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Fig. 6


Maps of the time-series CCFs from Run 2012, as a function of radial velocity relative to the star (in abscissa) and orbital phase (in ordinate, increasing vertically). Flux values increase from dark red to white. Vertical dashed white lines are plotted at ± v sin i, and white diamonds indicate the time of the first and fourth contacts. Top panel: CCFs produced by the SOPHIE pipeline. Dashed white areas separate the different datasets taken over three successive nights (see Sect. 2.2). The tilt of the continuum is visible as a flux increase from negative to positive velocities (see also Fig. 4), and does not vary significantly from one night to the other. Upper middle panel: map of the transit residuals after subtracting the model stellar profile. The signature of KOI-12.01 is the bright and wide feature that crosses the entire width of the line profile from ingress to egress. Lower middle panel: best-fit model for KOI-12.01 transiting signature, emphasized by the dark brown line (extended beyond the first/fourth contact and ± v sin i for the sake of clarity) obtained with λ = 12.5. This is consistent with the asymmetry of the signature visible in the above panel, whereas an aligned orbit would correspond to the lighter brown line. Bottom panel: overall residual map after the further subtraction of the model planet signature. The faint, alternating bright and dark parallel streaks may be caused by stellar intrinsic variability.

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