Description
The impact of the large-scale cosmic environment on galactic properties remains an open question in galaxy formation. While dark matter halos initially follow linear evolution, their subsequent growth is shaped by complex, non-linear interactions with their surroundings. Observational evidence suggests that proximity to large-scale structures, such as cosmic filaments, can induce quenching in galaxies, yet the underlying physical mechanisms remain unclear. In this talk, I will present a numerical experiment whereupon we make given Milky-Way-like halos form at increasing distances from a cosmological filament. This allows us to reveal that, while the mass and virial radius of the halos remain largely unaffected, their spin and shape orientation can vary by up to 80%, highlighting the strong influence of large-scale structures on their inner structure. By adding baryonic physics, and notably feedback, I will present how the large-scale environment affects feedback processes on small scale, shedding new light on the role of the cosmic web in regulating galaxy evolution. This reflects a differential accretion in the circumgalactic medium, which, in turn regulates gas inflows in the galaxy and ultimately star formation.
