2021MNRAS.502.4457G

We explore how the star formation and metal enrichment histories of present-day galaxies have been affected by environment combining stellar population parameter estimates and group environment characterization for SDSS DR7. We compare stellar ages, stellar metallicities, and crucially, element abundance ratios [α/Fe] of satellite and central galaxies, as a function of their stellar and host group halo mass, controlling for the current star formation rate and for the infall epoch. We confirm that below M_* ∼ 10^10.5 M_☉ satellites are older and slightly metal richer than equally massive central galaxies. In contrast, we do not detect any difference in their [α/Fe]: [α/Fe] depends primarily on stellar mass and not on group hierarchy nor host halo mass. We also find that the differences in the median age and metallicity of satellites and centrals at stellar mass below 10^10.5M_☉ are largely due to the higher fraction of passive galaxies among satellites and as a function of halo mass. We argue that the observed trends at low masses reveal the action of satellite-specific environmental effects in a 'delayed-then-rapid' fashion. When accounting for the varying quiescent fraction, small residual excess in age, metallicity and [α/Fe] emerge for satellites dominated by old stellar populations and residing in haloes more massive than 10¹⁴ M_☉, compared to equally massive central galaxies. This excess in age, metallicity, and [α/Fe] pertain to ancient infallers, i.e. satellites that have accreted on to the current halo more than 5 Gyr ago. This result points to the action of environment in the early phases of star formation in galaxies located close to cosmic density peaks.