Several phenomenological aspects of low-luminosity neutron star transients, such as atolls, remain poorly understood. One such source, MAXI J1807+132, entered its latest outburst in 2023 July. To thoroughly characterize this outburst, we conducted an extensive observational campaign spanning radio to X-ray wavelengths. Here we present the results

Dormant black holes in X-ray transients can be identified by the presence of broad Hα emission lines from quiescent accretion discs. Unfortunately, short-period cataclysmic variables can also produce broad Hα lines, especially when viewed at high inclinations, and are thus a major source of contamination. Here we compare the full width at half

Aims. We analyse ESPRESSO data for the stars HD 10700 (τ Ceti), HD 20794 (e Eridani), HD 102365, and HD 304636 acquired via its Guaranteed Time Observations (GTO) programme. We characterise the stars' radial velocity (RV) signals down to a precision of 10 cm/s on timescales ranging from minutes to planetary periods falling within the host's

We present the analysis of the stellar populations and kinematics of the globular cluster (GC)-rich ultra-diffuse galaxy (UDG), PUDG-R21, using spectroscopic observations obtained with the Keck Cosmic Web Imager. The recessional velocity is measured to be 5536 $\pm$ 10 km s ‑1, confirming its association with the Perseus Cluster. The galaxy

Context. The formation and evolution of ultra-short-period (USP) rocky planets is poorly understood. However, it is widely thought that these planets could not have formed at their present-day close-in orbits, but instead migrated inwards through interactions with outer neighbours. Aims. We aim to confirm and characterise the USP Earth-sized

We present a detailed optical and near-IR (NIR) spectral analysis of J-138717, a post-starburst galaxy at z = 1.8845 observed with JWST/NIRSpec, for which we derive a stellar mass of 3.5±0.2×10 10 M ⊙ and a stellar velocity dispersion of 198±10 km s ‑1. We estimate an age of ∼0.9 Gyr and a subsolar metallicity (between ‑0.4 and ‑0.2 dex). We find