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

Mergers are fundamental to our understanding of the processes driving the evolution of the structure and morphology of galaxies, star formation, active galactic nucleus activity, and the redistribution of stellar mass in the Universe. Determining the fraction and properties of mergers across cosmic time is critical to understanding the formation of

The Cygnus-X complex is the most powerful massive star-forming region at less than 2 kpc from us. The region has been largely studied along the last decades, but there has been no extensive and homogeneous spectroscopic survey on its stellar population despite its importance to our limited knowledge of star formation and evolution of star-forming