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We investigate the differential effects of metal cooling and galactic stellarwinds on the cosmological formation of individual galaxies with three sets ofcosmological, hydrodynamical zoom simulations of 45 halos in the mass range10^11<M_halo<10^13M_sun. Models including both galactic winds and metal cooling(i) suppress early star formation at z>1 and predict reasonable star formationhistories, (ii) produce galaxies with high cold gas fractions (30-60 per cent)at high redshift, (iii) significantly reduce the galaxy formation efficienciesfor halos (M_halo<10^12M_sun) at all redshifts in agreement with observationaland abundance matching constraints, (iv) result in high-redshift galaxies withreduced circular velocities matching the observed Tully-Fisher relation at z~2,and (v) significantly increase the sizes of low-mass galaxies(M_stellar<3x10^10M_sun) at high redshift resulting in a weak size evolution -a trend in agreement with observations. However, the low redshift (z<0.5) starformation rates of massive galaxies are higher than observed (up to ten times).No tested model predicts the observed size evolution for low-mass and high-massgalaxies simultaneously. Due to the delayed onset of star formation in the windmodels, the metal enrichment of gas and stars is delayed and agrees well withobservational constraints. Metal cooling and stellar winds are both found toincrease the ratio of in situ formed to accreted stars - the relativeimportance of dissipative vs. dissipationless assembly. For halo masses below~10^12M_sun, this is mainly caused by less stellar accretion and compares wellto predictions from semi-analytical models but still differs from abundancematching models. For higher masses, the fraction of in situ stars isover-predicted due to the unrealistically high star formation rates at lowredshifts.

The effect of metal enrichment and galactic winds on galaxy formation in cosmological zoom simulations