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Cosmological Parameters from the X-Ray Evolution of Clusters

Published online by Cambridge University Press:  25 May 2016

R.G. Bower
Affiliation:
University of Durham Department of Physics, Science Laboratories, South Road, Durham DH1 3LE, UK
S.T. Kay
Affiliation:
University of Durham Department of Physics, Science Laboratories, South Road, Durham DH1 3LE, UK

Extract

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This poster paper presents an extension of the entropy-driven model of cluster evolution developed by Bower, 1997 (MN, 288, 355) in order to study the evolution of clusters in a low density universe. Our approach allows us to explicitly seperate the contributions from gravitational collapse and changes in the core entropy of the intracluster gas. Here, we apply the model to determine whether a preferred value of Ω0 is selected by currently available constraints (Figure 1). Measurements of the X-ray evolution of clusters cannot, by themselves, select out a particular cosmological model. An additional constraint on the effective power spectrum index (n) is required. This can either come from a measurement of the large-scale galaxy correlation function or from the shape of the present-day temperature function. A theoretical calculation of the Ω0 dependence of the power spectrum does not help break the inherent degeneracy.

Type
IV. Structure Formation and Dark Matter
Copyright
Copyright © Kluwer 1999