The statistics of peaks of Gaussian random fields

Bardeen, John; Bond, J. R.; Kaiser, Nick; Szalay, Alexander S.

doi:10.1086/164143

Cited by 3,224 publications

(4,266 citation statements)

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“…As the primordial NG generates a cross-talk between short and long wavelengths, it alters significantly the local bias and introduces a strong scale dependence in it [25]. The same result can be also obtained through the peak-background split theory [26] where the underlying idea behind the generation of a local bias is that galaxies tend to form in regions where the dark matter density field is larger than some threshold value in Lagrangian space.…”

Section: Jcap04(2011)011supporting

confidence: 55%

Relativistic effects and primordial non-Gaussianity in the galaxy bias

Bartolo¹,

Matarrese²,

Riotto³

2011

J. Cosmol. Astropart. Phys.

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When dealing with observables, one needs to generalize the bias relation between the observed galaxy fluctuation field to the underlying matter distribution in a gauge-invariant way. We provide such relation at second-order in perturbation theory adopting the local Eulerian bias model and starting from the observationally motivated uniform-redshift gauge. Our computation includes the presence of primordial non-Gaussianity. We show that large scale-dependent relativistic effects in the Eulerian bias arise independently from the presence of some primordial non-Gaussianity. Furthermore, the Eulerian bias inherits from the primordial non-Gaussianity not only a scale-dependence, but also a modulation with the angle of observation when sources with different biases are correlated.

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Section: Jcap04(2011)011supporting

confidence: 55%

Relativistic effects and primordial non-Gaussianity in the galaxy bias

Bartolo¹,

Matarrese²,

Riotto³

2011

J. Cosmol. Astropart. Phys.

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“…In order to fix properly the initial conditions, we use the transfer function presented in references [51,49]. This transfer function assumes a scale invariant primordial spectrum, and determines the spectrum today considering the Universe composed of dark matter and a cosmological constant that generates the actual accelerated expansion phase.…”

Section: Power Spectrum and Transfer Functionmentioning

confidence: 99%

Density perturbations for a running cosmological constant

Fabris

Shapiro

Solà

2007

J. Cosmol. Astropart. Phys.

152

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The dynamics of density and metric perturbations is investigated for the previously developed model where the decay of the vacuum energy into matter (or vice versa) is due to the renormalization group (RG) running of the cosmological constant (CC) term. The evolution of the CC depends on the single parameter ν, which characterizes the running of the CC produced by the quantum effects of matter fields of the unknown high energy theory below the Planck scale. The sign of ν indicates whether bosons or fermions dominate in the running. The spectrum of perturbations is computed assuming an adiabatic regime and an isotropic stress tensor. Moreover, the perturbations of the CC term are generated from the simplest covariant form suggested by the RG model under consideration. The corresponding numerical analysis shows that for ν > 0 there is a depletion of the matter power spectrum at low scales (large wave numbers) as compared to the standard ΛCDM model, whereas for ν < 0 there is an excess of power at low scales. We find that the LSS data rule out the range |ν| > 10 −4 while the values |ν| ≤ 10 −6 look perfectly acceptable. For ν < 0 the excess of power at low scales grows rapidly and the bound is more severe. From the particle physics viewpoint, the values |ν| ≃ 10 −6 correspond to the "desert" in the mass spectrum above the GUT scale M X ∼ 10 16 GeV . Our results are consistent with those obtained in other dynamical models admitting an interaction between dark matter and dark energy. We find that the matter power spectrum analysis is a highly efficient method to discover a possible scale dependence of the vacuum energy.

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“…4 The collapse factor is defined as f = x/xm (see Del Popolo 2009, Appendix A) 5 The density profile of a proto-halo is taken to be the profile of a peak in a density field described by the Bardeen et al (1986) power spectrum, as is illustrated in Del Popolo (2009), Figure 6. Unauthenticated Download Date | 5/11/18 6:20 PM dynamical friction and angular momentum.…”

Section: Structure Formation Modelmentioning

confidence: 99%

Angular Momentum in Dwarf Galaxies

Popolo

2014

Open Astronomy

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Abstract. We study the "angular momentum catastrophe" in the framework of interaction among baryons and dark matter through dynamical friction. By means of Del Popolo (2009) model we simulate 14 galaxies similar to those investigated by van den Bosch, Burkert and Swaters (2001), and calculate the distribution of their spin parameters and the angular momenta. Our model gives the angular momentum distribution which is in agreement with the van den Bosch et al. observations. Our result shows that the "angular momentum catastrophe" can be naturally solved in a model that takes into account the baryonic physics and the exchange of energy and angular momentum between the baryonic clumps and dark matter through dynamical friction.

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The statistics of peaks of Gaussian random fields

Cited by 3,224 publications

References 0 publications

Relativistic effects and primordial non-Gaussianity in the galaxy bias

Relativistic effects and primordial non-Gaussianity in the galaxy bias

Density perturbations for a running cosmological constant

Angular Momentum in Dwarf Galaxies

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