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A complete revolution of exo-Neptune LTT 9779 b was observed with the NIRISS/SOSS instrument onboard the JWST. The resulting full phase curve is indicative of an equatorial jet that transports heat from the dayside to the colder nightside, resulting in an asymmetric distribution of clouds on the planet.

Ultra-hot Jupiters provide a unique window into atmospheric processes and this in-depth study enables integrated global snapshots of the atmosphere and more accurate identification of flow patterns, thus allowing for better comparison to models.

The atmospheric terminator region of WASP-39 b, a hot gas giant exoplanet, is inhomogeneous, despite past assumptions, with the evening terminator being hotter and thus probably clearer, and the morning terminator probably being cloudy and consequently cooler.

Analysis of the panchromatic transmission spectrum of the warm, low-density, Neptune-sized exoplanet WASP-107b from instruments aboard the HST and JWST suggests that tidal interaction with its host star led to changes in its atmospheric chemistry.

Phase-resolved mid-infrared observations from JWST of the hot gas giant WASP-43b detect a day–night difference of 659 ± 19 K. Comparison with climate models shows that the observations are compatible with cloudy skies, at least on the nightside, and the lack of methane detection suggests the presence of disequilibrium chemistry.

Time-series observations from the JWST of the transiting exoplanet WASP-39b show gaseous water in the planet’s atmosphere and place an upper limit on the abundance of methane.

The medium-resolution transmission spectrum of the exoplanet WASP-39b, described using observations from the Near Infrared Spectrograph G395H grating aboard JWST, shows significant absorption from CO₂ and H₂O and detection of SO₂.

The transmission spectrum of the exoplanet WASP-39b is obtained using observations from the Single-Object Slitless Spectroscopy mode of the Near Infrared Imager and Slitless Spectrograph instrument aboard the JWST.

Evidence of a large temperature difference between dawn and dusk has been observed on the exoplanet WASP-107 b. This planet is so cool that it was not expected to exhibit this phenomenon, implying a need to further explore the exoplanet population.

Observations from the JWST MIRI/LRS show the detection of SO₂ spectral features in the 5–12-μm transmission spectrum of the hot, Saturn-mass exoplanet WASP-39b, suggesting that photochemistry is a key process in high-temperature exoplanet atmospheres.

Transmission and emission spectra of the 825 K warm Jupiter WASP-80b taken with the NIRCam instrument of the JWST show strong evidence of CH₄ at greater than 6σ significance

The dayside thermal emission spectrum and brightness temperature map of the ultra-hot Jupiter WASP-18b obtained from the NIRISS instrument on the JWST showed water emission features, an atmosphere consistent with solar metallicity, as well as a steep and symmetrical decrease in temperature towards the nightside.

Observations from the JWST show the presence of a spectral absorption feature at 4.05 μm arising from SO₂ in the atmosphere of the gas giant exoplanet WASP-39b, which is produced by photochemical processes and verified by numerical models.

The C/O ratio of the transiting hot Jupiter WASP-77Ab is measured here and found to be approximately solar, though the (C+O)/H ratio is subsolar.

A spectroscopic thermal phase curve of GJ 1214b obtained with the JWST in the mid-infrared is reported and a planet with a high metallicity atmosphere blanketed by thick and reflective clouds or haze is found.

Transmission spectroscopy observations from the James Webb Space Telescope show the detection of carbon dioxide in the atmosphere of the gas giant exoplanet WASP-39b.

A population study of near-infrared spectra of 19 hot giant planets shows a correlation between the strength of the 1.4 μm water band and temperature, which is broadly regulated by irradiation. However, the observed scatter around the mean is indicative of the effect of individual planetary formation pathways on the composition.