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We present a novel implementation of supermassive black hole (SMBH)formation, dynamics, and accretion in the massively parallel tree+SPH code,ChaNGa. This approach improves the modeling of SMBHs in fully cosmologicalsimulations, allowing for a more de- tailed analysis of SMBH-galaxyco-evolution throughout cosmic time. Our scheme includes novel, physicallymotivated models for SMBH formation, dynamics and sinking timescales withingalaxies, and SMBH accretion of rotationally supported gas. The sub-gridparameters that regulate star formation (SF) and feedback from SMBHs and SNeare optimized against a comprehensive set of z = 0 galaxy scaling relationsusing a novel, multi-dimensional parameter search. We have incorporated our newSMBH implementation and parameter optimization into a new set of highresolution, large-scale cosmological simulations called Romulus. We presentinitial results from our flagship simulation, Romulus25, showing that our SMBHmodel results in SF efficiency, SMBH masses, and global SF and SMBH accretionhistories at high redshift that are consistent with observations. We discussthe importance of SMBH physics in shaping the evolution of massive galaxies andshow how SMBH feedback is much more effective at regulating star formationcompared to SNe feedback in this regime. Further, we show how each aspect ofour SMBH model impacts this evolution compared to more common approaches.Finally, we present a science application of this scheme studying theproperties and time evolution of an example dual AGN system, highlighting howour approach allows simulations to better study galaxy interactions and SMBHmergers in the context of galaxy-BH co-evolution.

The Romulus Cosmological Simulations: A Physical Approach to the Formation, Dynamics and Accretion Models of SMBHs