Context. Gas giant planets orbiting low-mass stars (T eff ≲ 4600 K) are uncommon outcomes of planet formation. Increasing the sample of well-characterised giants around early M dwarfs will enable population-level studies of their properties, offering valuable insights into their formation and evolutionary histories. Aims. We aim to confirm and

To investigate the formation and evolution of vertical structures in disk galaxies, we measure global sech 2 scale heights, averaging thin and thick components when present, for 2631 edge-on disk galaxies with M * > 10 10M ⊙ at 0 < z < 3.5 from the JWST COSMOS-Web survey. We show that dust extinction systematically overestimates scale heights at

Observations of exoplanetary atmospheres provide critical insights into their chemical composition, formation, and evolution history. Ultra-hot Jupiters serve as excellent targets for atmospheric characterization; studies of these planets may yield key understanding of gas giants' formation and evolution history. We present a thermal emission study

We study the stellar mass function (SMF) of quiescent and star-forming galaxies and its dependence on morphology in ten redshift bins at 0.2 < z < 5.5. We used the COSMOS2025 catalog, built from the 0.54 deg 2 JWST imaging from the COSMOS-Web survey, to select galaxies by type using the NUVrJ rest-frame color diagram and to classify them

Studying the composition and origin of the inner region of our Galaxy—the "Galactic bulge"—is crucial for understanding the formation and evolution of the Milky Way and other galaxies. We present new observational constraints based on a sample of around 18 000 stars in the inner Galaxy, combining Gaia DR3 RVS and APOGEE DR17 spectroscopy. Gaia-RVS

Aims. In this work, we exploit the most robust, old, and cosmology-independent age estimates of individual stars from Gaia DR3 to place a lower bound on the age of the Universe, t U. These constraints can be used as an anchor point for any cosmological model, thus providing an upper limit to the Hubble constant H 0. Methods. Our primary stellar age