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Fig. 7

image

Fit to our observed eclipse depths and two Ks band depths found by Croll et al. (2015) and Cruz et al. (2016), adopting model atmospheres for the planet (Fortney et al. 2006) and an ATLAS model atmosphere for the star. The four planetary models correspond to different heat redistribution coefficients, with f = 1.0 being only day-side redistribution and f = 0.5 being planet wide; the models contain no TiO/VO opacity and have no temperature inversions. Contrast (ordinate) is the planetary flux divided by the stellar flux. The Croll et al. result is offset in wavelength from 2.14 μm for clarity. The asterisks, also offset from the two Spitzer channels, are the contrasts that result from integrating the stellar and planetary fluxes over the Ks and Spitzer bandpass functions.

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