Context. The outer Galactic halo remains relatively unexplored, particularly regarding its metallicity distribution, merger debris, and the population of very and extremely metal-poor ([Fe/H] < -2.5) stars. Aims. Using photometric metallicities from the Pristine survey data release 1 (PDR1) and Pristine-Gaia synthetic (PGS) catalogue and Gaia DR3

Observations show that the first galaxy clusters were already assembling by z ~ 2-3, earlier and more massive than predicted by standard cosmological models. Understanding how these dense environments affect star formation provides direct insight into how galaxies form and evolve. SPOTLESS (Searching for Protoclusters through Observations Tracing

MATLAS-2019 (also known as NGC5846-UDG1) has attracted significant attention due to the ongoing debate surrounding its globular cluster (GC) population, with several studies addressing the issue, yet reaching little consensus. For this paper, we took advantage of HST's multi-wavelength coverage (F475W, F606W, and F814W observations) with the

In addition to comprehensive surveys of the Milky Way (MW) bulge, disk, and halo, the Apache Point Galactic Evolution Experiment (APOGEE) project observed seven dwarf spheroidal satellites (dSphs) of the MW: Carina, Sextans, Sculptor, Draco, Ursa Minor, Bootes 1, and Fornax. APOGEE radial velocities, stellar parameters, and Gaia EDR3 proper motions

Aims. We aim to measure the evolution of individual galaxies around the star formation main sequence (SFMS) during the last gigayear as a function of their stellar mass to quantify how much of its scatter is due to short-term variability. Methods. We derived star formation histories using full spectral fitting for a sample of 8960 galaxies from the

We present a spatially resolved analysis of galaxy quenching within the Spiderweb Protocluster at z ∼ 2.16, combining deep imaging from the James Webb Space Telescope (JWST) and the Hubble Space Telescope. Utilizing pixel-by-pixel spectral energy distribution fitting, we derive maps of stellar mass, star formation rate (SFR), specific SFR (sSFR)