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One Micron Photometry of Omega Centauri Giants

Published online by Cambridge University Press:  19 July 2016

Graeme H. Smith
Graeme H. Smith*
Affiliation:
Dominion Astrophysical Observatory Herzberg Institute of Astrophysics

Extract

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The globular cluster ω Centauri is known to be chemically inhomogeneous, a property that reveals itself via a wide giant branch in the V, B-V color-magnitude diagram (Cannon and Stobie 1973). Typically a color range of δ(B-V) = 0.3 − 0.4 exists among giants with V < 13. However, in the red R, R-I (Norris and Bessell 1975, Bessell and Norris 1976), and I, V-I (Lloyd Evans 1977) diagrams a much tighter giant branch is seen. This has lead to the suggestion (e.g. Bessell and Norris 1976) that molecular absorption in the bandpass of the B filter has significantly reddened the B-V color, and thereby produced an anomalously wide giant branch.

Type
Chapter VII. Poster Papers on Harlow Shapley and Globular Clusters in the Milky Way
Information
Symposium - International Astronomical Union , Volume 126: The Harlow-Shapley Symposium on Globular Cluster Systems in Galaxies , 1988 , pp. 503 - 504
Copyright
Copyright © Kluwer 1988 

References

REFERENCES

Bessell, M. S. 1979 Publ. Astron. Soc. Pacific 91, 589.Google Scholar
Bessell, M. S. and Norris, J. 1976 Astrophys. J. 208, 369.Google Scholar
Cannon, R. D. and Stobie, R. S. 1973 Monthly Notices Roy. Astron. Soc. 162, 207.Google Scholar
Lloyd Evans, T. 1977 Monthly Notices Roy. Astron. Soc. 178, 345.CrossRefGoogle Scholar
Persson, S. E., Frogel, J. A., Cohen, J. G., Aaronson, M. and Matthews, K. 1980 Astrophys. J. 235, 452.CrossRefGoogle Scholar
Woolley, R. v. d. R. 1966 Ann. Roy. Obs., No. 2.Google Scholar