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Thermal emission from WASP 24b at 3 6 and 4 5 μm

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Figure

Fig. 1. In each of the above three plots, the 3.6and with the best-fitting occultation models superimposed
Table 2. Trend model parameters and coefficients.
Table 3. WASP-24 system parameters.
Fig. 4. Spectral energy distribution of WASP-24b relative to that of itshost star. The blue circles with error bars are our best-fitting occultationdepths

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