On the radial distribution of white dwarfs in the globular cluster NGC 6397

Author:

Davis D. S.1,Richer H. B.1,King I. R.2,Anderson J.3,Coffey J.1,Fahlman G. G.4,Hurley J.5,Kalirai J. S.6

Affiliation:

1. 1Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC, V6T 1Z1, Canada

2. 2Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA

3. 3Department of Physics & Astronomy, Rice University, 6100 Main Street, Houston, TX 77005, USA

4. 4Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada

5. 5Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia

6. 6University of California at Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA

Abstract

Abstract We have examined the radial distribution of white dwarfs over a single Hubble Space Telescope/Advanced Camera for Surveys field in the nearby globular cluster NGC 6397. In relaxed populations, such as in a globular cluster, stellar velocity dispersion, and hence radial distribution, is directly dependent on stellar masses. The progenitors of very young cluster white dwarfs had a mass of ∼0.8 M⊙, while the white dwarfs themselves have a mass of ∼0.5 M⊙. We thus expect young white dwarfs to have a concentrated radial distribution (like that of their progenitors) that becomes more extended over several relaxation times to mimic that of ∼0.5-M⊙ main-sequence stars. However, we observe young white dwarfs to have a significantly extended radial distribution compared both with the most massive main-sequence stars in the cluster and with old white dwarfs.

Publisher

Oxford University Press (OUP)

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