Combined scattered and emitted light flux ratio Lp,tot,λ/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, 0.29−0.57 μm; Evans et al. 2013), HST WFC3 (green diamonds, 1.13−1.64 μm; Crouzet et al. 2014), HST NICMOS (orange squares, 1.46−2.44 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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