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

L. Magrini; C. Viscasillas Vazquez; L. Spina; S. Randich; D. Romano; E. Franciosini; A. Recio-Blanco; T. Nordlander; V. D'Orazi; M. Baratella; R. Smiljanic; M. L. L. Dantas; L. Pasquini; E. Spitoni; G. Casali; M. Van der Swaelmen; T. Bensby; E. Stonkute; S. Feltzing; G. G. Sacco; A. Bragaglia; E. Pancino; U. Heiter; K. Biazzo; G. Gilmore; M. Bergemann; G. Tautvaisiene; C. Worley; A. Hourihane; A. Gonneau; L. Morbidelli

doi:10.1051/0004-6361/202244957

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

L. Magrini^*
, C. Viscasillas Vazquez
, L. Spina
, S. Randich
, D. Romano
, E. Franciosini
, A. Recio-Blanco
, T. Nordlander
, V. D'Orazi
, M. Baratella
, R. Smiljanic
, M. L. L. Dantas
, L. Pasquini
, E. Spitoni
, G. Casali
, M. Van der Swaelmen
, T. Bensby
, E. Stonkute
, S. Feltzing
, G. G. Sacco

A. Bragaglia, E. Pancino, U. Heiter, K. Biazzo, G. Gilmore, M. Bergemann, G. Tautvaisiene, C. Worley, A. Hourihane, A. Gonneau, L. Morbidelli

^*Corresponding author af dette arbejde

Niels Bohr Internationale Akademi

Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › peer review

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Abstract

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

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 xi< 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.

Originalsprog	Engelsk
Artikelnummer	A119
Tidsskrift	Astronomy & Astrophysics
Vol/bind	669
Antal sider	25
ISSN	0004-6361
DOI	https://doi.org/10.1051/0004-6361/202244957
Status	Udgivet - 20 jan. 2023

Finansiering

We would like to thank the referee for her/his careful readingand useful suggestions. Based on data products from observations made withESO Telescopes at the La Silla Paranal Observatory under programmes 188.B-3002, 193.B-0936, and 197.B-1074. These data products have been processedby the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astron-omy, University of Cambridge, and by the FLAMES/UVES reduction teamat INAF/Osservatorio Astrofisico di Arcetri. These data have been obtainedfrom theGaia-ESO Survey Data Archive, prepared and hosted by the WideField Astronomy Unit, Institute for Astronomy, University of Edinburgh, whichis funded by the UK Science and Technology Facilities Council. This workwas partly supported by the European Union FP7 programme through ERCgrant number 320360 and by the Leverhulme Trust through grant RPG-2012-541.We acknowledge the support from INAF and Ministero dell'Istruzione,dell'Universita e della Ricerca (MIUR) in the form of the grant "PremialeVLT 2012". The results presented here benefit from discussions held duringtheGaia-ESO workshops and conferences supported by the ESF (EuropeanScience Foundation) through the GREAT Research Network Programme. LM,SR, EF, GC, MVdS, GGS, AB acknowledges partial support from Premiale2016 MITiC. MLLD and RS acknowledge support by the National ScienceCentre, Poland, project 2019/34/E/ST9/00133. MB is supported through theLise Meitner grant from the Max Planck Society. We acknowledge supportby the Collaborative Research centre SFB 881 (projects A5, A10), HeidelbergUniversity, of the Deutsche Forschungsgemeinschaft (DFG, German ResearchFoundation). This project has received funding from the European ResearchCouncil (ERC) under the European Union's Horizon 2020 research and inno-vation programme (Grant agreement No. 949173). TB was supported by grantNo. 2018-04857 from the Swedish Research Council. UH acknowledges supportfrom the Swedish National Space Agency (SNSA/Rymdstyrelsen). GC acknowl-edges support from the European Research Council Consolidator Grant fundingscheme (project ASTEROCHRONOMETRY, G.A. n. 772293,http://www.asterochronometry.eu). CVV acknowledges support from "Direzione Gen-erale per la diplomazia pubblica e culturale" of the "Ministero degli Affari Esterie della Cooperazione Internazionale" and the "Istituto Italiano di Cultura inVilnius

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Magrini, L., Vazquez, C. V., Spina, L., Randich, S., Romano, D., Franciosini, E., Recio-Blanco, A., Nordlander, T., D'Orazi, V., Baratella, M., Smiljanic, R., Dantas, M. L. L., Pasquini, L., Spitoni, E., Casali, G., Van der Swaelmen, M., Bensby, T., Stonkute, E., Feltzing, S., ... Morbidelli, L. (2023). The Gaia-ESO survey: Mapping the shape and evolution of the radial abundance gradients with open clusters. Astronomy & Astrophysics, 669, Artikel A119. https://doi.org/10.1051/0004-6361/202244957

