Hot Stellar Populations and Their Radial Gradients in Dense Globular Cluster Cores: CYCLE3 Medium

Details Hot Stellar Populations and Their Radial Gradients in Dense Globular Cluster Cores: CYCLE3 Medium Hot Stellar Populations and Their Radial Gradients in Dense Globular Cluster Cores: CYCLE3 Medium

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4366d&link_type=abstract

HST Proposal ID #4366

Physics

Hst Proposal Id #4366

Scientific paper

The goal of this program is to use both the resolving power and the far-UV imaging capability of HST to study the nature of hot stellar populations and their radial gradients in the centers of globular clusters that have undergone core collapse, or are close to it. This continues a Cycle 2 program which used the PC to study the radial gradients among the brighter stars, red giants, subgiants, and horizontal branch (HB) stars. Examination of archival IUE data has indicated that the gradients are present even at far-UV wavelengths. If this is true, some centrally concentrated hot stellar population must be present, e.g., faint BHB stars, blue stragglers, stripped red giant cores, merged stars, or some new, as yet unknown type of objects (recall the recent UIT discoveries of luminous hot UV stars in globulars). High-resolution observations of dense cluster cores in the far-UV are needed in order to check on the existence of population gradients among the hot stars, and establish their nature. Such data would provide essential input for theoretical models (as yet, our understanding of the gradients is very poor), and may be relevant for the origins of x-ray sources and millisecond pulsars in globular clusters, as well as the sources of far-UV light in elliptical galaxies. We propose parallel observations of outer fields using WFC, which would increase the radial baseline for the study of gradients, and substantially increase the true efficiency of the program.

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