Other
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....106.1024b&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 106, no. 3, p. 1024-1048.
Other
29
Globular Clusters, Stellar Luminosity, Abundance, Color-Magnitude Diagram, Metallicity, Star Distribution, Stellar Spectrophotometry, Ubv Spectra
Scientific paper
New BV CCD photometry for the bright stars in the core region of NGC 288, independently calibrated with Landolt (1983) and Graham (1982) standard stars, is presented. In contrast with the color-magnitude diagram of Buonanno et al. (1984), there are no obvious gaps along the giant branch, but two distinct gaps are evident in the distribution of stars along the horizontal branch (HB), one near V = 15.7 and one near V = 16.5. The faint blue HB stars defined by the gap at V = 16.5 are more centrally concentrated than the other HB stars; 80 percent of them are found within one core radius (1.6 arcmin) of the cluster center. From HB, isochrone, and luminosity function considerations, the preferred parameters are: Age= 14 Gyr, Fe/H = - 1.26, (m-MV) = 14.90, and E(B-V) = 0.03. Application of the R method calibrated by Caputo et al. (1987) gives a mass fraction helium abundance Y = 0.232 +0.020 -0.036, in excellent agreement with the value (Y = 0.236) adopted by VandenBerg (1992) for the oxygen-enhanced Fe/H = -1.26 evolutionary sequences. Since the age is comparable to that of the extreme metal-poor globular clusters with similar HB morphologies, it is argued that age cannot by itself account for the second parameter effect.
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