2021MNRAS.508.2307V

The kinematic morphology-density relation of galaxies is normally attributed to a changing distribution of galaxy stellar masses with the local environment. However, earlier studies were largely focused on slow rotators; the dynamical properties of the overall population in relation to environment have received less attention. We use the SAMI Galaxy Survey to investigate the dynamical properties of ∼1800 early and late-type galaxies with log (M_*/M_☉) > 9.5 as a function of mean environmental overdensity (Σ₅) and their rank within a group or cluster. By classifying galaxies into fast and slow rotators, at fixed stellar mass above log (M_*/M_☉) > 10.5, we detect a higher fraction (∼3.4σ) of slow rotators for group and cluster centrals and satellites as compared to isolated-central galaxies. We find similar results when using Σ₅ as a tracer for environment. Focusing on the fast-rotator population, we also detect a significant correlation between galaxy kinematics and their stellar mass as well as the environment they are in. Specifically, by using inclination-corrected or intrinsic λ_Re values, we find that, at fixed mass, satellite galaxies on average have the lowest λ_Re_, intr_, isolated-central galaxies have the highest λ_Re_, intr_, and group and cluster centrals lie in between. Similarly, galaxies in high-density environments have lower mean λ_Re_, intr_ values as compared to galaxies at low environmental density. However, at fixed Σ₅, the mean λ_Re_, intr_ differences for low and high-mass galaxies are of similar magnitude as when varying Σ₅ (Δλ_Re_, intr_ ∼0.05, with σ_random = 0.025, and σ_syst < 0.03). Our results demonstrate that after stellar mass, environment plays a significant role in the creation of slow rotators, while for fast rotators we also detect an independent, albeit smaller, impact of mass and environment on their kinematic properties.