Red giants in NGC 5286 Virtual Observatory Resource

Authors
  1. Marino A.F.
  2. Milone A.P.
  3. Karakas A.I.
  4. Casagrande L.
  5. Yong D.,Shingles L.
  6. Da Costa G.
  7. Norris J.E.
  8. Stetson P.B.
  9. Lind K.
  10. Asplund M.,Collet R.
  11. Jerjen H.
  12. Sbordone L.
  13. Aparicio A.
  14. Cassisi S.
  15. Published by
    CDS
Abstract

We present a high-resolution spectroscopic analysis of 62 red giants in the Milky Way globular cluster (GC) NGC 5286. We have determined abundances of representative light proton-capture, {alpha}, Fe-peak and neutron-capture element groups, and combined them with photometry of multiple sequences observed along the colour-magnitude diagram. Our principal results are: (i) a broad, bimodal distribution in s-process element abundance ratios, with two main groups, the s-poor and s-rich groups; (ii) substantial star-to-star Fe variations, with the s-rich stars having higher Fe, e.g. <[Fe/H]_s-rich_-<[Fe/H]>_s-poor_~0.1dex; and (iii) the presence of O-Na-Al (anti)correlations in both stellar groups. We have defined a new photometric index, c_BVI_=(B-V)-(V-I), to maximize the separation in the colour-magnitude diagram between the two stellar groups with different Fe and s-element content, and this index is not significantly affected by variations in light elements (such as the O-Na anticorrelation). The variations in the overall metallicity present in NGC 5286 add this object to the class of anomalous GCs. Furthermore, the chemical abundance pattern of NGC 5286 resembles that observed in some of the anomalous GCs, e.g. M 22, NGC 1851, M 2, and the more extreme {omega} Centauri, that also show internal variations in s-elements, and in light elements within stars with different Fe and s-elements content. In view of the common variations in s-elements, we propose the term s-Fe-anomalous GCs to describe this sub-class of objects. The similarities in chemical abundance ratios between these objects strongly suggest similar formation and evolution histories, possibly associated with an origin in tidally disrupted dwarf satellites.

Keywords
  1. globular-star-clusters
  2. giant-stars
  3. chemical-abundances
Bibliographic source Bibcode
2015MNRAS.450..815M
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/450/815
IVOA Identifier IVOID
ivo://CDS.VizieR/J/MNRAS/450/815
Document Object Identifer DOI
doi:10.26093/cds/vizier.74500815

Access

Web browser access HTML
http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/450/815
https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/450/815
http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/450/815
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/MNRAS/450/815/table2?
https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/450/815/table2?
http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/450/815/table2?

History

2016-03-16T14:08:46Z
Resource record created
2016-03-16T14:08:46Z
Created
2024-08-14T20:22:08Z
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