Non-Gaussian signatures from Gaussian initial fluctuations - Evolution of skewness and kurtosis from cosmological simulations in the highly nonlinear regime

Lahav, O.; Itoh, Makoto; Inagaki, Shogo; Suto, Yasushi

doi:10.1086/172143

Cited by 54 publications

(61 citation statements)

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“…for each of the simulations we added the z ‐component of the velocity, in units of the Hubble constant, to the z ‐component of the position before throwing the cells. These results confirm that redshift‐space distortions and variations in Ω m have a negligible impact upon the values of S 3 and S 4 that we calculate (Lahav et al 1993; Hivon et al 1995; Colombi et al 1996).…”

Section: Calculating the Momentssupporting

confidence: 88%

Higher order moments of the density field in a parametrized sequence of non-Gaussian theories

White

1999

Monthly Notices of the Royal Astronomical Society

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We calculate the higher order moments in a sequence of models where the initial density fluctuations are drawn from a distribution with a power‐law power spectrum. For large values of ν, the distribution is approximately Gaussian, and we reproduce the values known from perturbation theory. As ν is lowered the distribution becomes progressively more non‐Gaussian, approximating models with rare, high‐amplitude peaks. The limit ν=1 is a realization of recently proposed isocurvature models for producing early galaxy formation, where the density perturbations are quadratic in a Gaussian field.

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Section: Calculating the Momentssupporting

confidence: 88%

Higher order moments of the density field in a parametrized sequence of non-Gaussian theories

White

1999

Monthly Notices of the Royal Astronomical Society

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“…Fig. 5 shows that the scaling predicted by still holds in redshift space, a result originally found by Lahav et al (1993) and Hivon et al (1995) who showed that it holds even on smaller scales than those analysed here, that is, on domains where non‐linear effects become important. In an analogous way, Fig.…”

Section: Applying the Methodssupporting

confidence: 79%

Second-order matter fluctuations via higher order galaxy correlators

Bel

Marinoni

2012

Monthly Notices of the Royal Astronomical Society

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“…Note the similarity to the power spectrum results: at small scales the FOG effect maintains the redshift-space equilateral amplitude close to its perturbative value, while in real space the amplitude grows by a large factor. This result, or the analog of this result for the skewness S 3 (R) (i.e., the fact that S 3 in redshift space is less scale-dependent than in real space), has led previous authors to conclude that higher-order correlations are 'more hierarchical' in redshift-space than in real space (Lahav et al 1993;Matsubara 1994, Matsubara andSuto and Matsubara 1994;Bonometto et al 1995;Ghigna et al 1996). However, this interpretation is in fact not correct: the FOG effect at small scales decreases the equilateral amplitude with respect to the real space value and shifts power to the co-linear configurations.…”

Section: Comparison With Numerical Simulationsmentioning

confidence: 93%

The Bispectrum as a Signature of Gravitational Instability in Redshift Space

Scoccimarro¹,

Couchman

Frieman

1999

ApJ

283

434

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The bispectrum provides a characteristic signature of gravitational instability that can be used to probe the Gaussianity of the initial conditions and the bias of the galaxy distribution. We study how this signature is affected by redshift distortions using perturbation theory and highresolution numerical simulations. We obtain perturbative results for the multipole expansion of the redshift-space bispectrum which provide a natural way to break the degeneracy between bias and Ω present in measurements of the redshift-space power spectrum. We propose a phenomenological model that incorporates the perturbative results and also describes the bispectrum in the transition to the non-linear regime. We stress the importance of non-linear effects and show that inaccurate treatment of these can lead to significant discrepancies in the determination of bias from galaxy redshift surveys. At small scales we find that the bispectrum monopole exhibits a strong configuration dependence that reflects the velocity dispersion of clusters. Therefore, the hierarchical model for the three-point function does not hold in redshift-space.

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Non-Gaussian signatures from Gaussian initial fluctuations - Evolution of skewness and kurtosis from cosmological simulations in the highly nonlinear regime

Cited by 54 publications

References 0 publications

Higher order moments of the density field in a parametrized sequence of non-Gaussian theories

Higher order moments of the density field in a parametrized sequence of non-Gaussian theories

Second-order matter fluctuations via higher order galaxy correlators

The Bispectrum as a Signature of Gravitational Instability in Redshift Space

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