Cosmological simulations have become indispensable tools for understanding structure formation in the Universe. By modeling the complex interplay of gravity, baryonic physics, and galaxy formation across vast scales, these simulations provide crucial insights into the evolution of galaxies and the largescale structure of the cosmos.
This project aims to address several outstanding challenges in the field of galaxy formation, including: Impact of Baryons on Large-Scale Structure: We will investigate how baryonic processes, such as star formation and feedback from supernovae and active galactic nuclei (AGN), influence the growth of cosmic structures on the largest scales. Galaxy Formation in Clusters: Utilizing the Cluster-EAGLE simulations, we will generate accurate predictions for galaxy stellar masses and luminosity functions within clusters, enabling detailed comparisons with observations and a better understanding of galaxy evolution in dense environments. Milky Way Formation and Evolution: By combining simulations with observational data on stellar populations, we will investigate key aspects of our Galaxy's formation, including the origin of the thick disk and the accretion and mixing of low-metallicity gas.
Dwarf Galaxy Formation and Dark Matter Halos: We will explore the physics of halo expansion and its impact on the observed properties of dwarf galaxies. This includes investigating observational signatures in chemical abundance space to constrain models of star formation and feedback. Ultra Diffuse Galaxies: We will utilize simulations to investigate the potential existence of undiscovered ultra-diffuse galaxies in the Local Group. AGN Feedback in Dwarf Galaxies: We will study the impact of AGN feedback on the evolution of dwarf galaxies, considering the growing observational evidence for its importance.
To achieve these goals, we will continue to develop and refine our state-of-the-art cosmological hydrodynamics simulation code, incorporating the most up-to-date physical models and numerical methods.
