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Fig. 1


Secondary eclipses of GJ 436b observed with the IRS (top) and MIPS (bottom) instruments. Relative flux offsets are applied to datasets for clarity. On the left, raw data are represented by cyan dots for the unbinned data and by black dots for binned data per interval of 7 min with their error bars. The superimposed red line is the best-fitting model and includes the transit model. On the middle, the same binned data divided by the best-fitting baseline model reveal the occultation shape. The eclipse model is superposed in red. The right panel displays the binned residuals from the same dataset. The shaded green area of every panel shows the eclipse event.

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