The three-point function as a probe of models for large-scale structure

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Fermi National Accelerator Laboratory, National Aeronautics and Space Administration, National Technical Information Service, distributor , [Batavia, Ill.], [Washington, DC, Springfield, Va
Galaxies -- Problems, exercises,
Other titlesThree point function as a probe of models for large-scale structure.
StatementJoshua A. Frieman & Enrique Gaztanaga.
SeriesNASA contractor report -- NASA CR-193249., FERMILAB-pub -- 93/140-A., Fermilab pub -- 93/140-A.
ContributionsGaztanaga, Enrique., United States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL15378855M

We show that higher-order galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where the galaxy power arises from scale-dependent bias: a bias with rapid scale-dependence leads to a dramatic decrease of the hierarchical amplitudes at large by: We show that higher-order (n-point) galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where The three-point function as a probe of models for large-scale structure book galaxy power arises from scale-dependent bias: a bias with rapid scale dependence leads to a dramatic decrease of the hierarchical amplitudes Q_J_ at large scales, r >~ R_p_.

We show that higher-order (n-point) galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where the galaxy power arises from scale-dependent bias: a bias with rapid scale-dependence leads to a dramatic decrease of the hierarchical amplitudes QJ at large scales, r> Rp.

It is shown that higher-order (n-point) galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where the galaxy power arises from scale-dependent bias: a bias with rapid scale-dependence leads to a dramatic decrease of the hierarchical amplitudes Q J at large scales, r is approximately greater than R p.

Get this from a library. The three-point function as a probe of models for large-scale structure. [Joshua A Frieman; Enrique Gaztanaga; United States. National Aeronautics and Space Administration.].

The three-point function as a probe of models for large-scale structure: Author(eng) Gaztanaga, Enrique; Frieman, Joshua A. Author Affiliation(eng) NASA Headquarters: Issue Date: Language: eng: Description: We analyze the consequences of models of structure formation for higher order (n-point) galaxy correlation functions in the Cited by: We show that higher-order (n-point) galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where the galaxy power arises from scale-dependent bias: a bias with rapid scale-dependence leads to a dramatic decrease of the hierarchical amplitudes QJ at large scales, r> : Joshua A.

Frieman and Enrique Gaztañaga. The Three-point Function as a Probe of Models for Large-scale Structure By Joshua A. Frieman and Enrique Gaztanaga No static citation data No static citation data CiteAuthor: Joshua A.

Frieman and Enrique Gaztanaga. The three-point function as a probe of models for large-scale structure By Joshua A Frieman and E Gaztañaga No static citation data No static citation data CiteAuthor: Joshua A Frieman and E Gaztañaga.

We show that higher-order (n-point) galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where the galaxy power arises from scale-dependent bias: a bias with rapid scale dependence leads to a dramatic decrease of the the hierarchical amplitudes Q(sub J) at large scales, r is greater than or Author: Joshua A.

Frieman and Enrique Gaztanaga. Title: The three-point function as a probe of models for large-scale structure Authors: Frieman, J. & Gaztanaga, E. Journal: Astrophysical Journal, Part 1 (ISSN X), vol.no.

2, p. Bibliographic Code: ApJ F. Complete bibliographic record. Three-dimensional (3D) coupled Burgers' equations are used as an adhesive model for the large scale structure formation in the universe [10].

Under a special set of initial and boundary conditions. The large-scale structure of the Universe The Lyman α forest as a probe of large-scale structure. Baryon acoustic oscillations signature in the three-point angular correlation function Cited by: Many models of inflation predict oscillatory features in the bispectrum of primordial fluctuations.

Since it has been shown that primordial non-Gaussianity can lead to a scale-dependent halo bias, we investigate the effect of oscillations in the three-point function on the clustering of dark-matter halos.

The large-scale structure of the Universe Volker Springel 1, Carlos S. Frenk 2 & Simon D. White 1 Research over the past 25 years has led to the view that the rich tapestry of present-day cosmic structureCited by: Key words: cosmology: theory — gravitational lensing — large-scale st ructure of universe 1 INTRODUCTION The gravitational lensing of distant galaxy images due to large-scale structure, known as cosmic shear, has been well established as a cosmological probe (e.g, MellierBartelmann & Schneider and Wittman for reviews).

