The processes driving the formation and evolution of late-type galaxies continue to be a debated subject in extragalactic astronomy. Investigating stellar kinematics, especially when combined with age estimates, provides crucial insights into the formation and subsequent development of galactic discs. Post-processing of exceptionally high-quality

Aims. We carried out a project involving the systematic analysis of microlensing data from the Korea Microlensing Telescope Network survey. The aim of this project is to identify lensing events with complex anomaly features that are difficult to explain using standard binary-lens or binary-source models. Methods. Our investigation reveals that the

A pair-instability supernova (PISN) prevents black hole (BH) formation from stellar collapse within the approximate mass range M ∈ [65, 130] M ⊙. However, such BHs may form hierarchically through merging ancestral BHs, whose properties determine those of the "child" one: mass, spin, and recoil velocity. Crucially, the child will leave its host

We combine JWST/NIRCam and Subaru/MOIRCS dual Paβ+Hα narrowband imaging to trace the dust attenuation and the star formation activities of a sample of 43 Hα emitters at the core of one of the most massive and best-studied clusters in formation at the cosmic noon: the Spiderweb protocluster at z = 2.16. We find that most Hα emitters display Paβ/Hα

We report the initial result of our Paβ narrowband imaging on a protocluster with the JWST Near Infrared Camera (NIRCam). As NIRCam enables deep narrowband imaging of rest-frame near-infrared lines at z > 1, we target one of the most studied protoclusters, the Spiderweb protocluster at z = 2.16, in which previous studies have confirmed more than a

The identification of new white dwarfs (WDs) polluted with heavy elements is important since they provide a valuable tool for inferring the chemical properties of putative planetary systems accreting material on their surfaces. The Gaia space mission has provided us with an unprecedented amount of astrometric, photometric, and low-resolution (XP)