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We ask how the inclusion of various physical heating processes due to themetal content of gas affect the evolution of massive galaxies and compute asuite of cosmological hydrodynamical simulations that follow these systems andtheir supermassive black holes. We use a smoothed particle hydrodynamics codewith a pressure-entropy formulation and a more accurate treatment of the metalproduction, turbulent diffusion and cooling rate based on individual elementabundances. The feedback models include (1) AGN feedback via high velocity BALwinds and Compton/photoionization heating, (2) explicit stellar feedback frommultiple processes including powerful winds from supernova events, stellarwinds from young massive stars and AGB stars as well as radiative heatingwithin Stromgren spheres around massive stars, and (3) additional heatingeffects due to the presence of metals including grain photoelectric heating,metallicity dependent X-ray heating by nearby accreting black holes and fromthe cosmic X-ray background, which are the major improvement in our feedbackmodel. With a suite of zoom-in simulations of 30 halos with $M_{vir} \sim10^{12-13.4}$, we show that energy and momentum budget from all feedbackeffects generate realistic galaxy properties. We explore the detailed role ofeach feedback model with three additional sets of simulations with varyinginput physics. We show that the metal induced heating mechanisms reduce thefraction of accreted stellar material by mainly suppressing the growth ofdiffuse small stellar systems at high redshift but overall have a relativelyminor effect on the final stellar and gas properties of massive galaxies. Theinclusion of AGN feedback significantly improves the ability of ourcosmological simulations to yield realistic gas and stellar properties ofmassive galaxies with reasonable fraction of the final stellar mass accretedfrom other galaxies.

Physics of Galactic Metals: Evolutionary Effects due to Production, Distribution, Feedback & Interaction with Black Holes