![Sky positions of the TESS M&M sample (shown in a full-sky Mollweide projection), with number of single-sector TESS light curves through Year 6 as colorbar. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/The-Occurrence.png?resize=1200%2C717&ssl=1)
[astro-ph.EP] We present the first determination of the occurrence of transiting circumbinary planets (CBPs) in TESS data. Since tight binaries represent a constrained environment relative to single stars, CBPs contribute […]
M-dwarf
Posted inExoplanets, -moons, -comets
Hybrid Worlds Are The Commonest Outcome Among The M-dwarf Sub-Neptunes Characterised With JWST
[astro-ph.EP] The sub-Neptunes orbiting M dwarfs are usually assigned to one of two classes: rocky cores beneath primordial hydrogen, or volatile-rich bodies formed beyond the water-ice line.
![D.2: Transit signals recovery analysis in the TESS light curve of TOI-210. TOI-210 b is shown in gold at its period of 9.01 days. Candidate planets at 2.15 and 3.76 days tentatively detected in the NIRPS RVs are indicated as lower limits, with arrows extending from minimum (iron density) to realistic (Earth density) radii based on their minimum masses. The expected transit depths fall within the TESS sensitivity, suggesting that if these RV signals are planets, they are unlikely to be transiting. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/A-temperate.png?resize=1200%2C713&ssl=1)
Posted inExoplanets, -moons, -comets
A Temperate Sub-Neptune Transiting The M4 Dwarf TOI-210 Identified By NIRPS And TESS — Uncovering Hidden M-dwarf Planetary Systems In The Near-infrared
[astro-ph.EP] Super-Earths and sub-Neptunes dominate the exoplanet population, yet their compositions, formation mechanisms, and capability of retaining atmospheres remain poorly understood. M-type stars offer a unique opportunity to investigate these […]
![Wavelength distributions of candidate spectral lines retained at each step of the line-selection procedure. The histograms show the initial linelist (light), lines retained after automated vetting (intermediate), and the final manually vetted sample (dark). The shaded background regions indicate approximate wavelength ranges for the Y, J, H, and K-bands.-- [astro-ph.SR]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/Elemental.png?resize=1200%2C716&ssl=1)
Posted inStellar Cartography
Elemental Abundances of Cool Stars: A Spectroscopic Framework Applied to Five Planet-Host Stars
[astro-ph.SR] Stellar elemental abundances provide important constraints on the chemical environments from which planets form. M and late-K dwarfs are prime targets for the characterization of small exoplanets, yet their […]
![Panel (a): HR diagram of the OC members with detections. The blue solid line is the fitting results of MS. green dashed lines represent the upper and lower bounds of the MS fitted with a ±0.5 offset, and the red dashed line is the same sequence shifted upwards by 2. The color bars represent the stellar ages. Panel (b): HR diagram of the field stars with detections. Panel (c): The Galactic distribution of the selected sources from the detected OC members. Panel (d): The Galactic distribution of the selected sources from the detected field stars. -- [astro-ph.SR]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/Evolution-of.png?resize=1200%2C720&ssl=1)
Posted inHabitable Zones
Evolution of Stellar Activity and Habitable Zone (EATEN): III. X-ray Activity of Dwarfs in Open Clusters and Field Stars
[astro-ph.SR] Stellar X-ray emission serves as a direct diagnostic of coronal activity, which is fundamentally linked to coronal heating processes. It also strongly influences the atmospheres and long-term habitability of […]
![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)
Posted inExoplanets, -moons, -comets
GEMS JWST: HATS(-6 b): A Sub-solar Metallicity Giant Planet With Water, Methane And Ammonia In Its Atmosphere
[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 […]
![The Rapid ASKAP Continuum Survey (RACS) radio images of radio sources associated with candidates A (J1245-2652, top row) and B (J0356-4031, bottom row) are shown at three frequencies: 887.5 MHz (left), 1367.5 MHz (centre), and 1655.5 MHz (right), with each panel covering a field of view of 65" × 65" . White ellipses show the PyBDSF source fits from the RACS catalogues, with thick solid lines indicating the fits at the frequency of the image, while thin dashed lines show fits from the other radio frequencies for comparison. Large blue crosses (×) mark radio source positions for the corresponding frequency, and small blue plus signs (+) indicate positions at other frequencies. The red stars represent the Gaia positions propagated to the corresponding RACS observation epochs using the measured proper motions. -- [astro-ph.SR]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Archival-Diagnostics.png?resize=1200%2C720&ssl=1)
Posted inSETI & Technosignatures
Archival Diagnostics for Potential Background Contaminants Of Project Hephaistos Dyson Sphere Candidates
[astro-ph.SR] We report on the diagnostic inspection of nine Project Hephaistos Dyson Sphere candidate M-dwarfs based on archival data. By comparing the Gaia positions, propagated to the AllWISE epoch, with […]
Posted inUncategorized
An Agnostic Machine Learning Model of Photosynthetic Habitability
The search for exoplanet biosignatures is guided by whether planetary environments can sustain photosynthesis.
Posted inAstrogeology, Astronomy & Telescopes, Exoplanets, -moons, -comets, Status Report, Stellar Cartography
Revisiting The Exo-Mercury Candidate GJ 367 b With ESPRESSO And A Self-Consistent Tidal Distortion Model
We report revised mass and radius measurements for GJ 367 b, an ultra-short-period (7.7 hr) sub-Earth in a multi-planet system orbiting a nearby (~9 pc) M dwarf host. Previous mass […]
Posted inAtmospheres, Climate, Weather, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Status Report, Water/Hycean Worlds & Oceanography
Ultraviolet Radiation Effects on the Optical Properties of Water-Dominated Exoplanet Hazes
Temperate sub-Neptune and terrestrial exoplanets could contain large inventories of water in various phases, such as water-dominated atmospheres or even oceans. Observations have shown that many exoplanets, including water worlds, […]