Supermassive black holes (SMBHs) lurking at the centers of most galaxies are intriguing objects that are yet to be fully understood.
One of the best tools to investigate the growth and evolution of SMBHs, cosmological simulations, has advanced significantly in recent years
thanks to the rapid development in computing techniques. While numerical resolution of such simulations reach ever so close to resolve
individual star-forming clumps in a galaxy, however, a need for more sophisticated physics in a galaxy-scale simulation has never been greater.
To this end, we introduce a self-consistent numerical framework that includes explicit treatments of feedback from star-forming clumps and SMBHs.
We perform a state-of-the-art cosmological simulation of a SMBH-host galaxy (quasar) at redshift 7.5, and demonstrate that previously undiscussed types of interplay
between galactic components may hold important clues about the growth of SMBHs and their hosts.