Abundances of the brightest member of Tuc III Virtual Observatory Resource

Authors

1. Hansen T.T.
2. Simon J.D.
3. Marshall J.L.
4. Li T.S.
5. Carollo D.
6. Depoy D.L.,Nagasawa D.Q.
7. Bernstein R.A.
8. Drlica-Wagner A.
9. Abdalla F.B.
10. Allam S.,Annis J.
11. Bechtol K.
12. Benoit-Levy A.
13. Brooks D.
14. Buckley-Geer E.,Carnero Rosell A.
15. Carrasco Kind M.
16. Carretero J.
17. Cunha C.E.,da Costa L.N.
18. Desai S.
19. Eifler T.F.
20. Fausti Neto A.
21. Flaugher B.,Frieman J.
22. Garcia-Bellido J.
23. Gaztanaga E.
24. Gerdes D.W.
25. Gruen D.,Gruendl R.A.
26. Gschwend J.
27. Gutierrez G.
28. James D.J.
29. Krause E.
30. Kuehn K.,Kuropatkin N.
31. Lahav O.
32. Miquel R.
33. Plazas A.A.
34. Romer A.K.
35. Sanchez E.,Santiago B.
36. Scarpine V.
37. Smith R.C.
38. Soares-Santos M.
39. Sobreira F.,Suchyta E.
40. Swanson M.E.C.
41. Tarle G.
42. Walker A.R.
43. (the DES Collaboration)

Published by

CDS

Abstract

Chemically peculiar stars in dwarf galaxies provide a window for exploring the birth environment of stars with varying chemical enrichment. We present a chemical abundance analysis of the brightest star in the newly discovered ultra-faint dwarf galaxy candidate TucanaIII. Because it is particularly bright for a star in an ultra-faint Milky Way (MW) satellite, we are able to measure the abundance of 28 elements, including 13 neutron-capture species. This star, DESJ235532.66-593114.9 (DES J235532), shows a mild enhancement in neutron-capture elements associated with the r-process and can be classified as an r-I star. DES J235532 is the first r-I star to be discovered in an ultra-faint satellite, and Tuc III is the second extremely low-luminosity system found to contain r-process enriched material, after Reticulum II. Comparison of the abundance pattern of DES J235532 with r-I and r-II stars found in other dwarf galaxies and in the MW halo suggests a common astrophysical origin for the neutron-capture elements seen in all r-process enhanced stars. We explore both internal and external scenarios for the r-process enrichment of Tuc III and show that with abundance patterns for additional stars, it should be possible to distinguish between them.

Keywords

1. chemical-abundances
2. line-intensities
3. peculiar-variable-stars

Bibliographic source Bibcode

2017ApJ...838...44H

See also HTML

https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/838/44

IVOA Identifier IVOID

ivo://CDS.VizieR/J/ApJ/838/44

Document Object Identifer DOI

doi:10.26093/cds/vizier.18380044

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