Spectroscopic investigation of abundance gradients within galactic globular clusters. I - 47 Tucanae

Details Spectroscopic investigation of abundance gradients within galactic globular clusters. I - 47 Tucanae Spectroscopic investigation of abundance gradients within galactic globular clusters. I - 47 Tucanae

Feb 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979aj.....84..176s&link_type=abstract

Astronomical Journal, vol. 84, Feb. 1979, p. 176, 177, 179-185.

Astronomy and Astrophysics

Astronomy

13

Abundance, Astronomical Spectroscopy, Globular Clusters, Metallic Stars, Stellar Spectra, Astronomical Models, Balmer Series, Dwarf Stars, Dynamic Models, Giant Stars, K Lines, Line Spectra, Radio Telescopes, Star Distribution, Stellar Evolution, Stellar Magnitude, Stellar Mass

Scientific paper

High-spatial-resolution image-tube integrated spectra are analyzed which were obtained at eight distinct positions in the southern globular cluster 47 Tuc over the wavelength range from 3800 to 5500 A with a reciprocal resolution of 120 A/mm. The overall appearance of a cluster spectrum is found to resemble that of a mid-to-late G dwarf or subgiant. The strength of the 3883-A band is used as a measure of CN, the equivalent width of the Ca II K line at 3933 A is measured with respect to a pseudocontinuum, an index measuring the strength of the 4227-A Ca I line is determined, and CH strength is evaluated on the basis of the equivalent width of the G band. An averaged Balmer-line strength is calculated, an equivalent width is measured for the blended Mg I b triplet (5167, 5173, and 5183 A), and a (B/V) photographic color index is established. Dynamical models of 47 Tuc are employed to interpret the observed trends in the strengths of the different spectral features. It is concluded that the integrated spectra provide significant but not conclusive evidence for a small radial abundance gradient for at least some elements.

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