Constraining the solar neighbourhood age-metallicity relation from white dwarf-main sequence binaries

Rebassa-Mansergas, A.; Maldonado, J.; Raddi, R.; Knowles, A. T.; Torres, S.; Hoskin, M.; Cunningham, T.; Hollands, M.; Ren, J.; Gänsicke, B. T.; Tremblay, P. -E.; Castro-Rodríguez, N.; Camisassa, M.; Koester, D.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society

Advertised on:
8
2021
Description
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.
Related projects
NGC 2808 Globular Cluster
Milky Way and Nearby Galaxies

The general aim of the project is to research the structure, evolutionary history and formation of galaxies through the study of their resolved stellar populations, both from photometry and spectroscopy. The group research concentrates in the most nearby objects, namely the Local Group galaxies including the Milky Way and M33 under the hypothesis

Martín
López Corredoira