The literature on horn antennas dedicated to radio astronomy and satellite communications applications is very extensive and at times disjointed, relevant contributions being distributed as far back as from the 60's until the present today. This work combines a compact but complete review of the different theories, methodologies and techniques used

We study ultra-diffuse galaxies (UDGs) in zoom in cosmological simulations, seeking the origin of UDGs in the field versus galaxy groups. We find that while field UDGs arise from dwarfs in a characteristic mass range by multiple episodes of supernova feedback (Di Cintio et al.), group UDGs may also form by tidal puffing up and they become quiescent

Transmission spectroscopy using high-resolution spectrographs is quickly becoming a major tool to detect and understand planetary atmospheres, from ultra hot Jupiters to Neptunes-size planets. The CARMENES spectrograph started operations in 2016, and since then we have been using it for the study of planetary atmospheres taking advantage of it

This paper presents the results of an archaeoastronomical study of the Iberian Iron Age cave-sanctuary of Cueva Santa del Cabriel, near the town of Mira in the province of Cuenca, Castilla-La Mancha, central Spain, together with a review of the latest archaeological and ethnographical data about the site. We found that the cave's 12 m-long access

Active galactic nuclei (AGNs) with intermediate radio powers are capable of driving multiphase outflows in galaxy bulges, and are also more common than their high-radio-power counterparts. In-depth characterization of the typical host galaxies and likely triggering mechanisms for this population is therefore required in order to better understand

Transmission spectroscopy is an important technique to probe the atmospheres of exoplanets. With the advent of the Transiting Exoplanet Survey Satellite (TESS) and, in the future, of the PLAnetary Transits and Oscillations of stars (PLATO), more and more transiting planets around bright stars will be found and the observing time of current large