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Fig. 2


Top: follow-up transit photometry for WASP-103 b. For each light curve, the best-fit transit+baseline model deduced in our global analysis (Sect. 3.2) is superimposed. The light curves are shifted along the y-axis for clarity. BB = blue-blocking filter. The flux offset visible in each BB light curve corresponds to the meridian flip of the TRAPPIST German equatorial mount, resulting in a different position of the stars on the chip. Bottom: same follow-up photometry divided by the best-fit baseline functions, period-folded on the best-fit transit ephemeris, and binned in 2 min intervals. Each point corresponds to the mean flux value for the corresponding time interval. The best-fit transit model is overplotted in red.

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