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Red-giant branch morphology of metal-poor globular clusters in the Galactic bulge

Published online by Cambridge University Press:  01 July 2007

J. W. Kim ,
H. I. Kim  and
Y. J. Sohn
J. W. Kim
Affiliation:
Department of Astronomy, IEAA, Yonsei University, Seoul 120-749, Korea email: [email protected]
H. I. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea
Y. J. Sohn
Affiliation:
Department of Astronomy, IEAA, Yonsei University, Seoul 120-749, Korea email: [email protected]
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Abstract

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Using the (J − K, K) color-magnitude diagrams (CMDs) of 16 metal-poor globular clusters in the Galactic bulge, we investigate the morphological properties of their red-giant branch (RGB), comparing with those of metal-rich clusters in the Galactic bulge and metal-poor clusters in the Galactic halo. The RGB morphological parameters, such as colors at fixed magnitudes, magnitudes at a fixed color, the RGB slope, and a difference of color indices at two fixed magnitudes have been derived from the near-IR CMDs for each cluster. Metal-poor Galactic bulge clusters follow the previous empirical relations between colors at fixed magnitudes and magnitudes at a fixed color of the RGB and the cluster's metallicity. However, the RGB slope and the color difference parameters of some bulge clusters deviate slightly from the previous empirical linear relations for the other globular clusters, implying that the metal-poor bulge clusters may have different formation origin from the other globular clusters in the Galaxy.

Keywords

Galaxy: structure — Galaxy: globular cluster: general — infrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 363 - 364
Copyright
Copyright © International Astronomical Union 2008

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