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Population Models for Massive Globular Clusters

Published online by Cambridge University Press:  05 March 2015

Young-Wook Lee ,
Seok-Joo Joo ,
Sang-Il Han ,
Chongsam Na ,
Dongwook Lim  and
Dong-Goo Roh
Young-Wook Lee
Affiliation:
Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 120-749, Korea email: ywlee2@yonsei.ac.kr
Seok-Joo Joo
Affiliation:
Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 120-749, Korea email: ywlee2@yonsei.ac.kr
Sang-Il Han
Affiliation:
Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 120-749, Korea email: ywlee2@yonsei.ac.kr
Chongsam Na
Affiliation:
Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 120-749, Korea email: ywlee2@yonsei.ac.kr
Dongwook Lim
Affiliation:
Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 120-749, Korea email: ywlee2@yonsei.ac.kr
Dong-Goo Roh
Affiliation:
Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 120-749, Korea email: ywlee2@yonsei.ac.kr
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Increasing number of massive globular clusters (GCs) in the Milky Way are now turned out to host multiple stellar populations having different heavy element abundances enriched by supernovae. Recent observations have further shown that [CNO/Fe] is also enhanced in metal-rich subpopulations in most of these GCs, including ω Cen and M22 (Marino et al. 2011, 2012). In order to reflect this in our population modeling, we have expanded the parameter space of Y2 isochrones and horizontal-branch (HB) evolutionary tracks to include the cases of normal and enhanced nitrogen abundances ([N/Fe] = 0.0, 0.8, and 1.6). The observed variations in the total CNO content were reproduced by interpolating these nitrogen enhanced stellar models. Our test simulations with varying N and O abundances show that, once the total CNO sum ([CNO/Fe]) is held constant, both N and O have almost identical effects on the HR diagram (see Fig. 1).

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 247 - 248
Copyright
Copyright © International Astronomical Union 2015 

References

Joo, S.-J. & Lee, Y.-W. 2013, ApJ, submittedGoogle Scholar
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Marino, A. F., Sneden, C., Kraft, R. P., et al. 2011, A&A 532, A8Google Scholar
Marino, A. F., Milone, A. P., Piotto, G., et al. 2012, ApJ 746, 14CrossRefGoogle Scholar
Roh, D.-G., Lee, Y.-W., Joo, S.-J., Han, S.-I., Sohn, Y.-J., & Lee, J.-W. 2011, ApJ 733, L45CrossRefGoogle Scholar