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Substructure of Galaxy Clusters and Cosmological Constant

Published online by Cambridge University Press:  26 May 2016

Tamon Suwa ,
Asao Habe ,
Kohji Yoshikawa  and
Takashi Okamoto
Tamon Suwa
Affiliation:
Department of Physics, Hokkaido University, Sapporo 060-0810, Japan
Asao Habe
Affiliation:
Department of Physics, Hokkaido University, Sapporo 060-0810, Japan
Kohji Yoshikawa
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan
Takashi Okamoto
Affiliation:
Yukawa Institute, Kyoto University, Kyoto 606-8502, Japan

Abstract

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We calculate some indicators, which are closely related with galaxy clusters' substructure, for each cluster obtained in numerical simulations in OCDM and ΓCDM, and make a statistical comparison between two models. In ΓCDM the indicators, multipole moment power ratios and center shifts, are larger than those in OCDM. This result is consistent with the analytical prediction; galaxy clusters' formation epoch in ΓCDM is later than in OCDM and then clusters in OCDM are more relaxed than those in ΓCDM. We show that these indicators for X-ray surface brightness are useful tools to distinguish between OCDM and ΓCDM.

Type
Posters
Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 447 - 448
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Richstone, D., Loeb, A., & Turner, E. L. 1992, ApJ, 447, 8 Google Scholar
Suwa, T., Habe, A., Yoshikawa, K., & Okamoto, T. 2001 preprint (astro-ph/0108308) Google Scholar
Yoshikawa, K., Jing, Y. P., & Suto, Y. 2000, ApJ, 535, 593 Google Scholar