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

TOI-1518b, a hot Jupiter around a late A-type star, is one of the few planetary systems that transit the edge of the stellar surface (the impact parameter b~0.9) among hot Jupiters around hot stars (Cabot et al. 2021). The host star's high rotation speed (Vsini s~85 km s -1) and the planet's nearly polar orbit (λ~120 deg) may cause a nodal

Despite being the most abundant classes of known exoplanets, super-Earths and mini-Neptunes are absent in our Solar System, and the exact reason for this is still unknown. Some models suggest that cold-Jupiters play a major role in the formation of inner low-mass planets. This could explain the current architecture of our Solar System, and the

In recent years, a new generation of optical intensity interferometers has emerged, leveraging the existing infrastructure of Imaging Atmospheric Cherenkov Telescopes (IACTs). The MAGIC telescopes host the MAGIC-SII system (Stellar Intensity Interferometer), implemented to investigate the feasibility and potential of this technique on IACTs. After

Context. M-dwarf stars are the most common of potential exoplanet host stars in the Galaxy. It is therefore very important to understand planetary systems orbiting such stars and to determine the physical parameters of such planets with high precision. Also with the launch of the James Webb Space Telescope (JWST) the observation of atmospheric

The Transiting Exoplanet Survey Satellite (TESS) provides a continuous suite of new planet candidates that need confirmation and precise mass determination from ground-based observatories. This is the case for the G-type star TOI-1710, which is known to host a transiting sub-Saturn planet (M p = 28.3 ± 4.7 M ⊕) in a long-period orbit (P = 24.28