On the [α/Fe]-[Fe/H] relations in early-type galaxies

Fiorenzo Vincenzo, Chiaki Kobayashi, Philip Taylor

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We study how the predicted [α/Fe]-[Fe/H] relations in early-type galaxies vary as functions of their stellar masses, ages, and stellar velocity dispersions, by making use of cosmological chemodynamical simulations with feedback from active galactic nuclei. Our model includes a detailed treatment for the chemical enrichment from dying stars, core-collapse supernovae (both Type II and hypernovae) and Type Ia supernovae. At redshift z = 0, we create a catalogue of 526 galaxies, among which we determine 80 early-type galaxies. From the analysis of our simulations, we find [α/Fe]-[Fe/H] relations similar to the Galactic bulge. We also find that, in the oldest galaxies, Type Ia supernovae start to contribute at higher [Fe/H] than in the youngest ones. On the average, early-type galaxies with larger stellar masses (and, equivalently, higher stellar velocity dispersions) have higher [α/Fe] ratios, at fixed [Fe/H]. This is qualitatively consistent with the recent observations of Sybilska et al., but quantitatively there are mismatches, which might require stronger feedback, sub-classes of Type Ia Supernovae, or a variable initial mass function to address.

Original languageEnglish
Pages (from-to)L38–L42
JournalMonthly Notices of the Royal Astronomical Society: Letters
Issue number1
Early online date12 Jul 2018
Publication statusPublished - 1 Oct 2018


  • CD- galaxies: evolution
  • Galaxies: abundances
  • Galaxies: elliptical and lenticular
  • Hydrodynamics
  • Stars: abundances
  • Supernovae: general


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