The GAPS Programme at TNG XXXIX -- Multiple molecular species in the atmosphere of the warm giant planet WASP-80 b unveiled at high resolution with GIANO-B

TL;DR

This study used high-resolution spectroscopy to detect multiple molecules in the atmosphere of the warm giant exoplanet WASP-80 b, revealing complex chemistry and potential disequilibrium processes in its atmosphere.

Contribution

First detection of several molecules in WASP-80 b's atmosphere using high-resolution transmission spectroscopy, highlighting the presence of disequilibrium chemistry in a cooler giant planet.

Findings

Detection of H2O, CH4, NH3, and HCN with high significance

Tentative detection of CO2

Inconclusive results for C2H2 and CO

Abstract

Detections of molecules in the atmosphere of gas giant exoplanets allow us to investigate the physico-chemical properties of the atmospheres. Their inferred chemical composition is used as tracer of planet formation and evolution mechanisms. Currently, an increasing number of detections is showing a possible rich chemistry of the hotter gaseous planets, but whether this extends to cooler giants is still unknown. We observed four transits of WASP-80 b, a warm transiting giant planet orbiting a late-K dwarf star with the near-infrared GIANO-B spectrograph installed at the Telescopio Nazionale Galileo and performed high resolution transmission spectroscopy analysis. We report the detection of several molecular species in its atmosphere. Combining the four nights and comparing our transmission spectrum to planetary atmosphere models containing the signature of individual molecules within the cross-correlation framework, we find the presence of H2O, CH4, NH3 and HCN with high significance, tentative detection of CO2, and inconclusive results for C2H2 and CO. A qualitative interpretation of these results, using physically motivated models, suggests an atmosphere consistent with solar composition and the presence of disequilibrium chemistry and we therefore recommend the inclusion of the latter in future modelling of sub-1000K planets.