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Hiʻiaka is the largest moon of the distant dwarf planet Haumea. Here, the authors report the first multi-chord stellar occultations of Hiʻiaka, revealing its size, shape, and density, suggesting an origin from Haumea’s icy mantle.

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.

JWST observations suggest that both pebbles and planetesimals played an important role in forming the giant exoplanet WASP-121 b beyond the H₂O ice line. They also indicate that strong vertical mixing likely drives the nightside atmospheric chemistry.

Observations of the warm Neptune WASP-107b show that the planet has a hot interior with an intrinsic temperature of about 460 K.

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.

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.

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.

The warm Earth-sized planet LHS 475 b is validated and characterized with two transits observed by the JWST. The absence of evident spectroscopic features excludes a substantial hydrogen envelope and indicates that LHS 475 b has either little or no atmosphere or an optically thick cloud deck at high altitudes.

Analysis is presented that indicates that there is strong evidence that SiO or Mg, the major constituents of silicate condensates, must be present in gaseous form in the atmosphere of ultra-hot Jupiter WASP-178b.

A broad-wavelength 0.5–5.5 µm atmospheric transmission spectrum of WASP-39b, a 1,200 K, roughly Saturn-mass, Jupiter-radius exoplanet, demonstrates JWST’s sensitivity to a rich diversity of exoplanet compositions and chemical processes.

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.