Observational constraints on the origin of the elements. V. Constraints on the chemical enrichment by sub-Chandrasekhar mass SNe in the Milky Way. (arXiv:2206.10258v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Eitner_P/0/1/0/all/0/1">P. Eitner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergemann_M/0/1/0/all/0/1">M. Bergemann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruiter_A/0/1/0/all/0/1">A. J. Ruiter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seitenzahl_I/0/1/0/all/0/1">I. R. Seitenzahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gent_M/0/1/0/all/0/1">M. R. Gent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cote_B/0/1/0/all/0/1">B. Côté</a>
Aims. We constrain the role of different Type Ia supernovae (SN Ia)
sub-classes in the chemical enrichment of the Galaxy by studying the abundances
of iron and manganese in Galactic stars. We investigate four different SN Ia
sub-classes, including the classical single-degenerate near-Chandrasekhar mass
(Mch) SN Ia, the fainter SN Iax systems associated with He accretion from the
companion, as well as two sub-Chandrasekhar mass (sub-Mch) SN Ia models. The
latter include the double-detonation of a white dwarf accreting helium-rich
matter and violent white dwarf mergers. Methods. The chemical abundances in
Galactic stars are determined using Gaia eDR3 astrometry and photometry, and
the publicly released spectra obtained within the Gaia-ESO large spectroscopic
survey. Non-local thermodynamic equilibrium (NLTE) models are used in the
spectroscopic analysis. The GCE models have been updated to include detailed
delay time distributions arising from binary population synthesis simulations
and the different SN Ia channels, as well as recent yields for core-collapse
supernovae and AGB stars. The data-model comparison is performed using a Markov
chain Monte Carlo framework that allows us to explore the entire parameter
space allowed by the diversity of explosion mechanisms and the Galactic SN Ia
rate, taking into account the uncertainties of the observed data. Results.
Comparison of the new data with GCE models suggests that the observations can
only be explained if the fraction of sub-Mch SNe in the models varies between
50 % and 73 %. The standard Mch SNe are not the dominant channel, but are still
needed to account for the elevated [Mn/Fe] ratio in the thin disc. Our results
only weakly depend on the assumptions on AGB and core collapse SN yields,
providing a strong evidence that sub-Mch SNe play a major role in the chemical
evolution of our Galaxy.
Aims. We constrain the role of different Type Ia supernovae (SN Ia)
sub-classes in the chemical enrichment of the Galaxy by studying the abundances
of iron and manganese in Galactic stars. We investigate four different SN Ia
sub-classes, including the classical single-degenerate near-Chandrasekhar mass
(Mch) SN Ia, the fainter SN Iax systems associated with He accretion from the
companion, as well as two sub-Chandrasekhar mass (sub-Mch) SN Ia models. The
latter include the double-detonation of a white dwarf accreting helium-rich
matter and violent white dwarf mergers. Methods. The chemical abundances in
Galactic stars are determined using Gaia eDR3 astrometry and photometry, and
the publicly released spectra obtained within the Gaia-ESO large spectroscopic
survey. Non-local thermodynamic equilibrium (NLTE) models are used in the
spectroscopic analysis. The GCE models have been updated to include detailed
delay time distributions arising from binary population synthesis simulations
and the different SN Ia channels, as well as recent yields for core-collapse
supernovae and AGB stars. The data-model comparison is performed using a Markov
chain Monte Carlo framework that allows us to explore the entire parameter
space allowed by the diversity of explosion mechanisms and the Galactic SN Ia
rate, taking into account the uncertainties of the observed data. Results.
Comparison of the new data with GCE models suggests that the observations can
only be explained if the fraction of sub-Mch SNe in the models varies between
50 % and 73 %. The standard Mch SNe are not the dominant channel, but are still
needed to account for the elevated [Mn/Fe] ratio in the thin disc. Our results
only weakly depend on the assumptions on AGB and core collapse SN yields,
providing a strong evidence that sub-Mch SNe play a major role in the chemical
evolution of our Galaxy.
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