We provide an early assessment of the imaging capabilities of the Euclid space mission to deeply probe nearby star-forming regions and associated very young open clusters, and in particular, to determine to which extent it can shed light into the newborn free- floating planet population. This paper focusses on a low-reddening region observed in

EMIR was shipped to the GTC on May 2016 and had its first light on June 2016. After a short and intense commissioning period, a Scientific Verification phase took place in the first half of 2017 and the instrument began its routinely operation at the GTC by the end of that year. Since the beginning, the EMIR performances have been severely hampered

Beta Pictoris (BP) is a planetary system composed of an A-type star, two planets, and two debris disks. The short-term variability and the presence of absorption lines in the star indicate the existence of cometary material falling into the star. In this work, we present an ongoing investigation into the cause of the exocometary activity in the BP

The study of chemical abundances of stars that host planets is critical to our current un- derstanding of the structure, formation, evolution of rocky planets, and to understand the evolution and assembly of the Milky Way. Here we present the abundances of magnesium (Mg) and silicon (Si) for 314 dwarf stars with spectral types in the range K7.0-M5

WISEA J181006.18‑101000.5 (WISE1810) is the nearest metal-poor ultracool dwarf to the Sun. It has a low effective temperature and has been classified as an extreme early-T subdwarf. However, methane, the characteristic molecule of the spectral class T, was not seen in the previous low-resolution spectrum. Using the 10.4 m Gran Telescopio Canarias

We present preliminary results based on a homogeneous analysis of the DEep Spectra of Ionized REgions Database (DESIRED), a compilation of high signal-to-noise ratio optical spectra of photoionized nebulae. The database comprises more than 1800 spectra of Galactic and extragalactic H II regions and H II galaxies, and more than 200 spectra of