Research lines

Pristine Inner Galaxy Survey (PIGS) IX. The largest detailed chemical analysis of very metal-poor stars in the Sagittarius dwarf galaxy This paper is the result of a collaboration between ERIS and Pristine. Sara Vitali, one of our PhD students, came to Chile because she wants to see how with phylogenetic techniques we can learn about […]

There is still no model to infere 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. Currently, the well-known distance method known as “Neighbor Joining” clustering

To understand the impact on phylogenetic trees regarding the role of the various chemicalelements, semi-analytical models of chemical evolution are analyzed. These models includeFlex-CE or L-Galaxies, which take into account the non-linear evolution of a structure in acosmological framework and introduce the physics of baryons by using a set of recipeswhose free parameters are chosen

This research line aims to use computational simulations of galaxy evolution (such as [Patricia’s simulation] and L-Galaxies) to study the physical processes that occur throughout the life of galaxies, particularly focusing on the Milky Way. We are particularly interested in the chemical evolution of baryons as galaxies form, including enrichment processes from Type Ia &

We develop 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