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For refcode 1997ApJ...485L..13C:
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1997ApJ...485L..13C The Average Mass Profile of Galaxy Clusters R. G. CARLBERG, H. K. C. YEE, E. ELLINGSON, S. L. MORRIS, R. ABRAHAM, P. GRAVEL, C. J. PRITCHET, T. SMECKER-HANE, F. D. A. HARTWICK, J. E. HESSER, J. B. HUTCHINGS, AND J. B. OKE Received 1997 March 17; accepted 1997 May 23 ABSTRACT The average mass density profile measured in the Canadian Network for Observational Cosmology cluster survey is well described with the analytic form {rho}(r) = Ar-1(r + a_{rho}_)^-2^, as advocated on the basis of n-body simulations by Navarro, Frenk, & White. The predicted core radii are a_{rho}_ = 0.20 (in units of the radius where the mean interior density is 200 times the critical density) for an {OMEGA} = 0.2 open cold dark matter model and a_{rho}_ = 0.26 for a flat {OMEGA} = 0.2 model, with little dependence on other cosmological parameters for simulations normalized to the observed cluster abundance. The dynamically derived local mass-to-light ratio, which has little radial variation, converts the observed light profile to a mass profile. We find that the scale radius of the mass distribution, 0.20 <= a_{rho}_ <= 0.30 (depending on modeling details, with a 95% confidence range of 0.12- 0.50), is completely consistent with the predicted values. Moreover, the profiles and total masses of the clusters as individuals can be acceptably predicted from the cluster rms line-of-sight velocity dispersion alone. This is strong support for the hierarchical clustering theory for the formation of galaxy clusters in a cool, collisionless, dark-matter-dominated universe. Subject headings: galaxies: clusters: general-large-scale structure of universe
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