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The metal enrichment of passive galaxies in cosmological simulations of galaxy formation

Massive early-type galaxies have higher metallicities and higher ratios of $α$ elements to iron than their less massive counterparts. Reproducing these correlations has long been a problem for hierarchical galaxy formation theory, both in semi-analytic models and cosmological hydrodynamic simulations. We show that a simulation in which gas cooling in massive dark haloes is quenched by radio-mode active galactic nuclei (AGNs) feedback naturally reproduces the observed trend between $α$/Fe and the velocity dispersion of galaxies, $σ$. The quenching occurs earlier for more massive galaxies. Consequently, these galaxies complete their star formation before $α$/Fe is diluted by the contribution from type Ia supernovae. For galaxies more massive than $\sim 10^{11}~M_\odot$ whose $α$/Fe correlates positively with stellar mass, we find an inversely correlated mass-metallicity relation. This is a common problem in simulations in which star formation in massive galaxies is quenched either by quasar- or radio-mode AGN feedback. The early suppression of gas cooling in progenitors of massive galaxies prevents them from recapturing enriched gas ejected as winds. Simultaneously reproducing the [$α$/Fe]-$σ$ relation and the mass-metallicity relation is, thus, difficult in the current framework of galaxy formation.