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Fig. 10

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Spitzer photometry divided by two different best-fit baseline models. The first (top) aims to remove position- and PSF effects, and consists of a 4th order polynomial of the PSF x-and y-centres and widths, supplemented with the BLISS mapping method (Stevenson et al. 2012) to remove high-frequency position effects. The second baseline model (bottom) adds to the first a slope and a quadratic function of the logarithm of time to model the sharp decrease in the counts at the beginning of the run (negative ramp). Both light curves are binned per 0.005d = 7.2 min intervals.

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