Research lines

Unveiling the formation channels of stellar halos through their chemical fingerprints Stellar halos around galaxies contain key information about their formation and assembly history. Using simulations, we can trace the origins of different stellar populations in these halos, contributing to our understanding of galaxy evolution. Aims. We aim to investigate the assembly of stellar halos […]

There is still no model to infer phylogeny of galaxy evolution. We are developing such a method, by considering the rates of metal production by supernova and stellar winds based on gas density and star formation histories and comparing this method to chemical data.

This line aims at merging the astronomical lines on chemical abundance determination and galaxy evolution modeling by building and analyzing trees and networks. Here is where the key idea of ERIS to apply the principles and methods of phylogenetics to the evolution of galaxies happens. The well-known distance method known as “Neighbor Joining” clustering in

To understand the impact on phylogenetic trees regarding the role of the various chemical elements, stand-alone analytical models of chemical evolution are also analyzed. These models include FlexCE, which assumes a predefined star-formation history for an isolated galaxy and tracks the enrichment of the gas and stars as the system evolves. Such models are complementary

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

We developed methods to determine chemical composition in stars. ERIS attributes the chemical abundances imprinted in stellar atmospheres as the heritable marker for the phylogenetic signal of galaxy evolution. The problem of determining stellar atmospheric parameters (effective temperature, surface gravity, overall metallicity, etc.), and subsequently determining individual chemical abundances, is complex. Despite the rapid development