While the mission's primary goal was focused on exoplanet detection and characterization, Kepler made and continues to make extraordinary advances in stellar physics. Stellar rotation and magnetic activity are no exceptions. Kepler allowed for these properties to be determined for tens of thousands of stars from the main sequence up to the red

The archaeological World Heritage Site of Hegra (Mada´in Salih, Al-Hijr), in Saudi Arabia, is often considered the southern capital of the Nabataean Kingdom. Positioned just northeast of the AlUla Valley (where ancient Dadan is located), the Nabataeans recreated several aspects of their northern capital, Petra. They carved more than 130 tombs into

In the standard cosmological model, the assembly of galaxies is primarily driven by the growth of their host dark matter halos. At the centre of these halos, however, baryonic processes take over, leading to the plethora of observed galaxy properties. The coupling between baryonic and dark matter physics is central to our understanding of galaxies

The current studies of microlensing planets are limited by small number statistics. Follow-up observations of high-magnification microlensing events can efficiently form a statistical planetary sample. Since 2020, the Korea Microlensing Telescope Network (KMTNet) and the Las Cumbres Observatory (LCO) global network have been conducting a follow-up

We present the results of a fourth planetary defense exercise, focused this time on the small near-Earth asteroid (NEA) 2023 DZ2 and conducted during its close approach to the Earth in 2023 March. The International Asteroid Warning Network (IAWN), with support from NASA's Planetary Defense Coordination Office (PDCO), has been coordinating planetary

We present a comprehensive analysis of the presence of very massive stars (VMS > 100 M ⊙) in the integrated spectra of 13 UV-bright star-forming galaxies at 2.2 ≲ z ≲ 3.6 taken with the Gran Telescopio Canarias (GTC). These galaxies have very high UV absolute magnitudes (M UV ≃ −24), intense star formation (star formation rate ≃100 − 1000 M ⊙ yr −1