Rutgers University Astrophysics Seminar

The formation and evolution of stellar clusters is intrinsically linked to their environment. On the large-scale, star clusters form in galaxies embedded within the cosmic web. On the smaller scales, stars form in hierarchical clusters inside fractal giant molecular clouds (GMCs). This produces a broad diversity of stellar environments, from the old, dense, globular clusters (GCs) that we observe throughout galaxy discs and halos, to young massive clusters (YMCs) in the densest star forming environments of the present, to the field stars we see spread throughout the galaxy disc. The different clustered environments that stars find themselves in has typically been ignored in simulations of galaxy formation, as it occurs on length scales that are below the resolution limit of nearly all simulations. For the first time, we now can now couple galaxy formation simulations to physically-motivated models for star cluster formation (the cluster mass function and cluster formation efficiency) and cluster evolution (stellar evolution, dynamical friction, evaporation, and tidal shocks). These tools allow us to study the impact that the full cosmic environment and history has on the formation of star clusters. With this, we can predict the origin of the GC population in MW-like galaxies, reconstruct the formation history of our own galaxy, and better understand the structures we see in the universe. In this talk, I will explain how we have simulated the co-evolution of galaxies and star clusters in the E-MOSAICS simulations, the primary results (to date) of this project, and the next steps we will be taking to push our understanding of star and galaxy formation forward through simulation.