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Fig. 1

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Upper panel: least squares, deconvolved line profiles of CoRoT-11 (points with error bars), as obtained from the time-series HIRES spectra acquired during the transit of the planet. The limb-darkened, rotationally-broadened line profile of the best fitting model is shown with solid lines. Radial velocity (wavelength) increases from left to right, time from bottom to top. The planet signature is the bump that migrates from about −20  km s-1 near the middle of the time series, to about  + 15  km s-1 in the upper line profile. Lower panel: residuals of the composite spectral line profiles of CoRoT-11 following the subtraction of the above-mentioned synthetic profile. Orbital phase increases vertically. The two vertical dashed lines mark the  ± v sin i of the star. The three crosses denotes the first, second, and third planet’s contacts. A moderately bright feature, “travelling” from the bottom left to the top right corner, appears in the residual map as the result of the transit of the planet across the stellar disc.

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