All Figures

	Figure 1: Radial-velocity measurements of CoRoT-Exo-4 as a function of time, showing the best-fit solution and O-C residuals. Black filled circles are HARPS data, and red open diamonds are SOPHIE data.
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In the text

	Figure 2: Radial-velocity measurements of CoRoT-Exo-4 with respect to the orbital phase as estimated from the CoRoT ephemeris and the best-fit solution. Black filled circles are HARPS data, and red open diamonds are SOPHIE data.
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In the text

	Figure 3: Bisector variations (span of the bisector slope) as a function of orbital phase ( top panel) and radial velocity value ( bottom panel). Black filled circles are HARPS data, and red open diamonds are SOPHIE data.
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In the text

Figure 4: Theoretical models for the contraction of CoRoT-Exo-4b with time compared to the observations. The models (Guillot et al. 2006) assume either solar composition ( left panel) or the presence of a central dense core of ( right panel). In each case, three possible evolution models are shown: (1) a standard model; (2) a model assuming that 1% of the incoming stellar luminosity is transformed into kinetic energy and dissipated in the deep interior by tides; (3) a model in which interior opacities have been arbitrarily increased by a factor 30.

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In the text

	Figure 5: Mass-period diagram of the 35 known transiting planets showing the location of CoRoT-Exo-4b (diamond).
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In the text