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3.2.4. Power Spectrum in Nonlinear Galaxy Clustering

Peacock (1997) argued that the power spectrum in a small scale region (k-1 < 3 h-1 Mpc), where nonlinear effect is dominant, shows more power than is expected in Omega = 1 cosmological models. He showed that the excess power is understood if the mass density is Omega approx 0.3.