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We apply Monte Carlo Markov Chain (MCMC) methods to large-scale simulationsof galaxy formation in a LambdaCDM cosmology in order to explore how starformation and feedback are constrained by the observed luminosity and stellarmass functions of galaxies. We build models jointly on the Millennium andMillennium-II simulations, applying fast sampling techniques which allowobserved galaxy abundances over the ranges 7<log(M*/Msun)<12 and z=0 to z=3 tobe used simultaneously as constraints in the MCMC analysis. When z=0constraints alone are imposed, we reproduce the results of previous modellingby Guo et al. (2012), but no single set of parameters can reproduce observedgalaxy abundances at all redshifts simultaneously, reflecting the fact thatlow-mass galaxies form too early and thus are overabundant at high redshift inthis model. The data require the efficiency with which galactic wind ejecta arereaccreted to vary with redshift and halo mass quite differently thanpreviously assumed, but in a similar way as in some recent hydrodynamicsimulations of galaxy formation. We propose a specific model in whichreincorporation timescales vary inversely with halo mass and are independent ofredshift. This produces an evolving galaxy population which fits observedabundances as a function of stellar mass, B- and K-band luminosity at allredshifts simultaneously. It also produces a significant improvement in twoother areas where previous models were deficient. It leads to present day dwarfgalaxy populations which are younger, bluer, more strongly star-forming andmore weakly clustered on small scales than before, although the passivefraction of faint dwarfs remains too high.

monthly notices of the royal astronomical society

Simulations of the galaxy population constrained by observations from  z=3 to the present day: implications for galactic winds and the fate of their  ejecta