Speaker
Description
In light of recent high-redshift observations from JWST, it is imperative for large-volume cosmological simulations to provide accurate predictions on galaxy formation in the early Universe. However, low-resolution simulations such as IllustrisTNG or EAGLE have limited validity in this regime, not least because they have to rely on ISM sub-grid modeling that does not entirely reflect our modern, improved theoretical view of the ISM physics (such as the importance of metallicity and turbulence). We are proposing a new sub-grid ISM model, based on an equilibrium between gas cooling, stellar feedback, and turbulence, with gas contained in three distinct phases. To ensure that the model describes the underlying physical reality rather than providing a tuned fitting function, we use results from high-resolution, individual-galaxy simulations to develop theoretical prescriptions for the key pieces of physics.
In my talk, I will present progress on the feedback implementation, with the intention of facilitating a discussion on how high-resolution simulations can be used to determine simplified, theoretical prescriptions for feedback mechanisms in the ISM.
