We present the first measurement of H I mass of star-forming galaxies in different large scale structure environments from a blind survey at z ~ 0.37. In particular, we carry out a spectral line stacking analysis considering 2875 spectra of colour-selected star-forming galaxies undetected in H I at 0.23 < z < 0.49 in the COSMOS field, extracted

Over the past three decades, astronomers have discovered that small, rocky planets in temperate orbits are common around our neighboring stars. Whether or not these planets can maintain atmospheres is an open question in the field. Recently, considerable attention in this search has been focused on M dwarfs stars, as their small sizes make it

Context. In recent years, a number of Lyman continuum (LyC) leaker candidates have been found at intermediate redshifts, providing insight into how the Universe was reionised at early cosmic times. There are now around 100 known LyC leakers at all redshifts, which enables us to analyse their properties statistically. Aims: Here, we identify new LyC

The study of the rare decays B →K (*)ν ν ¯ offers a window into the dynamics operating at the electroweak scale, allowing studies of the Standard Model and searches for heavy new physics. However, the analysis of these decays is also potentially sensitive to the on shell production of new light bosons X through the process B →K (*)X . In particular

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

Primordial abundances of light elements are sensitive to the physics of the early Universe and can directly constrain cosmological quantities, such as the baryon-to-photon ratio $\eta _{10}$, the baryon density, and the number of neutrino families. Deuterium is especially suited for these studies: its primordial abundance is sensitive and