Статья

The <i>Gaia</i>-ESO survey: Mapping the shape and evolution of the radial abundance gradients with open clusters

L. MagriniINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyC. Viscasillas VázquezInstitute of Theoretical Physics and Astronomy, Vilnius University, Sauletekio av. 3, 10257 Vilnius, LithuaniaL. SpinaINAF – Padova Observatory, Vicolo dell’Osservatorio 5, 35122 Padova, ItalyS. RandichINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyD. RomanoINAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, ItalyE. FranciosiniINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyA. Recio-BlancoUniversité Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice, FranceThomas NordlanderARC Centre of Excellence for Astronomy in Three Dimensions (ASTRO-3D), Canberra, ACT 2611, AustraliaV. D’OraziDipartimento di Fisica, Università degli Studi di Roma Tor Vergata, Via della Ricerca scientifica 1, 00133 Roma, ItalyM. BaratellaLeibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, GermanyR. SmiljanićNicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, PolandM. L. L. DantasNicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, PolandL. PasquiniE. SpitoniUniversité Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice, FranceG. CasaliDipartimento di Fisica e Astronomia, Università degli studi di Bologna, Via Gobetti 93/2, 40129 Bologna, ItalyM. Van der SwaelmenINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyT. BensbyLund Observatory, Department of Astronomy and Theoretical Physics, Box 43, 221 00 Lund, SwedenE. StonkutėInstitute of Theoretical Physics and Astronomy, Vilnius University, Sauletekio av. 3, 10257 Vilnius, LithuaniaS. FeltzingLund Observatory, Department of Astronomy and Theoretical Physics, Box 43, 221 00 Lund, SwedenG. G. SaccoINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyA. BragagliaINAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, ItalyE. PancinoINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyU. HeiterObservational Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, SwedenK. BiazzoINAF – Rome Observatory, Via Frascati, 33, Monte Porzio Catone, (RM), ItalyG. GilmoreInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKM. BergemannMax Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, GermanyG. TautvaiśienėInstitute of Theoretical Physics and Astronomy, Vilnius University, Sauletekio av. 3, 10257 Vilnius, LithuaniaC. C. WorleyInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKA. HourihaneInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKA. GonneauInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKL. MorbidelliINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy

2022en

ABI

Аннотация

Context. The spatial distribution of elemental abundances and their time evolution are among the major constraints to disentangling the scenarios of formation and evolution of the Galaxy. Aims. In this paper we used the sample of open clusters available in the final release of the Gaia -ESO survey to trace the Galactic radial abundance and abundance-to-iron ratio gradients, and their time evolution. Methods. We selected member stars in 62 open clusters, with ages from 0.1 to about 7 Gyr, located in the Galactic thin disc at galactocentric radii ( R GC ) from about 6 to 21 kpc. We analysed the shape of the resulting [Fe/H] gradient, the average gradients [El/H] and [El/Fe] combining elements belonging to four different nucleosynthesis channels, and their individual abundance and abundance ratio gradients. We also investigated the time evolution of the gradients dividing open clusters in three age bins. Results. The [Fe/H] gradient has a slope of −0.054 dex kpc −1 . It can be better approximated with a two-slope shape, steeper for R GC ≤ 11.2 kpc and flatter in the outer regions. We saw different behaviours for elements belonging to different channels. For the time evolution of the gradient, we found that the youngest clusters (age < 1 Gyr) in the inner disc have lower metallicity than their older counterparts and that they outline a flatter gradient. We considered some possible explanations, including the effects of gas inflow and migration. We suggest that the most likely one may be related to a bias introduced by the standard spectroscopic analysis producing lower metallicities in the analysis of low-gravity stars. Conclusions. To delineate the shape of the ‘true’ gradient, we should most likely limit our analysis to stars with low surface gravity log g > 2.5 and microturbulent parameter ξ < 1.8 km s −1 . Based on this reduced sample, we can conclude that the gradient has minimally evolved over the time-frame outlined by the open clusters, indicating a slow and stationary formation of the thin disc over the last 3 Gyr. We found a secondary role of cluster migration in shaping the gradient, with a more prominent role of migration for the oldest clusters.

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Идентификаторы

DOI: 10.1051/0004-6361/202244957

Цитирования и источники

Цитирований: 2Использованных источников: 0

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