Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 473, Issue 4, Pages 5393-5406Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx2685
Keywords
stars: abundances; binaries: visual; Galaxy: structure
Categories
Funding
- European Research Councilunder the European Union's Seventh Framework Programme/ERC [617001]
- Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio [IC120009]
- Centro de Astronomia y Tecnologias Afines [PFB-06]
- National Science Foundation [PHY-1607611]
- Simons Foundation
- National Development and Reform Commission
- Australian Astronomical Observatory
- Leibniz-Institut fuer Astrophysik Potsdam (AIP)
- Australian National University
- Australian Research Council
- French National Research Agency
- German Research Foundation [SPP1177, SFB 881]
- European Research Council(ERC-StG) [240271]
- Istituto Nazionale di Astrofisicaat Padova
- Johns HopkinsUniversity
- National Science Foundationof the USA [AST-0908326]
- W. M. Keck foundation
- Macquarie University
- Netherlands Research School for Astronomy
- Natural Sciences and Engineering Research Council of Canada
- Slovenian Research Agency
- Swiss National Science Foundation
- Science & Technology Facilities Council of the UK
- Opticon
- Strasbourg Observatory
- University of Groningen
- University of Heidelberg
- University of Sydney
- European Research Council (ERC) [240271] Funding Source: European Research Council (ERC)
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From our recent catalogue based on the first Gaia data release (TGAS), we select wide binaries in which both stars have been observed by the Radial Velocity Experiment (RAVE) or the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). Using RAVE and LAMOST metallicities and RAVE Mg, Al, Si, Ti and Fe abundances, we find that the differences in the metallicities and elemental abundances of components of wide binaries are consistent with being due to observational uncertainties, in agreement with previous results for smaller and more restricted samples. The metallicity and elemental abundance consistency between wide binary components presented in this work confirms their common origin and bolsters the status of wide binaries as 'mini-open clusters'. Furthermore, this is evident that wide binaries are effectively co-eval and co-chemical, supporting their use for, e.g. constraining age-activity-rotation relations, the initial-final mass relation for white dwarfs and M-dwarf metallicity indicators. Additionally, we demonstrate that the common proper motion, common parallax pairs in TGAS with the most extreme separations (s greater than or similar to 0.1 pc) typically have inconsistent metallicities, radial velocities or both and are therefore likely to be predominantly comprised of random alignments of unassociated stars with similar astrometry, in agreement with our previous results. Finally, we propose that wide binaries form an ideal data set with which we can test chemical tagging as a method to identify stars of common origin, particularly because the stars in wide binaries span a wide range of metallicities, much wider than that spanned by nearby open clusters.
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