The emergence of habitable conditions on the early Earth and on rocky exoplanets requires persistent energy sources that can drive both prebiotic chemistry and climate warming under magnetically active young […]
The organosulfur biosignature gases dimethylsulfide (DMS) and dimethlydisulfide (DMDS) have recently been claimed to be present in the atmosphere of sub-Neptune exoplanet K2-18b, leading to the suggestion of possible extraterrestrial […]
The icy material within protoplanetary disks plays a central role in planet formation, yet remains poorly characterized by observations. We present 1.6-28μm spectra of five disks obtained as part of […]
As stars evolve, they undergo significant changes in their physical properties, which can have a profound impact on the planets orbiting them.
Neptune’s present axial tilt of approximately 28 deg. with respect to its orbital plane can be explained by collisions that its primordial core may have experienced with surrounding planetary embryos […]
A particularly intriguing subclass of rocky exoplanets are the ultra-short period (USP) worlds that orbit their host stars in less than a day. These planets are particularly rare around M […]
Transmission spectroscopy has greatly advanced the study of exoplanet atmospheres, but stellar surface heterogeneities can contaminate transit spectra. Characterising how stellar spectra vary across the stellar disc is therefore essential […]
High-resolution spectroscopy provides unique constraints on exoplanet atmospheric composition and dynamics. The past decade of ground-based campaigns has accumulated extensive public archives, yet many observations remain unanalysed.
![Eimission spectra of 3I/ATLAS taken with BFOSC and YFOSC. For clarity, the full spectral range is divided into three panels with different vertical offsets to emphasize specific features. The left panel highlights emission lines of Ni i (blue dashed lines) and Fe i (red dashed lines), and the CN violet band (blue shaded). The middle panel shows molecular bands of C3 (green shaded), CH (orange shaded), and C2 (red shaded), and lists the heliocentric distance for each spectrum. The right panel displays the [O i] λλ6300, 6364 doublet (green dashed lines). -- astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/03/Postperihelion-Coma-Composition.png?resize=1200%2C720&ssl=1)
We present multi-epoch optical spectroscopy of the interstellar comet 3I/ATLAS obtained from December 2025 to January 2026 (heliocentric distances 1.8 to 3.3 au). From these spectra, we derive post-perihelion production […]
The excess abundance of highly siderophile elements (HSEs), as inferred for the terrestrial planets and the Moon, is thought to record a `late veneer’ of impacts after the giant impact […]
