The C-19 star stream has the abundance characteristics of an unusually metal-poor globular cluster but kinematically is uncharacteristically hot and wide for a cluster stream, having a line-of-sight velocity dispersion of 7 ± 2 km s ‑1 and a 1σ width of 240 pc. We show that the tidal dissolution of an old, lower-mass globular cluster in a cold dark

We aim to determine the physical properties of OB stars from the multi-epoch Binarity at LOw Metallicity (BLOeM) spectroscopic survey of the Small Magellanic Cloud using the Very Large Telescope/Fibre Large Array Multi-Element Spectrograph. We apply a pipeline designed to analyse large spectroscopic samples of OB stars to the co-added, initial nine

We present extensive follow-up time-series photometry of WD J0049‑2525, the most massive pulsating white dwarf currently known, with T eff = 13,020 K and log g = 9.34 cm s ‑2. The discovery observations detected only two significant pulsation modes. Here, we report the detection of 13 significant pulsation modes ranging from 170 to 258 s based on

The morphology of circular polarization profiles from solar spectropolarimetric observations encodes information about the magnetic field strength, inclination, and line-of-sight velocity gradients. Previous studies used manual methods or unsupervised machine learning (ML) to classify the shapes of circular polarization profiles. We trained a

HD 138965 is a young A type star and member of the nearby young Argus association. This star is surrounded by a broad, bright debris disc with two temperature components that was spatially resolved at far-infrared wavelengths by Herschel. Here, we present Atacama Large Millimiter/Submillimeter Array (ALMA) millimetre-wavelength imaging of the cool

Context. The study of resonant oscillation modes in low-mass red giant branch stars enables us to infer their ages with exceptional (∼10%) precision. This unlocks the possibility to reconstruct the temporal evolution of the Milky Way at early cosmic times. Ensuring the accuracy of such a precise age scale is a fundamental but difficult challenge