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Fig. 9


Combined scattered and emitted light flux ratio Lp,tot/L.λ of our HD 189733b simulation as a function of wavelength at secondary eclipse (α = 0°). We compare our HD 189733b simulation results to available observational data from HST STIS (purple dots, 0.290.57 μm; Evans et al. 2013), HST WFC3 (green diamonds, 1.131.64 μm; Crouzet et al. 2014), HST NICMOS (orange squares, 1.462.44 μm; Swain et al. 2009; Barstow et al. 2014), and Spitzer IRAC (magenta pentagons, 3.6 μm, 4.5 μm; Knutson et al. 2012).

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