Most massive stars are born in binary systems, with 70% expected to interact with a companion within their lifetimes. The consequences of these interactions for subsequent evolutionary stages and for the endpoints of stellar evolution are still not well understood, particularly for the red supergiant (RSG) phase: the final evolutionary stage before

Galaxies exhibit a wide variety of morphologies which contain valuable information about their star formation histories. Having large samples of morphologically classified galaxies is fundamental to understand their formation and evolution. Deep learning algorithms have proven to be extremely successful for morphological classification of galaxies

We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe

In this new era of extensive variability surveys, classical pulsators such as RR Lyrae stars (RRLs) and Classical Cepheids play a crucial role. We focus our attention on the use of RRLs as tracers of the oldest stellar populations of the Galactic halo (Halo) and we compare their properties to those hosted by nearby Milky Way (MW) satellites. These

In order to connect galaxy clusters to their progenitor protoclusters, we must constrain the star formation histories within their member galaxies and the timescale of virial collapse. In this paper we characterize the complex star-forming properties of a z = 2.5 protocluster in the COSMOS field using ALMA dust continuum and new Very Large Array CO

We propose a dedicated, ultra-deep spectroscopic survey in the near infrared (NIR), that will target a mass-limited sample of galaxies during two of the most fundamental epochs of cosmic evolution: the formation of the first galaxies (at z ≳ 6; cosmic dawn), and at the peak of galaxy formation activity (at redshift z∼1-3; cosmic noon). By way of