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The kinematics and abundances of star clusters in the Large Magellanic Cloud

Published online by Cambridge University Press:  19 July 2016

R. A. Schommer
R. A. Schommer*
Affiliation:
Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile

Abstract

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We present velocities for 75 star clusters in the Large Magellanic Cloud (LMC), based on individual star measures at the Calcium triplet The spectra are also used to derive abundances for most of the clusters, and an age-metallicity relation is presented for the inner and outer regions. One half of the clusters are objects in the outer parts of the LMC (radius ≥5°), which had no previous velocity determinations. Published velocities for intermediate and old clusters are shown to have had systematic errors. We compare these velocities with various rotation curve analyses of the LMC, and test aspects of the twisted disk model of Freeman et al. (1983, hereafter FIO). Our outer cluster sample and the intermediate age inner clusters form a disk which agrees with the parameters of the optical isophotes and inner HI rotation curve. The oldest clusters are still enigmatic; they appear to be flattened and rotate much as FIO have described, although the parameters are poorly determined in this small sample.

Type
Star Formation and Clustering
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 171 - 176
Copyright
Copyright © Kluwer 1991 

References

Cohen, J. (1982), Ap. J. 258, 143.Google Scholar
Da Costa, G.S. (1988), IAU Symp, 126 Globular Cluster Systems in Galaxies , Grindlay, J.E., Philip, A.G.C. (eds.) (Reidel: Dordrecht) p.217.Google Scholar
Feitzinger, J., Isserstedt, J., Schmidt-Kahler, Th. (1977), Astron. Astrophys. 57, 265.Google Scholar
Freeman, K.C., Illingworth, G., Oemler, A. (1983), Ap. J. 272, 488. (FIO).Google Scholar
Jones, B., Klemola, A., Lin, D.C. (1989), Bull. A.A.S. 21, 1107.Google Scholar
Mateo, M. (1988), IAU Symp. 126 Globular Cluster Systems in Galaxies , Grindlay, J.E., Philip, A.G.C. (eds.) (Reidel: Dordrecht) p. 557.Google Scholar
Mateo, M., Hodge, P.W., Schommer, R.A. (1986), Ap. J. 311, 113.Google Scholar
Olszewski, E. (1988), IAU Symp. 126 Globular Cluster Systems in Galaxies , Grindlay, J.E., Philip, A.G.C. (eds.) (Reidel: Dordrecht) p. 159.Google Scholar
Olszewski, E., Harris, H., Schommer, R., Canterna, R. (1988), Astron. Journ. 95, 84.Google Scholar
Prevot, L., Rousseau, J., Martin, N. (1989), Astron. Astrophys. 225, 303.Google Scholar
Searle, L., Wilkinson, A., Bagnuolo, W.G. (1980), Ap. J. 239, 803. (SWB).Google Scholar
Zinn, R., (1985), Ap. J. 293, 424.Google Scholar