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As computational resolution of modern cosmological simulations reach ever soclose to resolving individual star-forming clumps in a galaxy, a need for"resolution-appropriate" physics for a galaxy-scale simulation has never beengreater. To this end, we introduce a self-consistent numerical framework thatincludes explicit treatments of feedback from star-forming molecular clouds(SFMCs) and massive black holes (MBHs). In addition to the thermal supernovaefeedback from SFMC particles, photoionizing radiation from both SFMCs and MBHsis tracked through full 3-dimensional ray tracing. A mechanical feedbackchannel from MBHs is also considered. Using our framework, we perform astate-of-the-art cosmological simulation of a quasar-host galaxy at z~7.5 for~25 Myrs with all relevant galactic components such as dark matter, gas, SFMCs,and an embedded MBH seed of ~> 1e6 Ms. We find that feedback from SFMCs and anaccreting MBH suppresses runaway star formation locally in the galactic coreregion. Newly included radiation feedback from SFMCs, combined with feedbackfrom the MBH, helps the MBH grow faster by retaining gas that eventuallyaccretes on to the MBH. Our experiment demonstrates that previously undiscussedtypes of interplay between gas, SFMCs, and a MBH may hold important clues aboutthe growth and feedback of quasars and their host galaxies in the high-redshiftUniverse.

High-redshift Galaxy Formation with Self-consistently Modeled Stars and Massive Black Holes: Stellar Feedback and Quasar Growth