I use cosmological simulations to study the coevolution of massive black holes and their host galaxies. My papers have investigated wandering black holes, AGN feedback, and the MBH–M★ relation. You can access them on my ADS/SciX library, or view some key figures below.

Figure 5 from Weller et al. 2023

Galactocentric distance (thick green line) and Eddington ratio (thin orange line) vs. time for a wandering intermediate-mass black hole in the ASTRID simulation. The Eddington ratio is high during the infall, and spikes when the distance is close to a minimum. The middle and bottom panels zoom in for better visualization. See Weller et al. 2023 (Figure 5).

Figure 9 from Weller et al. 2025

Maps of the gas density colored by temperature (top row, redder is hotter) and stellar density colored by age (bottom row, redder is older) for a galaxy in the TNG100 simulation. Brightness indicates the mass density. Each column shows the galaxy at a particular snapshot, and all boxes have a side length of 50 ckpc/h. At z~3 AGN kinetic feedback turns on, and gas is heated and expelled from the galaxy's center, quenching star formation. At z~1 new gas is brought into the galaxy via mergers with surrounding galaxies, reactivating star formation. See Weller et al. 2025 (Figure 9).