Context. Among the blazars whose emission has been detected up to very high-energy (VHE; 100 GeV

Cygnus OB2, within the Cygnus X complex, is one of the most active star-forming regions of our Galaxy, hosting hundreds of O and B-type stars across different evolutionary stages. Despite extensive studies of its massive stars, Cygnus OB2 exhibits a notable absence of fast rotating stars (v sin i > 200 ), which challenges existing models of massive

The star-formation main sequence (SFMS) and the mass-metallicity relation (MZR) are two tight, fundamental relations that govern galaxy evolution. Their intrinsic scatter originates from some galaxies having above- or below-average SFR and metallicity, which leads to the question of whether galaxies which are offset from the relations stay there

Ultra-deep optical imaging surveys have reached unprecedented depths (≳30 mag arcsec ‑2; 3σ, 10″ × 10″), thus facilitating the study of very faint galactic structures. However, the ultraviolet bands, which are key to the study of stellar populations, remain essentially unexplored at these depths. In this paper, we present a detailed surface

We present an innovative deblending method that uses the variation of seeing with wavelength to isolate AGN and host galaxy spectra in IFS data. We demonstrate its efficacy through application to MUSE observations of the type I AGN MRK 926.

The Cygnus OB2 association forms the core of the Cygnus-X complex, the closest region to Earth with significant massive star formation. Situated less than 2 kpc away, Cygnus OB2 hosts a young population of OB stars (aged between 1.5 and 6 Myr), making it an ideal laboratory for testing evolutionary channels of massive stars. The newly commissioned