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Fig. 14


Published secondary eclipse spectra of exoplanets observed by HST/WFC3 with the G141 grism. The vertical scale is different for each planet. The spectra have been ordered as a function of gravity and dayside equilibrium temperature assuming zero albedo and a dayside only redistribution of the absorbed stellar energy. H2 O dissociation should be important for planets right of the short dashed line and H opacities should be relevant for planets right of the long dashed line. We additionally show as a dotted line the putative separation between planets with gaseous TiO and planets where TiO is cold trapped either in the deep layers (Parmentier et al. 2016)or in the nightside of the planet (Parmentier et al. 2013; Beatty et al. 2017a). In each panel the orange line shows the best fit blackbody, whose temperature is given in Table 2.

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