Speaker
Description
Satellite galaxies experience multiple physical processes when interacting with their host halos, often leading to the quenching of star formation. In the Local Group, satellite quenching has been shown to be highly efficient, affecting most satellites except the most massive ones. While recent surveys are studying Milky Way analogs to assess how representative our Local Group is, the dominant physical mechanisms behind satellite quenching in Milky Way-mass halos remain under debate. We analyze satellite quenching within the same Milky Way-mass halo, simulated using various widely-used astrophysical codes, each using different code architecture and implementing different supernovae feedback recipes. The goal is to determine whether quenched fractions, quenching timescales and the dominant quenching mechanisms are consistent across codes or if they show sensitivity to the specific hydrodynamic method and supernovae feedback physics employed. We use a suite of high-resolution cosmological zoom-in simulations of a Milky Way-mass halo from the multiple-code AGORA CosmoRun simulations. Our analysis focuses on comparing satellite quenching across the different models and against observational data. We also analyze the dominant mechanisms driving satellite quenching in each model by examining the contributions of various processes commonly proposed in the literature: ram pressure stripping, tidal stripping, galaxy harassment and strangulation.
