We present the discovery and validation of a super-Earth planet orbiting the M dwarf star TOI-1846 (TIC 198385543). The host star ( $K_{\rm mag} = 9.6$) is located 47 pc away and has a radius of $R_\star = 0.41 \pm 0.01$ $\rm \, R_\odot$, a mass of $M_\star = 0.40 \pm 0.02$ $\rm \, M_\odot$ and an effective temperature of $T_{\rm eff} = 3568 \pm 44

We identify stellar tidal debris from the ω Centauri (ω Cen) system among field stars in the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey via chemical tagging using a neural network trained on APOGEE observations of the ω Cen core. We find a total of 463 ω Cen debris candidates have a probability P > 0.8 of sharing common

Context. Despite predictions from planetary population synthesis models indicating that such systems should be exceedingly rare, short-period gas giants do exist around low-mass stars (T eff < 4965 K), albeit at lower frequency than around hotter stars. Aims. By combining data from the Transiting Exoplanet Survey Satellite (TESS) and ground-based

Context. Nuclear rings are composed of gaseous material and/or stars and have a typical size ranging from 100 s pc to ~1 kpc. Their study is crucial to unravelling the processes involved in the evolution of the central regions of galaxies. Nuclear rings are long-lived structures, which allows the molecular gas inside to become sufficiently dense to

WASP-4 b is a hot Jupiter exhibiting a decreasing orbital period, prompting investigations into potential mechanisms driving its evolution. We analysed 173 transit light curves, including 37 new observations, and derived mid-transit timings with EXOFAST, forming the most extensive transit timing variation (TTV) data set for this system. Adding 58

Context. O Vz stars are identified by optical spectra where the He II λ4686 absorption line is more intense than any other He line, suggesting they may be less luminous, less evolved, and closer to the zero-age main sequence (ZAMS). Despite ongoing debate, these stars remain candidates for understanding the early evolutionary stages of O-type stars