# University of Hertfordshire

## He abundances in disc galaxies. I. Predictions from cosmological chemodynamical simulations

Research output: Contribution to journalArticle

### Documents

• 1905.08309

Accepted author manuscript, 3 MB, PDF document

• aa35886-19

Final published version, 2 MB, PDF document

• Fiorenzo Vincenzo
• Andrea Miglio
• Chiaki Kobayashi
• J. Ted Mackereth
• Josefina Montalban
Original language English Astronomy & Astrophysics 2 Aug 2019 2 Aug 2019 https://doi.org/10.1051/0004-6361/201935886 E-pub ahead of print - 2 Aug 2019

### Abstract

We investigate how the stellar and gas-phase He abundances evolve as functions of time within simulated star-forming disc galaxies with different star formation histories. We make use of a cosmological chemodynamical simulation for galaxy formation and evolution, which includes star formation, as well as energy and chemical enrichment feedback from asymptotic giant branch stars, core-collapse supernovae, and Type Ia supernovae. The predicted relations between the He mass fraction, $Y$, and the metallicity, $Z$, in the interstellar medium of our simulated disc galaxies depend on the past galaxy star formation history. In particular, $dY/dZ$ is not constant and evolves as a function of time, depending on the specific chemical element that we choose to trace $Z$; in particular, $dY/dX_{\text{O}}$ and $dY/dX_{\text{C}}$ increase as functions of time, whereas $dY/dX_{\text{N}}$ decreases. In the gas-phase, we find negative radial gradients of $Y$, due to the inside-out growth of our simulated galaxy discs as a function of time; this gives rise to longer chemical enrichment time scales in the outer galaxy regions, where we find lower average values for $Y$ and $Z$. Finally, by means of chemical evolution models, in the galactic bulge and inner disc, we predict steeper $Y$ versus age relations at high $Z$ than in the outer galaxy regions. We conclude that, for calibrating the assumed $Y$-$Z$ relation in stellar models, C, N, and C+N are better proxies for the metallicity than O, because they show steeper and less scattered relations.

### Notes

Accepted for publication in A&A

ID: 17171978