On the Contribution of Very Massive Stars to the Sulfur Abundance in Star-Forming Galaxies: the Role of PISN
arXiv:2402.13240 · doi:10.1051/0004-6361/202348231
Abstract
Recent work presented increasing evidence of high, non-constant S/O abundance ratios observed in star-forming metal-poor galaxies, showing deviations from the constant canonical S/O across a large range of O/H abundance. Similar peculiar high Fe/O ratios have been also recently detected. We investigate whether these high S/O ratios at low metallicities could be explained taking into consideration the process of Pair Instability Supernovae (PISN) in chemical modelling through which similar behaviour observed for Fe/O ratios was successfully reproduced. We use chemical evolution models which take into account the stages of PISN in the yields published by Goswami et al. 2022, and adopt a suitable initial mass function (IMF) to characterize this evolutionary stage .appropriately. The peculiar high values and the behaviour of the observed S/O versus O/H relation can be reproduced when the ejecta of very massive stars that go through the process of PISN are taken into account. Additionally, a bi-modal top-heavy IMF and an initial strong burst of star formation are required to attain the reported high S/O values. We show that the role of very massive stars going through the process of PISN should be taken into account when explaining the chemical enrichment of sulfur and oxygen in metal-poor star-forming regions.
8 pages, 3 figures, accepted for publication in A&A
References in corpus (26)
- Pre-Supernova Evolution of Massive Single and Binary Stars
- The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 Msun stellar mass limit
- Fragmentation of star-forming clouds enriched with the first dust
- An excess of massive stars in the local 30 Doradus starburst
- The Birth of a Galaxy. II. The Role of Radiation Pressure
- Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up and C(, )O rate on the pair-instability black hole mass gap
- CHAOS IV: Gas-Phase Abundance Trends From The First Four CHAOS Galaxies
- The AMBRE Project: chemical evolution models for the Milky Way thick and thin discs
- Life and times of dwarf spheroidal galaxies
- Modelling the spectral energy distribution of ULIRGs II: The energetic environment and the dense interstellar medium
- APOGEE DR16: a multi-zone chemical evolution model for the Galactic disc based on MCMC methods
- The Galactic radial abundance gradients of C, N, O, Ne, S, Cl and Ar from deep spectra of H II regions
- Carbon star formation as seen through the non-monotonic initial-final mass relation
- CHAOS VI: Direct Abundances in NGC 2403
- Evaluating and Improving Semi-analytic modelling of Dust in Galaxies based on Radiative Transfer Calculations
- Explosion and nucleosynthesis of low redshift pair instability supernovae
- A Bayesian direct method implementation to fit emission line spectra: Application to the primordial He abundance determination
- EMPRESS. IV. Extremely Metal-Poor Galaxies (EMPGs) Including Very Low-Mass Primordial Systems with M*=10^4--10^5 M_sun and 2--3% (O/H)_sun: High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability Supernovae
- Modelling the chemical evolution of Zr, La, Ce and Eu in the Galactic discs and bulge
- The impact of very massive stars on the chemical evolution of extremely metal-poor galaxies
- On the effects of the Initial Mass Function on Galactic chemical enrichment
- On the use of Sulphur as a tracer for abundances in galaxies
- Potential signature of Population III pair-instability supernova ejecta in the BLR gas of the most distant quasar at z = 7.54
- Combining Physical galaxy models with radio observations to constrain the SFRs of high-z dusty star forming galaxies
- Trading oxygen for iron I: the [O/Fe] -- specific star formation rate relation of galaxies
- Chemical abundances in Seyfert galaxies X. Sulphur abundance estimates