Deep surveys have helped to unveil the history of past and present galaxy mergers, and, in particular, uncovering their tidal debris and co-located globular clusters (GCs). Euclid's unique combination of capabilities (spatial resolution, depth, and wide sky coverage) will make it a groundbreaking tool for galactic archaeology in the Local Universe

We present the discovery of 11 new transiting brown dwarfs (BDs) and low-mass M dwarfs from NASA's Transiting Exoplanet Survey Satellite (TESS) mission: TOI-2844, TOI-3122, TOI-3577, TOI-3755, TOI-4462, TOI-4635, TOI-4737, TOI-4759, TOI-5240, TOI-5467, and TOI-5882. They consist of five BD companions and six very-low-mass stellar companions ranging

This paper presents the first effort to Extend the Investigation of Stellar Populations In RElics (E-INSPIRE). We present a catalogue of 430 spectroscopically confirmed ultra-compact massive galaxies (UCMGs) from the Sloan Digital Sky Survey at redshifts $0.01< z< 0.3$. This increases the original INSPIRE sample eightfold, bridging the gap with the

We obtained 420 high-resolution spectra of Proxima, over 159 nights, using the Near Infra Red Planet Searcher (NIRPS). We derived 149 nightly binned radial velocity measurements with a standard deviation of 1.69 ms ‑1 and a median uncertainty of 55 cms ‑1, and performed a joint analysis combining radial velocities, spectroscopic activity indicators

Central to our understanding of stellar evolution and its impact on processes in our Galaxy and across the Universe is the study of mass-loss. While the general framework is well established, recent JWST observations of objects like NGC 3132 have revealed intricate nebular structures, suggesting complex mass-loss processes likely driven by multiple

The Transiting Exoplanet Survey Satellite (TESS) discovered several new planet candidates that need to be confirmed and characterized with ground-based observations. This is the case of Ross 176, a late K-type star that hosts a promising water-world candidate planet. The star has a radius of R ⋆ = 0.569 ± 0.020 R ⊙ and a mass of M ⋆ = 0.577 ± 0.024