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	Figure 1: Radial-velocity measurements of HD 189733 superimposed on the best Keplerian solution. The higher density of points corresponds to spectroscopic-transit measurements. They are not used to derive the Keplerian solution. Error bars represent the photon-noise uncertainties.
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In the text

	Figure 2: Phase-folded radial velocity measurements of HD 189733 superimposed on the best Keplerian solution. Error bars represent the photon-noise uncertainties. The inset shows a zoom near phase zero where radial velocities exhibit the Rossiter-McLaughlin effect.
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In the text

	Figure 3: Photometric transits of HD 189733 observed with the 1.20-m OHP telescope. Triangles correspond to the observation on B band made on September 15th 2005. Full circles and open circles correspond to observation on R band made respectively on September 24th and 26th 2005. The solid curve represents the best-fit model for the complete B-band transit.
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In the text

Figure 4: Mass-radius diagram for the 9 transiting exoplanets. Jupiter and Saturn are indicated for comparison, as well as the loci of isodensities at 0.3, 0.7 and 1.3 g cm-3. Data are from Pont et al. (2004) (OGLE-TR-111b), Konacki et al. (2005) (OGLE-TR-10b), Moutou et al. (2004) (OGLE-TR-132b), Torres et al. (2004) (OGLE-TR-56b), Bouchy et al. (2004) (OGLE-TR-113b), Laughlin et al. (2005) (HD 209458b and TrES-1), Sato et al. (2005) (HD 149026b).

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In the text

	Figure 5: Mass-period diagram for the 9 transiting exoplanets.
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In the text