This research line aimed to use computational simulations of galaxy evolution (such as CIELO and L-Galaxies) to study the physical processes that occur throughout the life of galaxies, with special focus on the Milky Way. We were particularly interested in the chemical evolution of baryons as galaxies form, including enrichment processes from Type IA & II supernovae, AGB stars, and other possible sources. Simulations allow us to trace the chemical enrichment history of the interstellar medium and the stellar populations that form from it as galaxies form and evolve. We used isolated simulations tailored to a specific problem, where different physical processes are described with large details and time resolution, as well as cosmological simulations, which model the evolution of a variety of galaxies within the adopted cosmological framework. In this way, we could identify stars formed in the progenitors of today’s galaxies as well as those originating from satellites. The simulations provide spatial distributions, ages, chemical abundances, velocity dispersions of baryons (gas and stars) in galaxies, and also describe their interaction with the surrounding media. These simulations were crucial for applying and testing new concepts, methodologies, and techniques adopted from phylogenetics.
Highlight: Workshop in Puerto Varas: https://www.evolgal4d.com/dcc
English 
Español