Fig. 10

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TOI-5076’s CCFs and its residual. Top: the CCFs for each SOPHIE spectrum were computed using a G2V template. All CCFs were shifted from the velocity frame of the solar system barycenter where they are computed, to the frame of TOI-5076. Bottom: a Gaussian fit was subtracted to leave the residual noise. Both panels clearly display second broad CCFs, indicating a contaminated star. The feature in the center of the CCFs is caused by the primary’s imperfect Gaussian fit as a result of contamination.
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