AT2022rze is a luminous, ambiguous transient located south-east of the geometric centre of its host galaxy at redshift $z = 0.08$. The host appears to be formed by a merging galaxy system. The observed characteristics of AT2022rze are reminiscent of active galactic nuclei (AGNs), tidal disruption events, and superluminous supernovae. The transient

We present the third installment of the Alma Luminous Star catalogue, aimed at creating the most comprehensive and clean sample of Galactic massive stars. This update extends the sample by adding approximately 2000 OB stars, incorporating astrometric and photometric data from the Gaia Data Release 3 (DR3) alongside spectroscopic information from

Context. Technetium (Tc)-rich M stars have been known for more than 45 years. However, the origin of Tc in these stars, particularly its detection without the concomitant detection of other s-process elements, which are typically produced during asymptotic giant branch (AGB) s-process nucleosynthesis, remains poorly understood. Technetium was first

Asteroseismology of solar-like oscillators provides unique insights into stellar evolution, from the main sequence through to advanced stages of the red giant phase. In this poster, we present a study of the binary fraction among red giants, from combined data from the APOKASC-3 and APO-K2 catalogs with the Gaia Non-Single-Star catalog. This large

We present and analyse the results of the Science Data Challenge 3a (SDC3a, https://sdc3.skao.int/challenges/foregrounds), an epoch of reionization (EoR) foreground-removal exercise organized by the Square Kilometre Array Observatory (SKAO) on SKA simulated data. The challenge ran for 8 months, from 2023 March to October. Participants were provided

Context. We need to understand the spin evolution of massive stars to compute their internal rotation-induced mixing processes, isolate effects of close binary evolution, and predict the rotation rates of white dwarfs, neutron stars, and black holes. Aims. We discuss the spindown of massive main sequence stars imposed by stellar winds. Methods. We