Three-Point Phase Correlations: A New Measure of Nonlinear Large-Scale Structure

Wolstenhulme, Stephen; Bonvin, Camille; Obreschkow, Danail

doi:10.1088/0004-637x/804/2/132

Cited by 28 publications

(41 citation statements)

References 57 publications

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“…They appear in thin chains that extend into voids and display a different line correlation than those galaxies residing in the larger filaments. Finally, in Wolstenhulme, Bonvin & Obreschkow (2014), the ILCF was computed using tree-level perturbation theory giving good agreement with direct estimates from N-body simulations. An analytic formula for l(r) allows it to be modelled properly and opens the door for measuring various cosmological parameters.…”

Section: Properties and Applicationsmentioning

confidence: 96%

“…In writing Eq. (2) we adopted the same conventions as employed in Wolstenhulme, Bonvin & Obreschkow (2014). The ILCF differs from the conventional three-point correlator of whitened density fields in two respects.…”

Section: Definitionmentioning

confidence: 99%

“…This PDF was computed perturbatively for mildly non-Gaussian fields by Matsubara (2003), showing that it is not solely related to the bispectrum but a progression of all higher order spectra such as the trispectrum etc. Taking this result, Wolstenhulme, Bonvin & Obreschkow (2014) showed that the ILCF can be expressed to lowest order as follows:…”

Section: Definitionmentioning

confidence: 99%

“…Recently, a new measure for phase information, the line correlation function, was introduced by Obreschkow et al (2013) as a spherically-averaged three-point correlation of phase factors. In the follow-up paper (Wolstenhulme, Bonvin & Obreschkow 2014) it was computed perturbatively and related to the bispectrum and power spectrum at leading order.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The anisotropic line correlation function as a probe of anisotropies in galaxy surveys

Eggemeier

Battefeld

Smith

et al. 2015

Mon. Not. R. Astron. Soc.

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We propose an anisotropic generalisation of the line correlation function (ALCF) to separate and quantify phase information in the large-scale structure of galaxies. The line correlation function probes the strictly non-linear regime of structure formation and since phase information drops out of the power spectrum, the line correlation function provides a complementary tool to commonly used techniques based on two-point statistics. Furthermore, it is independent of linear bias as well as the Gaussian variance on the modulus of the density field and thus may also prove to be advantageous compared to the bispectrum or similar higher-order statistics for certain cases. For future applications it is vital, though, to be able to account for observational effects that cause anisotropies in the distribution of galaxies. Based on a number of numerical studies, we find that our ALCF is well suited to accomplish this task and we demonstrate how the Alcock-Paczyński effect and kinematical redshift-space distortions can in principle be measured via the ALCF.

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Section: Properties and Applicationsmentioning

confidence: 96%

Section: Definitionmentioning

confidence: 99%

Section: Definitionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The anisotropic line correlation function as a probe of anisotropies in galaxy surveys

Eggemeier

Battefeld

Smith

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…Using a simplistic information analysis Obreschkow et al speculated that the LCF is a promising estimator, especially when probing alternative cosmological models. Moreover, because the LCF measures the three-point statistics of the Fourier phases, irrespective of amplitudes, it is independent of linear bias (Wolstenhulme et al 2015), the uncertainty of which plagues all LSS surveys. To study the effectiveness of the LCF in galaxy surveys, studied its correlation with the 2-point estimator on different scales.…”

Section: Introductionmentioning

confidence: 99%

Cosmological constraints from Fourier phase statistics

Ali

Obreschkow

Howlett

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Most statistical inference from cosmic large-scale structure relies on two-point statistics, i.e. on the galaxy-galaxy correlation function (2PCF) or the power spectrum. These statistics capture the full information encoded in the Fourier amplitudes of the galaxy density field but do not describe the Fourier phases of the field. Here, we quantify the information contained in the line correlation function (LCF), a three-point Fourier phase correlation function. Using cosmological simulations, we estimate the Fisher information (at redshift z = 0) of the 2PCF, LCF and their combination, regarding the cosmological parameters of the standard ΛCDM model, as well as a Warm Dark Matter (WDM) model and the f (R) and Symmetron modified gravity models. The galaxy bias is accounted for at the level of a linear bias. The relative information of the 2PCF and the LCF depends on the survey volume, sampling density (shot noise) and the bias uncertainty. For a volume of 1h −3 Gpc 3 , sampled with points of mean density n = 2 × 10 −3 h 3 Mpc −3 and a bias uncertainty of 13%, the LCF improves the parameter constraints by about 20% in the ΛCDM cosmology and potentially even more in alternative models. Finally, since a linear bias only affects the Fourier amplitudes (2PCF), but not the phases (LCF), the combination of the 2PCF and the LCF can be used to break the degeneracy between the linear bias and σ 8 , present in 2-point statistics.

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Consistency relations in effective field theory

Munshi

Regan

2017

J. Cosmol. Astropart. Phys.

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Abstract. The consistency relations in large scale structure relate the lower-order correlation functions with their higher-order counterparts. They are direct outcome of the underlying symmetries of a dynamical system and can be tested using data from future surveys such as Euclid. Using techniques from standard perturbation theory (SPT), previous studies of consistency relation have concentrated on continuity-momentum (Euler)-Poisson system of an ideal fluid. We investigate the consistency relations in effective field theory (EFT) which adjusts the SPT predictions to account for the departure from the ideal fluid description on small scales. We provide detailed results for the 3D density contrast δ as well as the scaled divergence of velocityθ. Assuming a ΛCDM background cosmology, we find the correction to SPT results becomes important at k 0.05h/Mpc and that the suppression from EFT to SPT results that scales as square of the wave number k, can reach 40% of the total at k ≈ 0.25h/Mpc at z = 0. We have also investigated whether effective field theory corrections to models of primordial non-Gaussianity can alter the squeezed limit behaviour, finding the results to be rather insensitive to these counterterms. In addition, we present the EFT corrections to the squeezed limit of the bispectrum in redshift space which may be of interest for tests of theories of modified gravity.

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Three-Point Phase Correlations: A New Measure of Nonlinear Large-Scale Structure

Cited by 28 publications

References 57 publications

The anisotropic line correlation function as a probe of anisotropies in galaxy surveys

The anisotropic line correlation function as a probe of anisotropies in galaxy surveys

Cosmological constraints from Fourier phase statistics

Consistency relations in effective field theory

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