Modelling the chemical evolution of the Milky Way

Matteuccí, F.

doi:10.1007/s00159-021-00133-8

Cited by 108 publications

(45 citation statements)

References 338 publications

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“…Although detailed interpretation of the variation of scatter for different elements is complicated by the uncertainties in theoretical yields (see, e.g. Matteucci 2021, for a recent review) and other modelling aspects (see, e.g., Buck et al 2021) and is beyond the scope of this study, the increase of scatter at low metallicites is generally consistent with the interpretation that low-metallicity stars have formed during the fast gas accretion regime of the Milky Way formation.…”

Section: Transition Between Star Formation Regimes and Evolution Of S...supporting

confidence: 75%

From dawn till disk: Milky Way's turbulent youth revealed by the APOGEE+Gaia data

Belokurov,

Kravtsov

2022

Preprint

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We use accurate estimates of aluminium abundance provided as part of the APOGEE Data Release 17 and Gaia Early Data Release 3 astrometry to select a highly pure sample of stars with metallicity −1.5[Fe/H] 0.5 born in-situ in the Milky Way proper. We show that the low-metallicity ([Fe/H] −1.3) in-situ component that we dub Aurora is kinematically hot with an approximately isotropic velocity ellipsoid and a modest net rotation. Aurora stars exhibit large scatter in metallicity and in a number of element abundance ratios. The median tangential velocity of the in-situ stars increases sharply with increasing metallicity between [Fe/H]= −1.3 and −0.9, the transition that we call the spin-up. The observed and theoretically expected age-metallicity correlations imply that this increase reflects a rapid formation of the Milky Way disk over ≈ 1 − 2 Gyrs. The transformation of the stellar kinematics as a function of [Fe/H] is accompanied by a qualitative change in chemical abundances: the scatter drops sharply once the Galaxy builds up a disk during later epochs corresponding to [Fe/H]> −0.9. Results of galaxy formation models presented in this and other recent studies strongly indicate that the trends observed in the Milky Way reflect generic processes during the early evolution of progenitors of MW-sized galaxies: a period of chaotic pre-disk evolution, when gas is accreted along cold narrow filaments and when stars are born in irregular configurations, and subsequent rapid disk formation. The latter signals formation of a stable hot gaseous halo around the MW progenitor, which changes the mode of gas accretion and allows development of coherently rotating disk.

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Section: Transition Between Star Formation Regimes and Evolution Of S...supporting

confidence: 75%

From dawn till disk: Milky Way's turbulent youth revealed by the APOGEE+Gaia data

Belokurov,

Kravtsov

2022

Preprint

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“…Such differences will for example influence at which [Fe/H] we see the typical knee in the [α/Fe] versus [Fe/H] plane, at which SNIa kick in (e.g. Tinsley 1979;Gilmore & Wyse 1991;McWilliam 1997;Matteucci 2021). The chrono-chemodynamic data of GALAH+ DR3 is so rich that we cannot address all questions here.…”

Section: Prospects For Chemically Tagging the Accreted Halomentioning

confidence: 97%

The GALAH Survey: chemical tagging and chrono-chemodynamics of accreted halo stars with GALAH+ DR3 andGaiaeDR3

Buder

Lind

Ness

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Since the advent of Gaia astrometry, it is possible to identify massive accreted systems within the Galaxy through their unique dynamical signatures. One such system, Gaia-Sausage-Enceladus (GSE), appears to be an early “building block” given its virial mass >1010 M⊙ at infall (z ∼ 1 − 3). In order to separate the progenitor population from the background stars, we investigate its chemical properties with up to 30 element abundances from the GALAH+ Survey Data Release 3 (DR3). To inform our choice of elements for purely chemically selecting accreted stars, we analyse 4164 stars with low-α abundances and halo kinematics. These are most different to the Milky Way stars for abundances of Mg, Si, Na, Al, Mn, Fe, Ni, and Cu. Based on the significance of abundance differences and detection rates, we apply Gaussian mixture models to various element abundance combinations. We find the most populated and least contaminated component, which we confirm to represent GSE, contains 1049 stars selected via [Na/Fe] vs. [Mg/Mn] in GALAH+ DR3. We provide tables of our selections and report the chrono-chemodynamical properties (age, chemistry, and dynamics). Through a previously reported clean dynamical selection of GSE stars, including $30 < \sqrt{J_R / \, \mathrm{kpc\, km\, s^{-1}}} < 55$, we can characterise an unprecedented 24 abundances of this structure with GALAH+ DR3. With our chemical selection we characterise the dynamical properties of the GSE, for example mean $\sqrt{J_R / \, \mathrm{kpc\, km\, s^{-1}}} = 26^{+9}_ {-14}$. We find only $(29\pm 1)\%$ of the GSE stars within the clean dynamical selection region. Our methodology will improve future studies of accreted structures and their importance for the formation of the Milky Way.

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“…However, radial flows and stellar migration also have a role in modifying the observed gradients, for instance stellar migration might act in flattening the stellar metallicity gradients e.g., [9,19]. For a general review, we refer to Matteucci [23].…”

Section: Introductionmentioning

confidence: 99%

Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges

2022

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In this paper, we make use of data collected for open cluster members by high-resolution spectroscopic surveys and programmes (i.e., APOGEE, Gaia-ESO, GALAH, OCCASO, and SPA). These data have been homogenised and then analysed as a whole. The resulting catalogue contains [Fe/H] and orbital parameters for 251 Galactic open clusters. The slope of the radial metallicity gradient obtained through 175 open clusters with high-quality metallicity determinations is −0.064 ± 0.007 dex kpc−1. The radial metallicity distribution traced by open clusters flattens beyond RGal = 12.1 ± 1.1 kpc. The slope traced by open clusters in the [Fe/H]-Lz diagram is −0.31 ± 0.02 × 103 dex km−1 kpc−1 s, but it flattens beyond Lz = 2769 ± 177 km kpc s−1. In this paper, we also review some high-priority practical challenges around the study of open clusters that will significantly push our understanding beyond the state-of-the-art. Finally, we compare the shape of the galactic radial metallicity gradient to those of other spiral galaxies.

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Modelling the chemical evolution of the Milky Way

Cited by 108 publications

References 338 publications

From dawn till disk: Milky Way's turbulent youth revealed by the APOGEE+Gaia data

From dawn till disk: Milky Way's turbulent youth revealed by the APOGEE+Gaia data

The GALAH Survey: chemical tagging and chrono-chemodynamics of accreted halo stars with GALAH+ DR3 andGaiaeDR3

Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges

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