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The Gaia-ESO Survey: the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters
Univ Sao Paulo, Dept Astron, Rua Matao 1226, BR-05509900 Sao Paulo, SP, Brazil..
Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy..
Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy..
Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England..
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2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 601, article id A70Article in journal (Refereed) Published
Abstract [en]

Context. The radial metallicity distribution in the Galactic thin disc represents a crucial constraint for modelling disc formation and evolution. Open star clusters allow us to derive both the radial metallicity distribution and its evolution over time. Aims. In this paper we perform the first investigation of the present-day radial metallicity distribution based on [Fe/H] determinations in late type members of pre-main-sequence clusters. Because of their youth, these clusters are therefore essential for tracing the current interstellar medium metallicity. Methods. We used the products of the Gaia-ESO Survey analysis of 12 young regions (age < 100 Myr), covering Galactocentric distances from 6.67 to 8.70 kpc. For the first time, we derived the metal content of star forming regions farther than 500 pc from the Sun. Median metallicities were determined through samples of reliable cluster members. For ten clusters the membership analysis is discussed in the present paper, while for other two clusters (i.e. Chamaeleon I and Gamma Velorum) we adopted the members identified in our previous works. Results. All the pre-main-sequence clusters considered in this paper have close-to-solar or slightly sub-solar metallicities. The radial metallicity distribution traced by these clusters is almost flat, with the innermost star forming regions having [Fe/H] values that are 0.10-0.15 dex lower than the majority of the older clusters located at similar Galactocentric radii. Conclusions. This homogeneous study of the present-day radial metallicity distribution in the Galactic thin disc favours models that predict a flattening of the radial gradient over time. On the other hand, the decrease of the average [Fe/H] at young ages is not easily explained by the models. Our results reveal a complex interplay of several processes (e.g. star formation activity, initial mass function, supernova yields, gas flows) that controlled the recent evolution of the Milky Way.

Place, publisher, year, edition, pages
EDP Sciences, 2017. Vol. 601, article id A70
Keywords [en]
stars: abundances, stars: pre-main sequence, Galaxy: abundances, Galaxy: disk, Galaxy: evolution, open clusters and associations: general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-327049DOI: 10.1051/0004-6361/201630078ISI: 000402313500070OAI: oai:DiVA.org:uu-327049DiVA, id: diva2:1129462
Available from: 2017-08-03 Created: 2017-08-03 Last updated: 2017-08-03Bibliographically approved

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Korn, A. J.

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