F. Pont, D. K. Sing, N. P. Gibson, S. Aigrain, G. Henry, N. Husnoo
The hot Jupiter HD189733b is the most extensively observed exoplanet. Its atmosphere has been detected and characterised in transmission and eclipse spectroscopy, and its phase curve measured at several wavelengths. This paper brings together the results of our campaign to obtain the complete transmission spectrum of the atmosphere of this planet from UV to IR with HST, using the STIS, ACS and WFC3 instruments. We provide a new transmission spectrum across the entire visible and infrared range. The radius ratio in each wavelength band was re-derived, where necessary, to ensure a consistent treatment of the bulk transit parameters and stellar limb-darkening. Special care was taken to correct for both occulted and unocculted star spots, and derive realistic uncertainties. The combined spectrum is very different from the predictions of cloud-free models; it is dominated by Rayleigh scattering over the whole visible and NIR range, the only detected features being narrow Na and K lines. We interpret this as the signature of a haze of condensate grains extending over at least five scale heights. We show that a dust-dominated atmosphere could also explain several puzzling features of the emission spectrum and phase curves, including the large amplitude of the phase curve at 3.6um, the small hot-spot longitude shift and the hot mid-infrared emission spectrum. We discuss possible compositions and derive some first-order estimates for the properties of the putative condensate haze/clouds. We finish by speculating that the dichotomy between the two observationally defined classes of hot Jupiter atmospheres, of which HD189733b and HD209458b are the prototypes, might not be whether they possess a temperature inversion, but whether they are clear or dusty. We also consider the possibility of a continuum of cloud properties between hot Jupiters, young Jupiters and L-type brown dwarfs.
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http://arxiv.org/abs/1210.4163
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