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The highly irradiated transiting exoplanet, HAT-P-7b, currently provides oneof the best opportunities for studying planetary emission in the optical andinfrared wavelengths. We observe six near-consecutive secondary eclipses ofHAT-P-7b at optical wavelengths with the EPOXI spacecraft. We place an upperlimit on the relative eclipse depth of 0.055% (95% confidence). We also analyzeSpitzer observations of the same target in the infrared, obtaining secondaryeclipse depths of 0.098+/-0.017%, 0.159+/-0.022%, 0.245+/-0.031% and0.225+/-0.052% in the 3.6, 4.5, 5.8 and 8.0 micron IRAC bands respectively. Wecombine these measurements with the recently published Kepler secondary eclipsemeasurement, and generate atmospheric models for the day-side of the planetthat are consistent with both the optical and infrared measurements. The dataare best fit by models with a temperature inversion, as expected from the highincident flux. The models predict a low optical albedo of ~< 0.13, withsubsolar abundances of Na, K, TiO and VO. We also find that the best fittingmodels predict that 10% of the absorbed stellar flux is redistributed to thenight side of the planet, which is qualitatively consistent with theinefficient day-night redistribution apparent in the Kepler phase curve. Modelswithout thermal inversions fit the data only at the 1.25 sigma level, and alsorequire an overabundance of methane, which is not expected in the very hotatmosphere of HAT-P-7b. We also analyze the eight transits of HAT-P-7b presentin the EPOXI dataset and improve the constraints on the system parameters,finding a period of P = 2.2047308+/-0.25 days, a stellar radius of R* =1.824+/-0.089Rsun, a planetary radius of Rp = 1.342+/-0.068RJup and aninclination of i = 85.7+3.5-2.2 deg.

Studying the atmosphere of the exoplanet HAT-P-7b via secondary eclipse measurements with EPOXI, Spitzer and Kepler