The metal-rich globular cluster NGC 6553 - Clump morphology and age

Details The metal-rich globular cluster NGC 6553 - Clump morphology and age The metal-rich globular cluster NGC 6553 - Clump morphology and age

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...265...40d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 265, no. 1, p. 40-42.

Astronomy and Astrophysics

Astrophysics

4

Abundance, Globular Clusters, Horizontal Branch Stars, Metallic Stars, Cepheid Variables, Stellar Evolution, Stellar Luminosity, Stellar Models

Scientific paper

Stellar evolutionary tracks for metal-rich HB stars have been used to construct synthetic population models for the peculiar HB clump in NGC 6553. Although the uncertainties are large, it is possible to derive an age for NGC 6553 in the range 8-13 Gyr, which supports the idea that the disk globular cluster system is younger than the oldest stars in the Galactic halo and bulge.

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