Structure of Globular Clusters

Details Structure of Globular Clusters Structure of Globular Clusters

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990hst..prop.1279k&link_type=abstract

HST Proposal ID #1279

Physics

Hst Proposal Id #1279

Scientific paper

Four contrasting clusters are studied, to elucidate the differences in their dynamics. Omega Centauri and 47 Tucanae are normal clusters but differ in relaxation time by a factor of 30; they should show interesting differences of structure due to differences in anistropy and equipartition. NGC 6624 has a collapsed core, which has never been resolved. NGC 6752 is a concentrated cluster with a small distance modulus and can be studied quite faint. Each cluster is observed in B and V at the center and at 1 and 3 core radii; ground-based data will be secured to carry the distributions farther out. The distributions of all types of stars should be delineated, down to and including red dwarfs and white dwarfs. Far-UV exposures are made at the centers of M15 and NGC 6624, to search for possible counterparts to the X-ray sources, and in the NGC 6752, to determine the temperatures of the BHB stars. Simultaneous exposures are made in V and I with the WFC, to gain further structural information.

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