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The dynamics of cluster substructure

Published online by Cambridge University Press:  06 October 2004

Stuart P. D. Gill ,
Alexander Knebe  and
Brad K. Gibson
Stuart P. D. Gill
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, P.O. Box 218, Hawthorn, VIC 3122, Australia email: sgill@astro.swin.edu.au
Alexander Knebe
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, P.O. Box 218, Hawthorn, VIC 3122, Australia email: sgill@astro.swin.edu.au
Brad K. Gibson
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, P.O. Box 218, Hawthorn, VIC 3122, Australia email: sgill@astro.swin.edu.au
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Abstract

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To understand cluster formation and evolution it is important to understand the evolution of cluster substructure. The work described here focuses upon a set of fully self-consistent numerical simulations within a $\Lambda$CDM cosmology. Within the simulations we follow in detail the temporal and spatial properties of individually tracked satellite galaxies. The host galaxy clusters were chosen to sample a variety of formation histories, ages, and triaxialities. Despite their obvious differences, we find striking similarities within the associated substructure populations. Namely, the satellite galaxy orbital distributions are indistinguishable between the galaxy clusters.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUC195 , March 2004 , pp. 280 - 284
Copyright
© 2004 International Astronomical Union