S19A0066

In hot Jupiter, we have detected the signature of major opacity sources except VO. VO is one of the significant source of opacity that can be found in the atmosphere of late M-dwarfs. However, it has never been detected in the atmosphere of hot Jupiter mostly due to lack of the resolution power. Using IRD, we are aiming to detect VO in the day side of moderately hot Jupiter. The temperature of moderately hot Jupiter is cold enough to remove gaseous TiO (other major opacity source) but hot enough to keep gaseous VO in the atmosphere. By probing the planet radial velocity using high-resolution spectroscopy we expect to unambiguously not only for the first time detect VO signature in hot Jupiter, but also detect other strong opacity sources, such as H2O, FeH, allowing the constraint of the chemical composition and the temperature structure. Detecting VO using IRD will improve our understanding of the exoplanet atmosphere in general and the climates of the planet specifically.


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