Abundances of solar neighbourhood stars Virtual Observatory Resource

Authors
  1. Zenoviene R.
  2. Tautvaisiene G.
  3. Nordstroem B.
  4. Stonkute E.
  5. Barisevicius G.
  6. Published by
    CDS
Abstract

A combined study of kinematics and chemical composition of stars is one of the most promising tools of research in Galaxy formation. The main goal in this field of research is to reconstruct the formation history of our Galaxy, to reveal the origin of the thick disc, and to find remnants of ancient mergers. We determine detailed elemental abundances in stars belonging to the so-called Group 1 of the Geneva-Copenhagen survey (GCS) and compare the chemical composition with the Galactic thin- and thick-disc stars, with the GCS Group 2 and Group 3 stars, as well as with several kinematic streams of similar metallicities. The aim is to search for chemical signatures that might give information about the formation history of this kinematic group of stars. High-resolution spectra were obtained with the Fibre-fed Echelle Spectrograph spectrograph at the Nordic Optical Telescope, La Palma, and were analysed with a differential model atmosphere method. Comparison stars were observed and analysed with the same method. The average value of [Fe/H] for the 37 stars of Group 1 is -0.20+/-0.14dex. Investigated Group 1 stars can be separated into three age subgroups. Along with the main 8- and 12-Gyr-old populations, a subgroup of stars younger than 5Gyr can be separated as well. Abundances of oxygen, {alpha}-elements, and r-process dominated elements are higher than in Galactic thin-disc dwarfs. This elemental abundance pattern has similar characteristics to that of the Galactic thick disc and differs slightly from those in Hercules, Arcturus, and AF06 stellar streams. The similar chemical composition of stars in Group 1, as well as in Group 2 and 3, with that in stars of the thick disc might suggest that their formation histories are linked. The chemical composition pattern together with the kinematic properties and ages of stars in the investigated GCS groups provide evidence of their common origin and possible relation to an ancient merging event. A gas-rich satellite merger scenario is proposed as the most likely origin.

Keywords
  1. chemical-abundances
Bibliographic source Bibcode
2015A&A...576A.113Z
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/576/A113
IVOA Identifier IVOID
ivo://CDS.VizieR/J/A+A/576/A113
Document Object Identifer DOI
doi:10.26093/cds/vizier.35760113

Access

Web browser access HTML
http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/576/A113
https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/576/A113
http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/576/A113
IVOA Table Access TAP
http://tapvizier.cds.unistra.fr/TAPVizieR/tap
Run SQL-like queries with TAP-enabled clients (e.g., TOPCAT).
IVOA Cone Search SCS
For use with a cone search client (e.g., TOPCAT).
http://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/576/A113/abund?
https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/576/A113/abund?
http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/576/A113/abund?

History

2015-07-31T08:57:58Z
Resource record created
2015-07-31T08:57:58Z
Created
2017-06-22T14:29:24Z
Updated

Contact

Name
CDS support team
Postal Address
CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France
E-Mail
cds-question@unistra.fr