期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 505, 期 3, 页码 3165-3176出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab1559
关键词
techniques: spectroscopic; stars: abundances; binaries: spectroscopic; stars: low-mass; white dwarfs; solar neighbourhood
资金
- 2019 Leonardo Grant for Researchers and Cultural Creators, BBVA Foundation
- MINECO under the Ramon y Cajal program [RYC-2016-20254]
- Accordo Attuativo ASI-INAF [2018.22.HH.O]
- postdoctoral fellowship programme Beatriu de Pinos - AGAUR (Government of Catalonia)
- Horizon 2020 programme of research and innovation of the European Union under the MSCA (MarieC Sklodowska-Curie Actions) [801370]
- MINECO [AYA2017-86274-P]
- AGAUR [SGR-661/2017]
- UK Science and Technology Facilities Council [ST/R505195/1, ST/T000406/1]
- Leverhulme Research Fellowship
- European Research Council under the European Union's Horizon 2020 research and innovation programme [677706]
- Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma [GTC6-16B, GTC1-17A, GTC26-17B, GTC6-18A]
- ESO Telescopes at the La Silla Paranal Observatory [0101.B-0130]
- Telescopio Nazionale Galileo and Mercator Telescope [ITP18 8]
- Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
- STFC [ST/T000406/1, ST/R505195/1] Funding Source: UKRI
By analyzing binary stars that have not interacted, the study found a flat age-metallicity relation with a scatter of approximately +/- 0.5 dex around the solar metallicity at all ages. This independently confirms the lack of correlation between age and metallicity in the solar neighborhood observed in previous studies analyzing single main sequence stars and open clusters.
The age-metallicity relation (AMR) is a fundamental tool for constraining the chemical evolution of the Galactic disc. In this work, we analyse the observational properties of this relation using binary stars that have not interacted consisting of a white dwarf (WD) - from which we can derive the total age of the system - and a main sequence (MS) star - from which we can derive the metallicity as traced by the [Fe/H] abundances. Our sample consists of 46 widely separated, but unresolved spectroscopic binaries identified within the Sloan Digital Sky Survey, and 189 WD plus MS common proper motion pairs identified within the second data release of Gaia. This is currently the largest WD sample for which the metallicity of their progenitors have been determined. We find a flat AMR displaying a scatter of [Fe/H] abundances of approximately +/- 0.5 dex around the solar metallicity at all ages. This independently confirms the lack of correlation between age and metallicity in the solar neighbourhood that is found in previous studies focused on analysing single MS stars and open clusters.
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