Central to our understanding of stellar evolution and its impact on processes in our Galaxy and across the Universe is the study of mass-loss. While the general framework is well established, recent JWST observations of objects like NGC 3132 have revealed intricate nebular structures, suggesting complex mass-loss processes likely driven by multiple

The Transiting Exoplanet Survey Satellite (TESS) discovered several new planet candidates that need to be confirmed and characterized with ground-based observations. This is the case of Ross 176, a late K-type star that hosts a promising water-world candidate planet. The star has a radius of R ⋆ = 0.569 ± 0.020 R ⊙ and a mass of M ⋆ = 0.577 ± 0.024

Context. It is important to detect and study circumstellar disks around late-M and brown dwarfs of nearby young associations to understand how these very low-mass objects form and how rocky planets form around them. The detection of new very low-mass members of nearby young associations will also significantly improve our current understanding of

Context. The circumstellar environments of planetary nebulae (PNe) are remarkably chemically rich astrophysical laboratories, proving useful for studies of the ionization of atoms and the formation of simple and complex molecules. The new generation of high-sensitivity receivers opens up the possibility to carry out the deep observations needed to

One of the key steps in Cosmic Microwave Background (CMB) data analysis is component separation to recover the CMB signal from multi-frequency observations contaminated by foreground emissions. Needlet Internal Linear Combination (NILC) is one of the successful methods that applies the minimum variance estimation technique to a set of needlet

As surveys grow, the challenge is how to explore and interpret the increasing quantity of data. Integral field spectroscopic (IFS) galaxy surveys are a good example of how data have grown in complexity and in volume. In order to find complex relations between the spatially resolved structures of galaxies and their accretion histories, we combine