Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-04T21:10:08.637Z Has data issue: false hasContentIssue false
  • English
  • Français

The age-metallicity relation from a sample of white dwarf-main sequence binaries

Published online by Cambridge University Press:  02 August 2018

A. Rebassa-Mansergas ,
B. Anguiano ,
E. García-Berro  and
K. C. Freeman
A. Rebassa-Mansergas
Affiliation:
Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain email: [email protected] Institute for Space Studies of Catalonia, c/Gran Capità 2–4, Edif. Nexus 201, 08034 Barcelona, Spain
B. Anguiano
Affiliation:
Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA
E. García-Berro
Affiliation:
Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain email: [email protected] Institute for Space Studies of Catalonia, c/Gran Capità 2–4, Edif. Nexus 201, 08034 Barcelona, Spain
K. C. Freeman
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The age-metallicity relation (AMR) is a fundamental observational constraint for understanding how the Galactic disc formed and evolved chemically in time. However, there is not yet an agreement on the observational properties of the AMR, primarily due to the difficulty in obtaining accurate ages for individual field stars. We have started an observational campaign for providing new observational input by using wide white dwarf-main sequence (WDMS) binaries. WDs are natural clocks and can be used to derive accurate ages. Metallicities can be obtained from the MS companions. Since the progenitors of WDs and the MS stars were born at the same time, WDMS provide a unique opportunity to constrain in a robust way the properties of the AMR. We present the AMR derived from analysing a pilot sample of 23 WDMS and provide clear evidence for the lack of correlation between age and metallicity at young and intermediate ages.

Keywords

Galaxy: fundamental parameters(Galaxy:) solar neighborhood(stars:) white dwarfsstars: late-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 355 - 357
Copyright
Copyright © International Astronomical Union 2018 

References

Bergemann, M., Ruchti, G. R., Serenelli, A., et al. 2014, A&A, 565, A89Google Scholar
Catalán, S., Isern, J., García-Berro, E., & Ribas, I., 2008, MNRAS, 387, 1693Google Scholar
Newton, E. R., Charbonneau, D., Irwin, J., et al. 2014, AJ, 147, 20Google Scholar
Rebassa-Mansergas, A., Gänsicke, B. T., Rodríguez-Gil, P., Schreiber, M. R., & Koester, D., 2007, MNRAS, 382, 1377Google Scholar
Rebassa-Mansergas, A., Gänsicke, B. T., Schreiber, M. R., Koester, D., & Rodríguez-Gil, P., 2010, MNRAS, 402, 620Google Scholar
Rebassa-Mansergas, A., Ren, J. J., Parsons, S. G., et al. 2016a, MNRAS, 458, 3808Google Scholar
Rebassa-Mansergas, A., Anguiano, B., García-Berro, E., et al., 2016b, MNRAS, 463, 1137Google Scholar
Renedo, I., Althaus, L. G., Miller Bertolami, M. M., et al. 2010, ApJ, 717, 183Google Scholar
Soderblom, D. R., 2010, ARA&A, 48, 581Google Scholar
Soubiran, C., Bienaymé, O., Mishenina, T. V., & Kovtyukh, V. V., 2008, A&A, 480, 91Google Scholar