What role does stellar mass and halo mass play in determining galaxy quenching and morphological transformations for Dark Sage and IllustrisTNG galaxies?

Investigating the star formation quenching of central galaxies in the context of the stellar-to-halo mass relation (SHMR) has emerged as a valuable way to understand the roles of halo mass vs. stellar mass on galaxy quenching. We compare predictions for this using two very different galaxy formation models, the semi-analytic model DARK SAGE and the hydrodynamic simulation IllustrisTNG. In addition to galaxy quenching, we extend past studies to also include satellite galaxies, and investigate morphological transformation. Some of our results are as follows: Dark Sage and IllustrisTNG predict that both halo mass and stellar mass play a role in driving quenching and morphological transformation, with neither mass being solely responsible. However, the models predict that quenching and morphological transformation do not track each other simply. Both models also predict that satellite galaxies behave similar to centrals. However, the two models are quite different in detail, with Dark sage producing a SHMR with much larger scatter than IllustrisTNG