Galactic Archaeology at High Redshift: Inferring the Nature of GRB Host Galaxies from Abundances

Palla, Marco; Matteuccí, F.; Calura, F.; Longo, F.

doi:10.3847/1538-4357/ab6080

Cited by 11 publications

(21 citation statements)

References 101 publications

(215 reference statements)

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“…where the disc scale length R d is 3.5 kpc for the low-α disc (e.g. Spitoni et al 2017) and 2.3 kpc for the high-α disc (Pouliasis et al 2017, see also Palla et al 2020a). This leads to a Σ low /Σ high increasing with radius in agreement with recent observational and theoretical works (e.g.…”

Section: Chemical Evolution Modelssupporting

confidence: 89%

“…This parameter is set to 2 Gyr −1 for the first infall/high-α star formation episode and to 1 Gyr −1 for the second infall/low-α episode. R i (R, t) (see Palla et al 2020a for the complete expression) takes into account the nucleosynthesis from low-intermediate mass stars (LIMS, m < 8 M ), core collapse (CC) SNe (Type II and Ib/c, m > 8 M ) and Type Ia SNe (SN Ia). For these latter, we assume the single-degenerate (SD) scenario and in particular the delay-time-distribution (DTD) by Matteucci & Recchi (2001).…”

Section: Chemical Evolution Modelsmentioning

confidence: 99%

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[Mg/Fe] ratios in the solar neighbourhood: stellar yields and chemical evolution scenarios

Palla,

Santos-Peral,

Recio-Blanco

et al. 2022

Preprint

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Context. The [Mg/Fe] abundance ratios are a fundamental fossil signature to trace the chemical evolution of the disc and dissecting it into low-α and high-α populations. Despite of the huge observational and theoretical effort, discrepancies between models and data are still present and several explanations have been put forward to explain the [α/Fe] bimodality. Aims. In this work, we take advantage of a new AMBRE:HARPS dataset, which provides new and more precise [Mg/Fe] estimations, as well as reliable stellar ages for a subsample of stars, to study the [α/Fe] bimodality and the evolution of the solar neighbourhood. Methods. The above data are compared with detailed chemical evolution models for the Milky Way, exploring the most used prescriptions for stellar yields as well as different formation scenarios for the Galactic disc, i.e. the delayed two-infall and the parallel model, also including prescriptions for stellar radial migration. Results. We see that most of the stellar yield prescriptions struggle to reproduce the observed trend of the data and that semi-empirical yields are still the best to describe the [Mg/Fe] evolution in the thick and thin discs. In particular, most of the yields still predict a steeper decrease of the [Mg/Fe] ratio at high metallicity than what is shown by the data.The bulk of the data are well reproduced by the parallel and two-infall scenarios, but both scenarios have problems in explaining the most metal-rich and metal-poor tails of the low-α data. These tails can be explained in light of radial migration from inner and outer disc regions, respectively. Conclusions. Despite of the evidence of stellar migration, it is difficult to estimate the actual contribution of stars from other parts of the disc to the solar vicinity in the data we adopt. However, the comparison between data and models suggests that peculiar histories of star formation, such as that of the two-infall model, are still needed to reproduce the observed distribution of stars.

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Section: Chemical Evolution Modelssupporting

confidence: 89%

Section: Chemical Evolution Modelsmentioning

confidence: 99%

[Mg/Fe] ratios in the solar neighbourhood: stellar yields and chemical evolution scenarios

Palla,

Santos-Peral,

Recio-Blanco

et al. 2022

Preprint

Self Cite

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“…where gas is the surface gas density, k = 1.5 is the law index, and ν is the SFE. R i (R, t) (see Palla et al 2020 for the complete expression) takes into account the nucleosynthesis from low-intermediate mass stars (LIMS, m < 8M ), core collapse (CC) SNe (Type II and Ib/c, m > 8M ), and Type Ia SNe. For these latter, we assume the single-degenerate (SD) scenario, in which a C-O white dwarf in a binary system accretes mass from a non-degenerate companion until it reaches nearly the Chandrasekhar mass (∼1.44M ).…”

