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Improved dynamical modelling of the Arches cluster

Published online by Cambridge University Press:  22 May 2014

Joowon Lee  and
Sungsoo S. Kim
Joowon Lee
Affiliation:
School of Space Research, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea email: jwlee9033@khu.ac.kr
Sungsoo S. Kim
Affiliation:
School of Space Research, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea email: jwlee9033@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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Recently, Clarkson et al. (2012) measured the intrinsic velocity dispersion of the Arches cluster, a young and massive star cluster in the Galactic center. Using the observed velocity dispersion profile and the surface brightness profile of Espinoza et al. (2009), they estimate the cluster's present-day mass to be ∼ 1.5×104 M⊙ by fitting an isothermal King model. In this study, we trace the best-fit initial mass for the Arches cluster using the same observed data set and also the anisotropic Fokker-Planck calculations for the dynamical evolution.

Keywords

Galaxy: globular clusters: individual(Arches)–Galaxy: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S303: The Galactic Center: Feeding and Feedback in a Normal Galactic Nucleus , October 2013 , pp. 59 - 60
Copyright
Copyright © International Astronomical Union 2014 

References

Clarkson, W. I., Ghez, A. M., Morris, M. R., et al. 2012, ApJ 751, 132Google Scholar
Espinoza, P. & Selman, F. J., Melnic, J. 2009, A&A 501, 563Google Scholar
Kim, S. S., Figer, D. F., Kudritzki, R. P., & Najarro, F. 2006, ApJ 653, L113Google Scholar
Kim, S. S., Morris, M., & Lee, H. M. 1999, ApJ 525, 22Google Scholar