GRADIENTS IN GIANT BRANCH MORPHOLOGY IN THE CORE OF 47 TUCANAE

I describe an algorithm which uses the high spatial resolution of the Hubble Space Telescope to complement the high signal-to-noise, approximately symmetric point response function, relatively large spatial coverage, and standard filters available from ground based images of crowded fields. Applying this technique to the central regions of the globular cluster 47 Tucanae, I find that the morphology of the giant branch in the core is significantly different from that in more distant regions (r almost equal to 5-10 core radii) of the cluster. In particular, there appear to be fewer bright giants in the core, along with an enhanced ''asymptotic giant branch'' sequence. Depletion of giants has been observed in the cores of other dense clusters, and may be due to ''stripping'' of large stars by stellar encounters and/or mass transfer in binary systems. Central concentrations of true asymptotic giant branch stars are not expected to result from dynamical processes; possibly some of these stars may be evolved blue stragglers.