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K-Line Photometry: Coma and NGC 6475

Published online by Cambridge University Press:  14 August 2015

Richard C. Henry  and
James E. Hesser
Richard C. Henry
Affiliation:
The Johns Hopkins University
James E. Hesser
Affiliation:
Cerro Tololo Inter-American Observatory

Abstract

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Photometry of the K line of calcium in A-type stars is useful in segregation of Am stars and in estimating the metal abundance of field stars and of stars in clusters. To date, K-line photometry data for six clusters have been analyzed using uvbyß data: Hyades, Pleiades, IC 2391, and IC 2602 (Hesser and Henry 1971), Orion (Hesser, McClintock, and Henry 1977), and Praesepe (Henry, Anderson, and Hesser 1977). We present similar analyses for the Coma and NGC 6475 star clusters, using the uvbyß data of Crawford and Barnes (1969) and of Snowden (1976) respectively. The Coma stars closely resemble field stars. NGC 6475, on the other hand, is most remarkable. Of 31 stars for which complete data are available, 9 are metal-rich, 3 are metal-poor, and 19 (about 2/3 of the stars!) are Am.

Type
Part IV: HR Diagrams, Clusters
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 161 - 162
Copyright
Copyright © Reidel 1978 

References

Crawford, D. L., and Barnes, J. V. (1969). Astron. J. 74, 407.Google Scholar
Henry, R. C., Anderson, R., and Hesser, J. E. (1977). Astrophys. J. 214, 742.Google Scholar
Hesser, J. E., and Henry, R. C. (1971). Astrophys. J. Suppl. 202, 453.Google Scholar
Hesser, J. E., McClintock, W., and Henry, R. C. (1977). Astrophys. J. 213, 100.Google Scholar
Snowden, M. S. (1976). Publ. Astron. Soc. Pacific 88, 174.Google Scholar