Structure and Populations of Globular Clusters

Details Structure and Populations of Globular Clusters Structure and Populations of Globular Clusters

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5301k&link_type=abstract

HST Proposal ID #5301

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Hst Proposal Id #5301 Cool Stars Old Clusters

Scientific paper

The globular clusters Omega Centauri and 47 Tucanae will be observed with the "B" and "V" filters of the FOC f/96. An 80-min total in each color will reach well down the main sequence in each cluster, to fainter limiting magnitude than ground-based observations, in central regions that ground-based observations cannot resolve at all. Three FOC fields will be observed in each cluster: at the center, and one and three core radii out. One main objective is to observe the radial distributions of main-sequence stars of different mass, so as to determine the degree of equipartion at the center of each cluster. Along with this goes the luminosity function of the same stars. Another objective is to carry the CMD and luminosity functions as faint as possible. Also, the top of the white-dwarf sequence should be observable. This is a repeat of a program taken with the aberrated HST; it should now be possible, in these crowded regions, to go 3 to 5 magnitudes fainter.

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