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Chinese Journal of Astronomy and Astrophysics
, 2000
"... Abstract The power spectrum estimator based on the Discrete Wavelet Transformation (DWT) is applied to detect the clustering power in the IRAS Point Source Catalog Redshift Survey (PSCz). Comparison with mock samples extracted from Nbody simulation shows that the DWT power spectrum estimator could ..."
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could provide a robust measurement of banded fluctuation power over a range of wavenumbers 0.1 ∼ 2.0hMpc−1. We have fitted three typical CDM models (SCDM, τCDM and ΛCDM) using the PeacockDodds formula including nonlinear evolution and redshift distortion. We find that, our results are in good
Stable clustering, the halo model and nonlinear cosmological power spectra
 MNRAS
, 2003
"... We present the results of a large library of cosmological Nbody simulations, using powerlaw initial spectra. The nonlinear evolution of the matter power spectra is compared with the predictions of existing analytic scaling formulae based on the work of Hamilton et al. The scaling approach has assu ..."
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Cited by 20 (0 self)
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matter haloes by continuing mergers. These effects are naturally included in the analytic ‘halo model ’ for nonlinear structure; we use this approach to fit both our scalefree results and also our previous CDM data. This method is more accurate than the commonlyused Peacock–Dodds formula and should
The Power Spectrum of the PSC Redshift Survey
"... We measure the redshiftspace power spectrum P (k) for the recently completed IRAS Point Source Catalogue (PSC) redshift survey, which contains 14500 galaxies over 84% of the sky with 60 micron flux 0:6 Jansky. Comparison with simulations shows that our estimated errors on P (k) are realistic, and ..."
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have fitted families of CDMlike models using the PeacockDodds formula for nonlinear evolution; the results are somewhat sensitive to the assumed smallscale velocity dispersion oe V . Assuming a realistic oe V 300 km s \Gamma1 yields a shape parameter \Gamma 0:25 and normalisation boe 8 0
NBody Simulations of Alternate Gravity Models
 Phys. Rev
, 2006
"... Theories in which gravity is weaker on cosmological scales have been proposed to explain the observed acceleration of the universe. The nonlinear regime in such theories is not well studied, though it is likely that observational tests of structure formation will lie in this regime. A class of alter ..."
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Cited by 3 (1 self)
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it easier to distinguish such models from general relativity using the threedimensional power spectrum probed by galaxy surveys and the weak lensing power spectrum. We find that gravitational evolution shows an approximate universality even for modified gravity – based on this, the PeacockDodds approach
A Fitting Formula for the NonLinear Evolution of the
, 2008
"... The largescale structure of the universe observed in galaxy surveys is thought to arise from the growth of primordial fluctuations due to gravitational instability. Making accurate ..."
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The largescale structure of the universe observed in galaxy surveys is thought to arise from the growth of primordial fluctuations due to gravitational instability. Making accurate
Universal fitting formulae for baryon oscillation surveys, MNRAS 365
, 2006
"... The next generation of galaxy surveys will attempt to measure the baryon oscillations in the clustering power spectrum with high accuracy. These oscillations encode a preferred scale which may be used as a standard ruler to constrain cosmological parameters and dark energy models. In this paper we p ..."
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present simple analytical fitting formulae for the accuracy with which the preferred scale may be determined in the tangential and radial directions by future spectroscopic and photometric galaxy redshift surveys. We express these accuracies as a function of survey parameters such as the central redshift
Y.: QuasiSelfSimilar Evolution of the TwoPoint Correlation Function: Strongly Nonlinear Regime
 in Ω0 < 1 Universes, The Astrophysical Journal 566
, 2002
"... The wellknown selfsimilar solution for the twopoint correlation function of the density field is valid only in an Einstein – de Sitter universe. We attempt to extend the solution for non – Einstein – de Sitter universes. For this purpose we introduce an idea of quasiselfsimilar evolution; this ..."
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The wellknown selfsimilar solution for the twopoint correlation function of the density field is valid only in an Einstein – de Sitter universe. We attempt to extend the solution for non – Einstein – de Sitter universes. For this purpose we introduce an idea of quasiselfsimilar evolution; this approach is based on the assumption that the evolution of the twopoint correlation is a succession of stages of evolution, each of which spans a short enough period to be considered approximately selfsimilar. In addition we assume that clustering is stable on scales where a physically motivated ‘virialization condition ’ is satisfied. These assumptions lead to a definite prediction for the behavior of the twopoint correlation function in the strongly nonlinear regime. We show that the prediction agrees well with Nbody simulations in non – Einstein – de Sitter cases, and discuss some remaining problems. Subject headings: cosmology: theory — largescale structure of universe — gravitation — methods: Nbody simulations 1.
Analytical Approximation to the Nonlinear Power Spectrum of Gravitational Clustering
, 1998
"... This paper presents an analytical formula that closely approximates the fully nonlinear power spectrum of matter fluctuations for redshift z ≈ 5 to 0 over a wide range of cosmologically interesting flat models with varying matter density Ωm and neutrino fraction Ων. The functional form is motivated ..."
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This paper presents an analytical formula that closely approximates the fully nonlinear power spectrum of matter fluctuations for redshift z ≈ 5 to 0 over a wide range of cosmologically interesting flat models with varying matter density Ωm and neutrino fraction Ων. The functional form is motivated
The 2dF Galaxy Redshift Survey: Powerspectrum analysis of the final dataset and cosmological implications
, 2004
"... We present a power spectrum analysis of the final 2dF Galaxy Redshift Survey, ..."
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We present a power spectrum analysis of the final 2dF Galaxy Redshift Survey,
Linear Power Spectra in Cold+Hot Dark Matter Models: Analytical Approximations and Applications
, 1996
"... This paper presents simple analytic approximations to the linear power spectra, linear growth rates, and rms mass fluctuations for both components in a family of cold+hot dark matter (CDM+HDM) models that are of current cosmological interest. The formulas are valid for a wide range of wavenumber, ne ..."
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) or n = 0.95 (with tensor mode) in Ων ∼ 0.1 − 0.2 CDM+HDM models gives a power spectrum similar to that of an open CDM model with a shape parameter Γ = 0.25, providing good agreement with the power spectrum reconstructed by Peacock and Dodds (1994) and the observed cluster abundance. Subject headings
Results 1  10
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