Abstract: Many models of inflation predict oscillatory features in the bispectrum of primordial fluctuations.

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Since it has been shown that primordial non-Gaussianity can lead to a scale-dependent halo bias, we investigate the effect of oscillations in the three-point function on the clustering of dark-matter by: 9.

non-Gaussianities using the information contained in the large-scale structure of the Universe. During the next decade, several galaxy surveys, as DESI [35], LSST [36] and Euclid [37], will probe a large volume of our Universe, providing an unprecedented amount of new by: 6.

In a detailed analysis of the three-point correlation function (3PCF) for the 2dF Galaxy Redshift Survey (2dFGRS), we have accurately measured the 3PCF for galaxies of different luminosities. The 3PCF amplitudes [Q red (s,u,v) or Q proj (r p,u,v)] of the galaxies generally decrease with increasing triangle size and increase with the shape parameter v, in qualitative agreement with the Cited by: dial correlation functions in addition to reviewing the techniques one can employ to probe observations.

Description The three-point function as a probe of models for large-scale structure PDF

These observations include cosmic microwave background anisotropies and spectral distortions as well as the matter two and three point functions as inferred from large-scale structure and potentially, 21 cm surveys.

Contents by:   Abstract. Cosmic microwave background and large-scale structure data will shortly improve dramatically with the Microwave Anisotropy Probe and Planck Surveyor, and the Anglo-Australian 2-Degree Field and Sloan Digital Sky is therefore timely to ask which of the microwave background and large-scale structure will provide a better probe of primordial non Cited by: We report results for the angular three-point galaxy correlation function in the APM Galaxy Survey and compare them with theoretical expectations.

For the first time, these measurements extend to sufficiently large scales to probe the weakly nonlinear regime. The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies, by Slepian, Z., Eisenstein, et al., MNRAS,() 7.

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: higher order correlations revealed by germ-grain Minkowski functionals, by Wiegand, A., Eisenstein, D. J., MNRAS. The three-point correlation function of cosmological fluctuations is a sensitive probe of the physics of inflation.

We calculate the bispectrum, B g (k 1, k 2, k 3), Fourier transform of the three-point function of density peaks (e.g., galaxies), using two different methods: the Matarrese-Lucchin-Bonometto formula and the locality of galaxy bias.

Many inflation models predict that primordial density perturbations have a nonzero three-point correlation function, or bispectrum in Fourier space.

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Of the several possibilities for this bispectrum, the most common is the local-model bispectrum, which can be described as a spatial modulation of the small-scale (large-wavenumber) power spectrum by long-wavelength density by: Binding Site Configurations Probe Structure and Dynamics of the Zinc-finger NEMO Article in Biochemistry 56(4) December with 30 Reads How we measure 'reads'.

Get this from a library. The large-scale structure of the universe. [P J E Peebles] -- Opinions on the large-scale structure of the early universe range widely from primeval chaos to a well-ordered mass distribution.

P.J.E. Peebles argues that the evolution proceeded from a nearly. Figure 1 strikingly illustrates how well this standard model can fit nearby structure.

as a probe of large-scale structure. in the three-point angular correlation function from the SDSS. Tamara M. Davis's 55 research works with 3, citations and 2, reads, including: Cosmology with Phase 1 of the Square Kilometre Array Red Book Technical specifications and performance.

The three-point correlation function (3PCF) of the spin-2 fields, cosmic shear and microwave background polarization, is a statistical measure of non-Gaussian signals. At each vertex of a triangle, the shear field has two independent components.

journal article: three-point phase correlations: a new measure of nonlinear large-scale structure.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. Subject headings: large-scale structure of universe; methods: numerical; methods: statistical – 2 –.We place limits on inflationary models; for example, a minimally-coupled ¡£ ¢ 4 is disfavored at more 3- ¤ than using WMAP data in combination with smaller scale CMB and large scale structure.