![]() To estimate the power spectra over a wide range of wavenumbers, we have used the method of Jenkins et al. At z = 0, the halo power spectrum is antibiased ( b P 120 km s -1. The halo power spectrum evolves much slower than the power spectrum of matter and has a different shape which indicates that the bias is time and scale dependent. ![]() We present accurate estimates of the evolution of the matter power spectrum probed deep into the stable clustering regime and find that its shape and evolution can be well described, with only a minor modification, by the fitting formula of Peacock & Dodds. In addition to the previous studies of the halo two-point correlation function, we consider the evolution of bias estimated using two different statistics: power spectrum b P and a direct correlation of smoothed halo and matter overdensity fields b. ![]() We present results from a study of bias and its evolution for galaxy-size halos in a large, high-resolution simulation of a low-density, cold dark matter model with a cosmological constant. Received 1998 December 17 accepted 1999 March 11 The Origin and Evolution of Halo Bias in Linear and Nonlinear RegimesĪstronomy Department, New Mexico State University, Box 30001, Department 4500, Las Cruces, NM 88003-0001 Kravtsov & Klypin, Halo Bias in Linear and Nonlinear Regimes
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