Fig. 1.
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Dayside brown dwarf to star flux ratio posteriors measured from TESS Sector 17 photometry, CHEOPS secondary eclipse observations, and TESS Sector 57 photometry. The y-axis offsets represent the average time differences between the observation sets (one year between the TESS S. 17 and CHEOPS observations and two years between the CHEOPS and TESS S. 57 observations).
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