Based on observations obtained with CoRoT, a space project operated by the French Space Agency, CNES, with participation of the Science Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany and Spain; and on observations made with SOPHIE spectrograph at Observatoire de Haute Provence, France (PNP.07 A.MOUT), CORALIE, and HARPS spectrograph at ESO La Silla Observatroy (079.C-0127/F)).

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Table 2 is only available in electronic form at http://www.aanda.org

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... coefficients

We used a quadratic law for the limb darkenning, given by $I(\mu)=I(1)[1-u_a(1-\mu)-u_b(1-\mu)^2]$ , where I is the distribution of brightness over the star and $\mu$ is the cosine of the angle between the normal to the local stellar surface and the line of sight. The use of u₊ and u_- is a better choice to avoid correlations between the two limb darkening coefficients u_a and u_b, as described in Giménez (2006).

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