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Fig. 25


Top: the observed phase curve of GJ 436 at 8 μm (2008 July 12, AORs: 27863296, 27863552, 27863808) superimposed to a model for a Lambert sphere (red line). The adopted baseline models are respectively p([xy], p([xy], and p([xy] to exclude temporal models. The black crosses are binned data with their 1σ error bars. The peak-to-peak flux difference equals 268 ppm while A = 189 ± 100 ppm. Our model for a Lambert sphere is compared with Lewis et al. (2010) models shifted vertically. The models correspond to 1×-solar (green stars) and 50×-solar (magenta circles) metallicity cases. The observed day-night temperature contrast indicates a metal-rich atmosphere. Bottom: the residual light curve.

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