ABSTRACT:
Cosmic environment play a critical role in the picture of galaxy evolution. I will present a multifaceted approach---drawing on observational data, analytic models, and cosmological hydrodynamic simulations---to understanding the evolution of star formation and gas flows in galaxies and its environmental dependence, from massive galaxy clusters down to the Local Group. A third of all low-mass galaxies are satellites in groups or clusters, and satellite quenching is the dominant process for building the quiescent (red-sequence) population at low mass. I will show that the star formation histories of satellite galaxies follow a delayed-then-rapid quenching scenario, with strong dependence on stellar mass, and I will discuss these results in light of the physical mechanisms of environmental quenching, including their redshift evolution. I also will demonstrate that the spatial extent of environmental quenching is governed by satellites that orbit beyond the virial radius of their host halo. I will finish by discussing recent work on isolated dwarf galaxies and their host halos, demonstrating that their gas flow at late cosmic times is largely divored from the cosmic web and instead is governed largely by rotational support and stellar feedback.