High-resolution day-side spectroscopy of the ultra-hot Jupiter WASP-33b (Tday∼3300 K), have revealed a plethora of atomic and molecular species including Fe, Ti, Si, H2O, OH and CO. Even more interestingly, some species appear to show a different distribution across the planet’s day-side, with OH having the strongest signal just after eclipse, which could indicate that it is mostly concentrated closest to the morning terminator. Since OH results from the dissociation of H2O, this could be evidence of water formation on the planet’s night-side, which then gets dissociated into OH when it gets blown across the morning terminator. Here we propose to use IRD to observe three transits of this planet and determine its transmission spectrum. This will enable us to further determine the presence of various species and determine their abundances. In addition, by taking advantage of the rotation of the tidally locked planet we can probe the atmosphere along different longitudes. This will enable us to to place strong constraints on the location of the region with the highest concentration of OH and observationally study one of the first 3D-nature and atmospheric dynamics of an ultra-hot Jupiter.
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