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Results from HST Observations of Six LMC Globular Cluster Fields

  • K. A. G. Olsen (a1), P. W. Hodge (a2), M. Mateo (a3), E. W. Olszewski (a4), R. A. Schommer (a1), N. B. Suntzeff (a1) and A. R. Walker (a1)...

Abstract

We present deep HST color-magnitude diagrams of fields centered on the six old LMC globular clusters NGC 1754, NGC 1835, NGC 1898, NGC 1916, NGC 2005, and NGC 2019. Separate cluster and field star CMDs are shown. The time of formation of the LMC is studied from an analysis of the cluster CMDs. Based on a comparison of the CMDs with sequences of the Milky Way clusters M3, M5, and M55, we suggest that the LMC formed its first stars at the same time as the Milky Way to within 1 Gyr. We find additional evidence that these LMC globular clusters are as old as the oldest Milky Way clusters through a comparison of our data with the horizontal branch evolutionary models of Lee, Demarque, & Zinn (1994).

The evolution of the LMC following its formation is studied through an analysis of the field star CMDs. Through an automated comparison with stellar evolution models, we extract the star formation histories implied by the CMDs. Our best-fit star formation histories imply that the LMC has been actively forming stars over the last 4 Gyr, in agreement with previous field star studies. The four fields that lie in the Bar also contain significant numbers of stars with ages of 4–8 Gyr in the best-fit cases. The most notable disagreement between the best-fit models and observed CMDs is in the color of the red giant branch.

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References

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Bertelli, G. et al. 1994, A&AS, 106, 275
Dolphin, A. 1997, New Astronomy, 2, 397
Lee, Y.-W., Demarque, P., & Zinn, R. 1994, ApJ, 423, 248
VandenBerg, D., Bolte, M., & Stetson, P. 1990, AJ, 100, 445

Results from HST Observations of Six LMC Globular Cluster Fields

  • K. A. G. Olsen (a1), P. W. Hodge (a2), M. Mateo (a3), E. W. Olszewski (a4), R. A. Schommer (a1), N. B. Suntzeff (a1) and A. R. Walker (a1)...

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