Time Evolution of Galaxy Scaling Relations in Cosmological Simulations
  We predict the evolution of galaxy scaling relationships from cosmological,
hydrodynamical simulations, that reproduce the scaling relations of present-day
galaxies. Although we do not assume co-evolution between galaxies and black
holes a priori, we are able to reproduce the black hole mass--velocity
dispersion relation. This relation does not evolve, and black holes actually
grow along the relation from significantly less massive seeds than have
previously been used. AGN feedback does not very much affect the chemical
evolution of our galaxies. In our predictions, the stellar mass--metallicity
relation does not change its shape, but the metallicity significantly increases
from $z\sim2$ to $z\sim1$, while the gas-phase mass-metallicity relation does
change shape, having a steeper slope at higher redshifts ($z\lesssim3$).
Furthermore, AGN feedback is required to reproduce observations of the most
massive galaxies at $z\lesssim1$, specifically their positions on the star
formation main sequence and galaxy mass--size relation.
