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Ages and Metallicities of Globular Clusters in NGC 4472

Published online by Cambridge University Press:  03 August 2017

M.A. Beasley ,
R.M. Sharples ,
T.J. Bridges ,
D.A. Hanes ,
S.E. Zepf ,
K.M. Ashman  and
D. Geisler
M.A. Beasley
Affiliation:
University of Durham, Department of Physics, South Road, Durham, DH1 3LE, UK
R.M. Sharples
Affiliation:
University of Durham, Department of Physics, South Road, Durham, DH1 3LE, UK
T.J. Bridges
Affiliation:
Anglo-Australian Observatory, P.O. Box 296, Epping, NSW, 2121, Australia
D.A. Hanes
Affiliation:
Department of Physics, Queen's University, Kingston, ON K7L 3N6, Canada
S.E. Zepf
Affiliation:
Dept. of Astronomy, Yale University, New Haven, CT 06520, USA
K.M. Ashman
Affiliation:
Department of Physics and Astronomy, University of Kansas, Lawrence KS 66045, USA
D. Geisler
Affiliation:
Departamento de Fisica, Grupo de Astronomia, Universidad de Concepción, Casilla 160-C, Concepción, Chile

Abstract

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We have derived ages and metallicities from co-added spectra of 131 globular clusters (GCs) associated with the giant Virgo elliptical NGC 4472. ¿From their metal-line indices, we find that our sample of GCs span a metallicity range of approximately −1.6 ≤ [Fe/H] ≤ 0 dex. The SSP models of Worthey (1994; W94) predict that the metal-poor population of GCs has an age of 14.5 ± 4 Gyr and that the metal-rich population is 13.8 ± 6 Gyr old, whilst the models of Kurth, Fritze-v. Alvensleben & Fricke (1999; KFF99) predict ages of 6.0 ± 2 and 8.0 ± 5 respectively. We conclude that, within the uncertainties, the GCs are old and coeval, and that the bimodality seen in the broadband colours primarily reflects metallicity and not age differences.

Type
Part 2. Globular Cluster Systems of Distant Galaxies
Information
Symposium - International Astronomical Union , Volume 207: Extragalactic Star Clusters , 2002 , pp. 318 - 320
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

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