Section: Milky Way Two-infall Modelsmentioning

confidence: 99%

Chemical evolution of the Milky Way: constraints on the formation of the thick and thin discs

Palla

Matteuccí

Spitoni

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the evolution of Milky Way thick and thin discs in the light of the most recent observational data. In particular, we analyze abundance gradients of O, N, Fe and Mg along the thin disc as well as the [Mg/Fe] vs. [Fe/H] relations and the metallicity distribution functions at different Galactocentric distances. We run several models starting from the two-infall paradigm, assuming that the thick and thin discs formed by means of two different infall episodes, and we explore several physical parameters, such as radial gas flows, variable efficiency of star formation, different times for the maximum infall onto the disc, different distributions of the total surface mass density of the thick disc and enriched gas infall. Our best model suggests that radial gas flows and variable efficiency of star formation should be acting together with the inside-out mechanism for the thin disc formation. The timescale for maximum infall onto the thin disc, which determines the gap between the formation of the two discs, should be tmax ≃ 3.25 Gyr. The thick disc should have an exponential, small scale length density profile and gas infall on the inner thin disc should be enriched. We compute also the evolution of Gaia-Enceladus system and study the effects of possible interactions with the thick and thin discs. We conclude that the gas lost by Enceladus or even part of it could have been responsible for the formation of the thick disc but not the thin disc.

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“…where Σ gas is the surface gas density, k = 1.5 is the law index and ν is the star formation efficiency. R i (R, t) (see Palla et al 2020 for the complete expression) takes into account the nucleosynthesis from lowintermediate mass stars (LIMS, m < 8M ), core collapse (CC) SNe (Type II and Ib/c, m > 8M ) and Type Ia SNe. For these latter, we assume the single-degenerate (SD) scenario, in which a C-O white dwarf in a binary system accretes mass from a non-degenerate companion until it reaches nearly the Chandrasekhar mass (∼ 1.44M ).…”

Section: Milky Way Two-infall Modelsmentioning

confidence: 99%

Chemical evolution of the Milky Way: constraints on the formation of the thick and thin discs

Palla,

Matteucci,

Spitoni

et al. 2020

Preprint

Self Cite

View full text Add to dashboard Cite

We study the evolution of Milky Way thick and thin discs in the light of the most recent observational data. In particular, we analyze abundance gradients of O, N, Fe and Mg along the thin disc as well as the [Mg/Fe] vs. [Fe/H] relations and the metallicity distribution functions at different Galactocentric distances. We run several models starting from the two-infall paradigm, assuming that the thick and thin discs formed by means of two different infall episodes, and we explore several physical parameters, such as radial gas flows, variable efficiency of star formation, different times for the maximum infall onto the disc, different distributions of the total surface mass density of the thick disc and enriched gas infall. Our best model suggests that radial gas flows and variable efficiency of star formation should be acting together with the inside-out mechanism for the thin disc formation. The timescale for maximum infall onto the thin disc, which determines the gap between the formation of the two discs, should be t max 3.25 Gyr. The thick disc should have an exponential, small scale length density profile and gas infall on the inner thin disc should be enriched. We compute also the evolution of Gaia-Enceladus system and study the effects of possible interactions with the thick and thin discs. We conclude that the gas lost by Enceladus or even part of it could have been responsible for the formation of the thick disc but not the thin disc.

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Galactic Archaeology at High Redshift: Inferring the Nature of GRB Host Galaxies from Abundances

Cited by 11 publications

References 101 publications

[Mg/Fe] ratios in the solar neighbourhood: stellar yields and chemical evolution scenarios

[Mg/Fe] ratios in the solar neighbourhood: stellar yields and chemical evolution scenarios

Chemical evolution of the Milky Way: constraints on the formation of the thick and thin discs

Chemical evolution of the Milky Way: constraints on the formation of the thick and thin discs

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