S20B0008abst
S20B0008
With an effective temperature of almost 3300K, WASP-33b is one of the hottest planet’s known to date. Due to this high temperature, comparable to that of an M5V star, TiO is expected to be in the gas-phase that can cause inversion layers in hot Jupiters, since it has many spectral lines at optical and near-infrared wavelengths. Here we propose to observe the day-side of this planet at high spectral resolution with IRD to probe molecular species of WASP-33b at near-infrared wavelengths, and constrain the temperature structure of the planet in a wide pressure range. The near-infrared observations will enable us to directly probe a variety of molecules simultaneously, especially TiO, H2O and CH4, in the planet’s atmosphere, thereby providing a direct constraint on the abundances and atmospheric composition. We will combine the signal from a large number of lines, thereby increasing the SNR, and enabling a robust detection of the targeted molecules, provide a direct determination of the planet’s orbital velocity, and allow a direct measurement of the mass of both the star and planet. Finally, as we are looking at the day- and night-side rotating in and out of view, we will search for difference in the emission spectrum of the planet over time.
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