Magrini, L, Vazquez, CV, Spina, L, Randich, S, Romano, D, Franciosini, E, Recio-Blanco, A, Nordlander, T, D'Orazi, V, Baratella, M, Smiljanic, R, Dantas, MLL, Pasquini, L, Spitoni, E, Casali, G, Van der Swaelmen, M, Bensby, T, Stonkute, E, Feltzing, S, Sacco, GG, Bragaglia, A, Pancino, E, Heiter, U, Biazzo, K, Gilmore, G, Bergemann, M, Tautvaisiene, G, Worley, C, Hourihane, A, Gonneau, A & Morbidelli, L 2023, 'The Gaia-ESO survey: Mapping the shape and evolution of the radial abundance gradients with open clusters', Astronomy & Astrophysics, bind 669, A119. https://doi.org/10.1051/0004-6361/202244957

@article{7805decd04f649f99d54a2daa9cf8570,

title = "The Gaia-ESO survey: Mapping the shape and evolution of the radial abundance gradients with open clusters",

abstract = "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-GCConclusions. 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 xi< 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.",

keywords = "stars: abundances, stars: evolution, open clusters and associations: general, Galaxy: evolution, OLD OPEN CLUSTERS, GALACTIC METALLICITY GRADIENT, POPULATION ASTROPHYSICS SPA, YOUNG OPEN CLUSTERS, CHEMICAL EVOLUTION, ELEMENT ABUNDANCES, MILKY-WAY, ATMOSPHERIC PARAMETERS, PLANETARY-NEBULAE, IRON ABUNDANCES",

author = "L. Magrini and Vazquez, \{C. Viscasillas\} and L. Spina and S. Randich and D. Romano and E. Franciosini and A. Recio-Blanco and T. Nordlander and V. D'Orazi and M. Baratella and R. Smiljanic and Dantas, \{M. L. L.\} and L. Pasquini and E. Spitoni and G. Casali and \{Van der Swaelmen\}, M. and T. Bensby and E. Stonkute and S. Feltzing and Sacco, \{G. G.\} and A. Bragaglia and E. Pancino and U. Heiter and K. Biazzo and G. Gilmore and M. Bergemann and G. Tautvaisiene and C. Worley and A. Hourihane and A. Gonneau and L. Morbidelli",

year = "2023",

month = jan,

day = "20",

doi = "10.1051/0004-6361/202244957",

language = "English",

volume = "669",

journal = "Astronomy \& Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

TY - JOUR

T1 - The Gaia-ESO survey

T2 - Mapping the shape and evolution of the radial abundance gradients with open clusters

AU - Magrini, L.

AU - Vazquez, C. Viscasillas

AU - Spina, L.

AU - Randich, S.

AU - Romano, D.

AU - Franciosini, E.

AU - Recio-Blanco, A.

AU - Nordlander, T.

AU - D'Orazi, V.

AU - Baratella, M.

AU - Smiljanic, R.

AU - Dantas, M. L. L.

AU - Pasquini, L.

AU - Spitoni, E.

AU - Casali, G.

AU - Van der Swaelmen, M.

AU - Bensby, T.

AU - Stonkute, E.

AU - Feltzing, S.

AU - Sacco, G. G.

AU - Bragaglia, A.

AU - Pancino, E.

AU - Heiter, U.

AU - Biazzo, K.

AU - Gilmore, G.

AU - Bergemann, M.

AU - Tautvaisiene, G.

AU - Worley, C.

AU - Hourihane, A.

AU - Gonneau, A.

AU - Morbidelli, L.

PY - 2023/1/20

Y1 - 2023/1/20

N2 - 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-GCConclusions. 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 xi< 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.

AB - 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-GCConclusions. 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 xi< 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.

KW - stars: abundances

KW - stars: evolution

KW - open clusters and associations: general

KW - Galaxy: evolution

KW - OLD OPEN CLUSTERS

KW - GALACTIC METALLICITY GRADIENT

KW - POPULATION ASTROPHYSICS SPA

KW - YOUNG OPEN CLUSTERS

KW - CHEMICAL EVOLUTION

KW - ELEMENT ABUNDANCES

KW - MILKY-WAY

KW - ATMOSPHERIC PARAMETERS

KW - PLANETARY-NEBULAE

KW - IRON ABUNDANCES

U2 - 10.1051/0004-6361/202244957

DO - 10.1051/0004-6361/202244957

M3 - Journal article

SN - 0004-6361

VL - 669

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A119

ER -