Speaker
Description
Understanding the response of dark matter to baryonic feedback is crucial before dwarf galaxy observations can be used to constrain dark matter particle physics. For the last decade, the stellar-to-halo mass ratio ($M_{\star}/M_{200}$) has been widely regarded as the single most important quantity in determining the expected effect of most baryonic feedback models on cold dark matter halos at $z=0$. In this talk, I will present results from the EDGE2 state-of-the-art radiation-hydrodynamical simulations that suggest that $M_{\star}/M_{200}$ ratio is only partially correlated with dark matter core formation. I will show that the dark matter density at $z=0$ is highly sensitive to the specific formation history of a galaxy, and introduce a new quantity that can be used to accurately predict the impact of baryonic feedback on dark matter halos (Muni et al 2024). I will also present a new technique, first of its kind, to examine variations in the gravitational potential at the centres of EDGE halos on timescales shorter than their dynamical time (< 5 Myr). I will provide evidence that these potential fluctuations are directly driven by supernova feedback and discuss their correlation with the presence of cores (Muni et al in prep 2025).
