotation velocity of the primary vs. period for our sample. The lines show the expected rotation velocity for tidally locked systems with radii of 1 ${R}_\odot$ and 2 ${R}_\odot$ for the primary. For objects at v sin i = 5 km s^-1 (dotted line), the value given is an upper limit. Uncertainties are indicated only when larger than the symbols (an uncertainty of 10% is used for values based on single spectra). Black dots show objects with a precise radial velocity orbits, triangles the detected planets. The three open circles isolated in the lower left are OGLE-TR-97 (triple system), 124 and 131 (suspected false transit detections). For all other objects the rotation velocity is compatible with synchronous rotation.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.7cm,clip]{2771f3a.ps}\hspa... ...space*{2mm} \includegraphics[angle=-90,width=5.7cm,clip]{2771f3h.ps}\end{figure}$ Figure 3: Radial velocity data and orbits for single-lined spectroscopic binaries. The orbital periods and epochs are constrained in combination with the photometric signal. The corresponding parameters are given in Table 1. The measurements uncertainties are smaller than the symbols.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.7cm,clip]{2771f4a.ps}\hspace*{2mm}\includegraphics[angle=-90,width=5.7cm,clip]{2771f4b.ps}\end{figure}$ Figure 4: Radial velocity data and tentative orbital solution for OGLE-TR-123 and OGLE-TR-129. The orbital periods and epochs are constrained in combination with the photometric signal. The corresponding parameters are given in Table 1. The measurements uncertainties are plotted only when larger than the symbols.
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In the text

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics[angle=-90]{2771f5a.ps}\i... ...cs[angle=-90]{2771f5e.ps}\includegraphics[angle=-90]{2771f5f.ps}} % \end{figure}$ Figure 5: Radial velocity data and resulting orbits for double-lined and triple-lined spectroscopic binaries. The transit epoch is derived from the photometric data. The corresponding parameters are given in Table 3. The different components identified in the spectra are identified with different symbols. In all plots the black dots indicate the object undergoing the eclipse at $T_{\rm tr}$ (OGLE). Error bars are comparable to the size of the symbols or smaller. The radial velocity of components witout significant radial velocity changes was fixed to a constant values to allow a better solution for the other components. Note that OGLE-TR-112 is plotted in date instead of phase because of the two different periods.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2771f6.ps}\end{figure}$ Figure 6: Radial velocity data and orbit for the three detected transiting planets. Adapted from Pont et al. (2004); Bouchy et al. (2004); Moutou et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=4.7cm,clip]{2771f7a.ps}\hspa... ...space*{2mm} \includegraphics[angle=-90,width=4.7cm,clip]{2771f7c.ps}\end{figure}$ Figure 7: Radial velocity data for the objects without radial velocity variations in phase with the transit signal. The dotted line indicates the orbit corresponding to a transiting 1 $M_{\rm J}$ planet.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2771f8.ps} % \end{figure}$ Figure 8: Lower limit for the rotation velocity as a function of period for objects without detected signal in the CCF, if they are single stars of spectral type later than F2. Lines as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2771f9.ps}\end{figure}$ Figure 9: Mass-radius relation for low-mass stars and planets. Black dots show the objects in this study with well-determined mass and radius, crosses the objects with higher uncertainties. Diamonds show Jupiter and Saturn, open circles the results of the OGLE bulge fields from Paper I, the hexagons are the three other transiting planets HD 209458 (Brown et al. 2001), OGLE-TR-56 (Konacki et al. 2003a) and TrES-1 (Alonso et al. 2004). The lines show the models of Girardi et al. (2002) for Solar-type stars, for ages 0, 3 and 10 Gyr, and of Baraffe et al. (1998) and Chabrier et al. (2000) for low-mass stars, brown dwarfs and planets for ages 0.5 and 5 Gyr.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2771f10.ps}\end{figure}$ Figure 10: Mass-radius relation for M-dwarfs. Black dots show the objects in this study with well-determined mass and radius, open circles the results of the OGLE bulge fields from Paper I. Triangles are data from equal-mass eclipsing binaries (Ribas 2003; Metcalfe et al. 1996) and crosses from interferometry (Ségransan et al. 2003; Lane et al. 2001). The lines show the models of Baraffe et al. (1998) and Chabrier et al. (2000) for low-mass stars and brown dwarfs for ages 0.5 and 5 Gyr. The vertical line shows the brown dwarf limit. The crossed circle is the position of our tentative solution for OGLE-TR-123.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{2771f11.ps}\end{figure}$ Figure 11: Transit signal-to-noise ratio ( $d/\sigma _{\rm phot} \sqrt {N_{\rm tr}}$ ) as a function of magnitude, for the objects in our sample. The crosses identify the objects without signal in the CCF, for which our measurements do not confirm the presence of a transiting companion. Black dots indicate the objects without significant radial velocity variations. The lines show possible detectability limits according to the discussion in Sect. 5.4.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2771f12.ps}\end{figure}$ Figure 12: Detection probability of a transiting planet in the OGLE Carina survey as a function of orbital period, according to Monte Carlo simulations, for three transit depths: 3 times ( top), 2.5 times ( middle) and 2 times ( bottom) the dispersion of the photometric data. The detection criteria is $d/\sigma _{\rm phot} \sqrt {N_{\rm tra}}>18$ . A $R\sim {R}_{\rm J}$ planet in front of a solar-type star with m_I<16 would be in the lower panel, a $R\sim 1.3 \;{R}_{\rm J}$ planet would be in the upper panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{2771f1.ps}\end{figure}$	Figure 1: Example of cross-correlation functions from our programme: for an unrotating star ( left), for a rotating star synchronised with the eclipsing companion ( middle) and for a triple-lined spectroscopic binary ( right). In the last case, the third component is the wide depression between the two deeper dips.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.7cm,clip]{2771f3a.ps}\hspa... ...space*{2mm} \includegraphics[angle=-90,width=5.7cm,clip]{2771f3h.ps}\end{figure}$	Figure 3: Radial velocity data and orbits for single-lined spectroscopic binaries. The orbital periods and epochs are constrained in combination with the photometric signal. The corresponding parameters are given in Table 1. The measurements uncertainties are smaller than the symbols.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.7cm,clip]{2771f4a.ps}\hspace*{2mm}\includegraphics[angle=-90,width=5.7cm,clip]{2771f4b.ps}\end{figure}$	Figure 4: Radial velocity data and tentative orbital solution for OGLE-TR-123 and OGLE-TR-129. The orbital periods and epochs are constrained in combination with the photometric signal. The corresponding parameters are given in Table 1. The measurements uncertainties are plotted only when larger than the symbols.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2771f6.ps}\end{figure}$	Figure 6: Radial velocity data and orbit for the three detected transiting planets. Adapted from Pont et al. (2004); Bouchy et al. (2004); Moutou et al. (2004).
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$\begin{figure} \par\includegraphics[angle=-90,width=4.7cm,clip]{2771f7a.ps}\hspa... ...space*{2mm} \includegraphics[angle=-90,width=4.7cm,clip]{2771f7c.ps}\end{figure}$	Figure 7: Radial velocity data for the objects without radial velocity variations in phase with the transit signal. The dotted line indicates the orbit corresponding to a transiting 1 $M_{\rm J}$ planet.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2771f8.ps} % \end{figure}$	Figure 8: Lower limit for the rotation velocity as a function of period for objects without detected signal in the CCF, if they are single stars of spectral type later than F2. Lines as in Fig. 2.
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