Annu. Rev. Astron. Astrophys. 1996. 34: 511-550
Copyright © 1996 by . All rights reserved

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We conclude this paper by listing observations we hope will be made and papers we hope will be written on the old and intermediate-age populations in the Magellanic Clouds:

  1. Deep, wide-field field star photometry in both Clouds.
  2. Complete samples of ages and abundances of clusters in well-defined areas of the Clouds.
  3. Precise ages of the oldest Cloud clusters.
  4. Definitive evidence for or against a blue HB in the Cloud fields.
  5. Red Clump magnitude distributions in the central and western portions of the SMC, keeping in mind that the northeast and east regions of the SMC have a large Line-of-sight depth.
  6. Magnitude and structure of the intermediate-age red clump and of the old red HB in the LMC.
  7. Identification and spectroscopy of radially distant mass tracers in the LMC.
  8. Detailed abundances, especially [alpha / Fe] for the ancient population and for the stars and clusters in the LMC burst that began 4 Gyr ago.
  9. Metallicity distribution of clump giants.
  10. Star-formation rates in both Clouds, based on deep field star photometry.
  11. Abundances of a large sample of SMC clusters.
  12. Identification of metal-rich RR Lyraes in the LMC and the abundance-luminosity relation for RR Lyraes.
  13. An RR Lyrae survey in the SMC.
  14. A firm photometric footing for the previous RR Lyrae work.
  15. Age of the youngest RR Lyraes.
  16. Resolution of the RR Lyrae and Cepheid distance scales in the Clouds.
  17. Velocity dispersion of RR Lyrae stars and extremely metal poor giants in the LMC.
  18. Catalogs of anomalous Cepheids in the Clouds.
  19. Identification of long-period variables in the Cloud clusters.
  20. Proper motions of the globular clusters thought to once be Cloud members, but are now Milky Way members.
  21. Modeling of dynamical changes in Cloud clusters if they were removed from the Clouds and put into the Milky Way halo.
  22. Continued detailed modeling of the Cloud/Galaxy interactions, with an eye to providing times of strongest interactions.
  23. Search for tidal signatures in field star components of the Clouds and the Magellanic Stream.
  24. Improved proper motions of the Clouds.


EO was partly supported by the NSF through grants AST92-10830 and AST92-23967. NBS gratefully acknowledges the hospitality of the Dominion Astrophysical Observatory where part of this review was written. MM was partly supported by the NSF through grants AST91-18086 and AST92-23968.

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