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Globular Clusters within Dark Matter Halos: Case Studies of 47 Tuc, NGC 1851 and M 15

Published online by Cambridge University Press:  31 March 2017

Joowon Lee ,
Jihye Shin  and
Sungsoo S. Kim
Joowon Lee
Affiliation:
School of Space Research, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea email: joowon.lee@khu.ac.kr
Jihye Shin
Affiliation:
Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, China
Sungsoo S. Kim
Affiliation:
School of Space Research, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea email: joowon.lee@khu.ac.kr Department of Astronomy and Space Science, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea
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Abstract

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Globular clusters (GCs) are known to have a very small amount of or no dark matter (DM). Even if GCs are formed in individual DM halos, they must have lost the majority of the DM through dynamical processes such as mass segregation or tidal stripping. Using Fokker-Planck (FP) calculations, we investigate the dynamical evolution of three Galactic GCs with an assumption that they were formed in mini DM halos. We trace the amount of DM of 47 Tuc, NGC 1851, and M 15, which are a ‘disk/bulge’ cluster, an ‘old halo’ cluster, and a ‘young halo’ cluster, respectively. We find that these three GCs must have initially had insignificant amounts of DM, less than 10 percent of the initial stellar mass of each cluster.

Keywords

stellar dynamicsmethods: numericalgalaxy: globular clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S316: Formation, evolution, and survival of massive star clusters , August 2015 , pp. 336 - 337
Copyright
Copyright © International Astronomical Union 2017 

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