The search for Life in the Universe generally assumes three basic life’s needs: I) building block elements (i.e., CHNOPS), II) a solvent to life’s reactions (generally, liquid water) and III) […]
![Results of the pRT retrievals for the atmosphere of HD 86226 c. Left: PACMAN spectrum (black data) and 1, 2, and 3σ percentiles of the spectra from the posteriors of the pRT retrieval with scaled solar chemistry (green shadings). The gray spectra show cloud-free models with 1× and 1000× solar metallicity. Right: Posterior distribution for the two retrieval runs with scaled solar chemistry (green) and H-He-H2O atmosphere (purple). The pressures are provided in units of log10([bar]). Contours are drawn at the 1, 2, and 3σ levels. Vertical dashed lines mark the 16%, 50%, and 84% quantiles. astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2025/07/The-SPACE-Program-I.png?resize=1200%2C709&ssl=1)
Sub-Neptune exoplanets are the most abundant type of planet known today. As they do not have a Solar System counterpart, many open questions exist about their composition and formation.
Metal-bearing species in diffuse or molecular clouds are often overlooked in astrochemical modeling except for the charge exchange process.
We present a near-infrared spectroscopic analysis (0.9-2.4 micron) of gravity indices for 57 ultracool dwarfs (spectral types M5.5 to L0), including exoplanet hosts TRAPPIST-1, SPECULOOS-2, SPECULOOS-3, and LHS 3154. Our […]
We have developed a 1D planetary atmosphere model that solves in a self-consistent manner the evolution of temperature and disequilibrium chemistry in the vertical direction.
Whether the presence of planets affects the lithium (Li) abundance of their host stars is still an open question.
HD 209458 b is the first exoplanet on which an atmosphere was detected. Since then, its atmosphere has been investigated using multiple telescopes and instruments. However, many of its atmospheric […]
The formation and migration history of a planet is expected to be imprinted in its atmosphere, in particular its carbon-to-oxygen (C/O) ratio and metallicity.
Low-mass, metal-enriched stars were likely present as early as cosmic dawn. In this work, we investigate whether these stars could have hosted planets in their protoplanetary disks.
The shape of a planet’s orbit is one of its fundamental properties, along with its size and distance from its host star. Earth has a nearly circular orbit, but some […]
