We investigate how the environment affects the galaxy structure in the Spiderweb protocluster at z = 2.16 using JWST/NIRCam F115W, F182M, and F410M imaging (rest-frame ~3500 Å to 1.4 μm). We performed homogeneous multi-wavelength parametric modelling of the single-Sérsic and bulge--disc decomposition for a sample of 103 Spiderweb member galaxies

Asteroseismic estimates of the magnetic field strength in the radiative interior of red giant stars depend strongly on the internal stellar structure derived from models. Since red-giant-branch merger products have been shown to be able to possess a different core structure than single stars of the same mass, we investigated how a mass-gain history

Dwarf galaxies, in the ΛCDM framework, are expected to dominate the galaxy number density at all redshifts. As such, studying active galactic nuclei (AGN) in these systems, including characterizing their local environments and emission properties, is essential in obtaining a comprehensive view of the AGN population and their influence on their host

Context. The Pennsylvania-Toruń Planet Search, which operates on a sample of ~1000 northern-hemisphere stars, has been underway since 2004. Stars with radial velocity (RV) amplitudes exceeding 2 km s -1 represent a backup subprogram sample dedicated to monitoring binary stars with multiple instruments. Aims. We used almost 21 years of combined RV

White dwarf--brown dwarf (WD+BD) binaries are rare laboratories for probing both substellar survival through post-main-sequence evolution and the physics of strongly irradiated atmospheres. We present time-resolved eclipse photometry and radial-velocity confirmation of J0404+1112, a compact (P = 2.93 hr), totally eclipsing WD+BD system initially

The solar convective envelope generates, by the dynamo effect, a surface magnetic field whose strength evolves on an 11-year cycle, with a change in polarity at the end of each cycle. A similar magnetic variability exists in other solar-type stars, influencing their dynamics. Furthermore, solar-like oscillators exhibit acoustic modes whose