Hostname: page-component-586b7cd67f-r5fsc Total loading time: 0 Render date: 2024-11-25T10:30:18.253Z Has data issue: false hasContentIssue false
  • English
  • Français

A spectroscopy-based Age-Metallicity Relation of the SMC

Published online by Cambridge University Press:  01 December 2006

Andrea Kayser ,
Eva K. Grebel ,
Daniel R. Harbeck ,
Andrew A. Cole ,
Andreas Koch ,
Katharina Glatt ,
John S. Gallagher  and
Gary S. Da Costa
Andrea Kayser
Affiliation:
Astronomical Institut, U. Basel, Venusstr. 7, 4102 Binningen, Switzerland
Eva K. Grebel
Affiliation:
Astronomical Institut, U. Basel, Venusstr. 7, 4102 Binningen, Switzerland
Daniel R. Harbeck
Affiliation:
Dept. Astronomy, U. Wisconsin, 475 N. Carter St. Madison, WI 53706, USA
Andrew A. Cole
Affiliation:
Astronomy Dept., U. Minnesota, 116 Church St. SE, MN 55455, USA
Andreas Koch
Affiliation:
Astronomical Institut, U. Basel, Venusstr. 7, 4102 Binningen, Switzerland Dept. of Astronomy, U. of California, 430 Portola Plaza, Los Angeles, CA 90095-1547, USA
Katharina Glatt
Affiliation:
Astronomical Institut, U. Basel, Venusstr. 7, 4102 Binningen, Switzerland
John S. Gallagher
Affiliation:
Dept. Astronomy, U. Wisconsin, 475 N. Carter St. Madison, WI 53706, USA
Gary S. Da Costa
Affiliation:
ANU, Mt Stromlo Observatory, Cotter Rd, Weston ACT 2611, Australia
Rights & Permissions [Opens in a new window]

Extract

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 Small Magellanic Cloud (SMC) is the only dwarf galaxy in the Local Group that is known to have formed and preserved populous star clusters continuously over the past 12 Gyr. Due to its proximity (≈ 60 kpc), stars can be resolved well below the oldest main sequence turnoff points. This facilitates accurate age and metallicity determinations without suffering from the age-metallicity degeneracy. Therefore, the SMC star clusters provide a unique closely spaced set of single-age, single-metallicity tracers to derive a well-sampled age-metallicity relation required for the understanding of the star formation history of this satellite galaxy. Up to date spectroscopically based metallicity estimates exist only for the small number of 7 clusters (Da Costa & Hatzidimitriou 1998). Our project now more than doubles the available data set by the observation of 10 additional clusters.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 351 - 352
Copyright
Copyright © International Astronomical Union 2007

References

Armandroff, T. E. & DaCosta, G. S. Costa, G. S., 1991: AJ 101, 1329CrossRefGoogle Scholar
Carretta, E. & Gratton, R. G. 1997: A&AS 121, 95Google Scholar
Cole, et al. 2004: MNRAS 347, 367CrossRefGoogle Scholar
DaCosta, G. S. Costa, G. S. & Hatzidimitriou, D. 1998: AJ 115, 1934Google Scholar
deFreitas Pacheco, J. A. Freitas Pacheco, J. A., Barbuy, B. & Idiart, T. 1998: A&A 332, 19Google Scholar
Mighell, K. J., Sarajedini, A. & French, R. S. 1998: AJ 116, 2395CrossRefGoogle Scholar
Piatti, A. E. et al. 2001: MNRAS 325, 792CrossRefGoogle Scholar
Rutledge, G. A., Hesser, J. E. & Stetson, P. B. 1997: PASP 109, 907CrossRefGoogle Scholar