Speaker
Description
In our understanding of galaxy evolution, dwarf galaxies represent a key ingredient, as these act as the building blocks of larger galaxies, and they can help us understand the early stages of the first galaxies in the Universe. In the context of simulations, the dwarf galaxy mass scale represents a challenge itself just to be able to resolve them within a cosmological box. State-of-the-art zoom-in simulations solve this issue but still rely on the chosen sub-grid physics model to account for the processes involved. For instance, supernova feedback is a fundamental process regulating the evolution of dwarf galaxies and, therefore, sensitive to the chosen model. LYRA is a new set of zoom-in cosmological hydrodynamical simulations designed to resolve the formation and evolution of dwarf galaxies in great detail. These simulations have a baryonic mass resolution of 4 $M_\odot$, hence resolving individual stars above that and supernovae shocks self-consistently, removing the need for sub-grid physics implementation of this process. These simulations offer a promising avenue for advancing our understanding of the formation and assembly of dwarf galaxies, their stellar populations, and the influence of baryon physics in their assembly history. I will present some results from these simulations, focusing on the connection between the stellar distribution and the underlying dark matter halo. I will show how the stellar morphology evolves and how it can provide information on the effects of reionisation and the dark matter halo.
