All Figures

	Figure 1: Doppler measurements of the standard star HD 162907 made with UVES. The dispersion of 93  m s-1 is dominated by the centering error. Encircled points correspond to measurements made with a seeing lower than 0.9 arcsec.
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In the text

	Figure 2: Positions of the 54 OGLE candidates on the sky and location of our 3 selected FLAMES fields. Bold circles correspond to the 17 OGLE candidates observed during our run.
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In the text

	Figure 3: Number of detected transits vs. , where d is the depth of the transit signal and the photometric uncertainty. Open symbols indicate objects for which the period had to be modified according to the radial velocity data (OGLE-TR-12, 17 and 59), crosses the objects for which no radial velocity variation was detected.
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In the text

	Figure 4: Phase-folded light curve and best-fit transit curve for all the OGLE candidates followed.
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In the text

Figure 5: Illustration (for OGLE-TR-12) of the residual permutation method for the estimation of the uncertainties. In both panels the open symbols indicate the original data, and the dots indicate two realizations (among a total of 100 realizations) of the data with residuals permutated between different nights. The lines indicate the best fits to the permitted data. The resulting values are 0.254 and 0.292 respectively. Because the transit coverage is constituted by only two nights, systematic trends in the residuals have a large effect on the resulting parameters. In the case of OGLE-TR-12, this error estimate leads to a much higher 1-sigma interval than a analysis.

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In the text

	Figure 6: Phase-folded radial velocities of the low mass star transiting companions. For OGLE-TR-12, black and white points correspond to FLAMES and UVES measurements, respectively.
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In the text

	Figure 7: Phase-folded radial velocities of grazing eclipsing binaries. Black and white points correspond to component a and b, respectively.
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In the text

	Figure 8: Phase-folded radial velocities of triple system. Black and white points correspond respectively to component b and a.
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In the text

Figure 9: Phase-folded Doppler measurements of planetary candidates and unsolved cases. For OGLE-TR-10, black and white points correspond respectively to FLAMES and UVES measurements. Encircled points correspond to measurements made with a seeing lower than 0.9 arcsec. For OGLE-TR-56, black, white and dotted cross points correspond respectively to FLAMES, HARPS and Torres et al. (2004a) measurements. For OGLE-TR-10, 19 and 56, the dotted lines correspond to fitted curves for lower and upper 1-sigma intervals of semi-amplitude K.

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In the text

	Figure 10: Light curve data during the night of detected transits for OGLE-TR-19, 48, 49, and 58 ( from top to bottom) and light curve of OGLE-TR-49 for some days after the first detected transit ( bottom). The correlation of the residuals is clearly visible in the other nights as well.
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In the text

Figure 11: The mass-radius relation for all stellar objects in our sample, primary and secondary. Open circles correspond to candidates OGLE-TR-12, 17 and 55 with a wide range of possible radii. Triangles correspond to the three known M-type eclipsing binaries. The dashed curve up to 0.6  corresponds to the 1 Gyr theoretical isochrones of Baraffe et al. (1998). Above 0.6  the 3 dashed curves show the Padova model mass-radius relations for solar metallicity for three age values.

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In the text