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We present a thermal emission spectrum of the bloated hot Jupiter HAT-P-32Abfrom a single eclipse observation made in spatial scan mode with the Wide FieldCamera 3 (WFC3) aboard the Hubble Space Telescope (HST). The spectrum coversthe wavelength regime from 1.123 to 1.644 microns which is binned into 14eclipse depths measured to an averaged precision of 104 parts-per million. Thespectrum is unaffected by a dilution from the close M-dwarf companionHAT-P-32B, which was fully resolved. We complemented our spectrum withliterature results and performed a comparative forward and retrieval analysiswith the 1D radiative-convective ATMO model. Assuming solar abundance of theplanet atmosphere, we find that the measured spectrum can best be explained bythe spectrum of a blackbody isothermal atmosphere with Tp = 1995 +/- 17K, butcan equally-well be described by a spectrum with modest thermal inversion. Theretrieved spectrum suggests emission from VO at the WFC3 wavelengths and noevidence of the 1.4 micron water feature. The emission models with temperatureprofiles decreasing with height are rejected at a high confidence. Anisothermal or inverted spectrum can imply a clear atmosphere with an absorber,a dusty cloud deck or a combination of both. We find that the planet can havecontinuum of values for the albedo and recirculation, ranging from high albedoand poor recirculation to low albedo and efficient recirculation. Opticalspectroscopy of the planet's day-side or thermal emission phase curves canpotentially resolve the current albedo with recirculation degeneracy.

Hubble PanCET: An isothermal day-side atmosphere for the bloated gas-giant HAT-P-32Ab