Non-Gaussian initial conditions in cosmological N-body simulations - II. Cold Dark Matter models

Moscardini, L.; Matarrese, S.; Lucchin, F.; Messina, A.

doi:10.1093/mnras/248.3.424

Cited by 67 publications

(85 citation statements)

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“…The non-Gaussian statistics considered here are those adopted by Moscardini et al (1991), namely the Lognormal (hereafter LN ) and the Chi-squared with one degree of freedom (hereafter χ 2 ), chosen as distributions for the peculiar gravitational potential, Φ(x), before the modulation by the CDM transfer function. These distributions actually split in two different types of models: the positive (LNp and χ 2 p ) and negative (LNn and χ 2 n ) models, according to whether the sign of the skewness for linear mass fluctuations, δ 3 M , is positive or negative respectively.…”

Section: Skewed Cdm Models and N-body Simulationsmentioning

confidence: 99%

“…The non-linear transformations from w to ϕ is ϕ(x) ∝ e w(x) and ϕ(x) ∝ w 2 (x) for LN and χ 2 respectively (Coles & Barrow 1987;Coles & Jones 1991;Moscardini et al 1991).…”

Section: Skewed Cdm Models and N-body Simulationsmentioning

confidence: 99%

“…The velocity field of NGCDM models has not received as detailed a study as its Gaussian counterpart; a preliminary analysis was done by Moscardini et al (1991). For this reason, before comparing the observed cosmic velocity field with the prediction of our models, we would like to briefly discuss the role of primordial density skewness on velocity field statistics.…”

Section: General Properties Of Velocity Fieldsmentioning

confidence: 99%

“…Klypin et al 1993, and references therein), iii) CDM models with a relic cosmological constant (e.g. Efstathiou, Bond & White 1992, and references therein), iv) non-Gaussian CDM models (hereafter NGCDM; Moscardini et al 1991;Messina et al 1992).…”

Section: Introductionmentioning

confidence: 99%

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Velocity fields in non-Gaussian cold dark matter models

Lucchin¹,

Matarrese²,

Messina³

et al. 1995

Monthly Notices of the Royal Astronomical Society

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We analyse the large-scale velocity field obtained by N-body simulations of cold dark matter (CDM) models with non-Gaussian primordial density fluctuations, considering models with both positive and negative primordial skewness in the density fluctuation distribution. We study the velocity probability distribution and calculate the dependence of the bulk flow, one-point velocity dispersion and Cosmic Mach Number on the filtering size. We find that the sign of the primordial skewness of the density field provides poor discriminatory power on the evolved velocity field. All non-Gaussian models here considered tend to have lower velocity dispersion and bulk flow than the standard Gaussian CDM model, while the Cosmic Mach Number turns out to be a poor statistic in characterizing the models. Next, we compare the large-scale velocity field of a composite sample of optically selected galaxies as described by the Local Group properties, bulk flow, velocity correlation function and Cosmic Mach Number, with the velocity field of mock catalogues extracted from the N-body simulations. The comparison does not clearly permit to single out a best model: the standard Gaussian model is however marginally preferred by the maximum likelihood analysis.

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Section: Skewed Cdm Models and N-body Simulationsmentioning

confidence: 99%

“…The non-linear transformations from w to ϕ is ϕ(x) ∝ e w(x) and ϕ(x) ∝ w 2 (x) for LN and χ 2 respectively (Coles & Barrow 1987;Coles & Jones 1991;Moscardini et al 1991).…”

Section: Skewed Cdm Models and N-body Simulationsmentioning

confidence: 99%

Section: General Properties Of Velocity Fieldsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Velocity fields in non-Gaussian cold dark matter models

Lucchin¹,

Matarrese²,

Messina³

et al. 1995

Monthly Notices of the Royal Astronomical Society

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“…Models of this type were originally proposed by Coles & Barrow (1987) in connection with the statistics of CMB anisotropies in the large-angle (SachsWolfe) limit. Moscardini et al (1991) considered various models belonging to this class as initial conditions for Nbody simulations of large-scale structure formation in a cold dark matter (CDM) cosmology. Falk, Rangarajan, & Srednicki (1993) showed that perturbations produced during inflation in single-field models are characterized by a low non-Gaussianity level, which can be parameterized as (e.g., Wang & Kamionkowski 2000)…”

Section: Introductionmentioning

confidence: 99%

High‐Resolution Simulations of Non‐Gaussian Cosmic Microwave Background Maps in Spherical Coordinates

Liguori

Matarrese

Moscardini

2003

ApJ

Self Cite

113

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We describe a new numerical algorithm for obtaining high-resolution simulated maps of the cosmic microwave background (CMB) for a broad class of non-Gaussian models. The kind of non-Gaussianity we account for is based on the simple idea that the primordial gravitational potential is obtained by a nonlinear but local mapping from an underlying Gaussian random field, as results from a variety of inflationary models. Our technique, which is based on a direct realization of the potential in spherical coordinates and fully accounts for the radiation transfer function, allows us to simulate non-Gaussian CMB maps down to the Planck resolution (l max $ 3000) with reasonable memory storage and computational time.

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pairs, groups and clusters of galaxies; 9.3.5 Superclusters and large-scale structure

Biermann¹

Interstellar Matter, Galaxy, Universe

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Non-Gaussian initial conditions in cosmological N-body simulations - II. Cold Dark Matter models

Cited by 67 publications

References 0 publications

Velocity fields in non-Gaussian cold dark matter models

Velocity fields in non-Gaussian cold dark matter models

High‐Resolution Simulations of Non‐Gaussian Cosmic Microwave Background Maps in Spherical Coordinates

pairs, groups and clusters of galaxies; 9.3.5 Superclusters and large-scale structure

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