![The best-fit chemical equilibrium models to our co-added data performed with three different retrieval suites. For all chemical equilibrium fits, the models produced poor fits to several features on the spectrum, namely near 3 µm and between 4 − 5 µm region. For the 4.3 micron region, the differences between features are due to a combination of differences in the retrieval framework (namely prior constraints) and chemical networks used (FastChem vs GGChem) for each retrieval suite. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/GEMS-JWST.png?resize=1200%2C719&ssl=1)
[astro-ph.EP] HATS-6 b is one of several recently discovered Giant Exoplanets orbiting M-dwarf Stars (GEMS) and is part of a JWST survey that aims to compare bulk and atmospheric properties […]
NIRSpec
Posted inExoplanets, -moons, -comets
JWST Transmission Spectroscopy Of TOI-3235 b: Challenges In Constraining Giant Planet Atmospheres Around M Dwarfs Amid Stellar Contamination
[astro-ph.EP] Giant planets orbiting low-mass M dwarfs challenge current planet formation theories, which predict that such planets are unlikely to form. Characterizing their atmospheres can provide key insight into their […]
![Vertical cut through the best-fit disk model on a logarithmic radial scale. Shown are temperatures, where the gas density, ϱdisk, exceeds an assumed ISM density of ϱISM = 2.7 × 10−24 g cm−3 (Ferrière 2001) by a factor of 1000. The snowline at Tsnow = 170 K and the 100 K-line, as well as the unity optical depth lines at a wavelength of 3.1 µm (computed for the best-fit model described in Sect. 5.2.2) measured from the star to the observer and from observer to the star, illustrate the temperature and dust density structure of the disk. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/Spatial.png?resize=1200%2C715&ssl=1)
Posted inAstrochemistry
Spatial Distribution Of Water Ice In The Protoplanetary Silhouette Disk d216-0939
[astro-ph.EP] The composition of rocky planets depends on the dust in their natal protoplanetary disk (PPD), potentially containing water ice. Crystalline water ice was detected in the PPD d216-0939 in […]
Posted inIcy Worlds
Tracing The Source Of Carbon Oxides On The Large Moons Of Uranus
[astro-ph.EP] The Uranian moons Ariel, Umbriel, Titania, and Oberon are enriched in CO2 mixed with CO, but the origin(s) of these carbon oxides, be they primarily native or radiolytic, remains […]
Posted inBeta Pictoris
Discovery Of An Exterior Third Planet Orbiting β Pictoris
[astro-ph.EP] We report the discovery of β Pictoris d (β Pic d), a third giant planet in the β Pictoris system, which now becomes only the second directly imaged system […]
Posted inExoplanets, -moons, -comets
C,N,O,S, And Photochemistry In A Temperate Giant Planet Orbiting A Late M Dwarf
[astro-ph.EP] We report the JWST NIRSpec/PRISM transit spectrum of TOI-6894b, an exceptional 420 K sub-Saturn that is the only known giant planet transiting a late M dwarf. Remarkably, both the […]
Posted inComets and Asteroids
Webb Finds Clues To The Ancient Origin Of Comet 3I/ATLAS
The third identified interstellar comet in human history has a surprising chemical makeup, raising questions as to how common, or unusual, conditions in our own Solar System may be.
Posted inAstronomy & Telescopes, Atmospheres, Climate, Weather, Biosignatures & Paleobiology, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Status Report
JWST-TST High Contrast: First Direct Spectroscopy of GJ 504 b Reveals Clouds And Possible Metal Enrichment
Characterizing the coldest directly imaged companions through direct spectroscopy has only recently become possible with the James Webb Space Telescope.
Posted inAstrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biogeochemical Cycles & Geobiology, Biosignatures & Paleobiology, Icy Worlds, Imaging & Spectroscopy, Pluto, Status Report, Titan
An Unidentified Absorption Feature At 5.11 μm On The Surface Of Titan And Pluto From JWST Spectroscopy
Titan possesses a thick N2-CH4 atmosphere that makes it difficult to study its surface spectroscopically. The chemical composition of the solid surface of Titan thus remains very uncertain.
Posted inAtmospheres, Climate, Weather, Exoplanets, -moons, -comets, Gas Giants, Imaging & Spectroscopy, Status Report
Horizontal Transport As A Source Of Disequilibrium Chemistry On The Nightside Of A Hot Exoplanet
Hot Jupiters have temperature gradients of several hundreds of degrees between their permanent daysides and nightsides. Such a strong gradient creates winds with speeds of the order of kilometres per […]