4. WISH LIST
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:
- Deep, wide-field field star photometry in both Clouds.
- Complete samples of ages and abundances of clusters in well-defined
areas of the Clouds.
- Precise ages of the oldest Cloud clusters.
- Definitive evidence for or against a blue HB in the Cloud fields.
- 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.
- Magnitude and structure of the intermediate-age red clump and of
the old red HB in the LMC.
- Identification and spectroscopy of radially distant mass tracers in
- Detailed abundances, especially
[ / Fe] for the ancient
population and for the stars and clusters in the LMC burst that began 4 Gyr ago.
- Metallicity distribution of clump giants.
- Star-formation rates in both Clouds, based on deep field star
- Abundances of a large sample of SMC clusters.
- Identification of metal-rich RR Lyraes in the LMC and the abundance-luminosity relation for RR
- An RR Lyrae survey in the SMC.
- A firm photometric footing for the previous RR Lyrae work.
- Age of the youngest RR Lyraes.
- Resolution of the RR Lyrae and Cepheid distance scales in the
- Velocity dispersion of RR Lyrae stars and extremely metal poor
giants in the LMC.
- Catalogs of anomalous Cepheids in the Clouds.
- Identification of long-period variables in the Cloud clusters.
- Proper motions of the globular clusters thought to once be Cloud
members, but are now Milky Way members.
- Modeling of dynamical changes in Cloud clusters if they were
removed from the Clouds and put into the Milky Way halo.
- Continued detailed modeling of the Cloud/Galaxy interactions, with
an eye to providing times of strongest interactions.
- Search for tidal signatures in field star components of the Clouds
and the Magellanic Stream.
- 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.