Memory of initial conditions in gravitational clustering

By Martín Crocce, R. Scoccimarro. 2005

244 citations recorded by the source corpus.

We study the nonlinear propagator, a key ingredient in renormalized perturbation theory (RPT) that allows a well-controlled extension of perturbation theory into the nonlinear regime. We show that it can be thought as measuring the memory of density and velocity fields to their initial conditions. This provides a clean definition of the validity of linear theory, which is shown to be much more restricted than usually recognized in the literature. We calculate the nonlinear propagator in RPT and compare to measurements in numerical simulations, showing remarkable agreement well into the nonlinear regime. We also show that N-body simulations require a rather large volume to recover the correct propagator, due to the missing large-scale modes. Our results for the nonlinear propagator provide an essential element to compute the nonlinear power spectrum in RPT.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c1ba92927fa75b5e4ec713efab54e562a758e38f

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Citations in the corpus

A Closure Theory for Nonlinear Evolution of Cosmological Power Spectra (2007, methodology): “…with Ωw = 0 and f = 1, the analytical solution for linear propagator gab satisfying the evolution equation (58) is obtained and is given by (e.g., Crocce & Scoccimarro 2006a; Valageas 2007a): gab(η1, η2)= {eη1−η2 5 ( 32 32 ) + e−(3/2)(η1−η2) 5 ( 2 −2 −3 3 )} Θ(η1 − η2) (66) with Θ(x) being…”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, background): “A step in the direction of improved predictions is offered by the promising results of Renormalized Perturbation Theory (Bernardeau et al., 2008; Crocce & Scoccimarro, 2006a,b) and of the Renormalization Group approach (Matarrese & Pietroni, 2007; Pietroni, 2008).”
Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, methodology): “Furthermore, Smith et al. (2008) and Crocce & Scoccimarro (2008) have shown that both large volume numerical simulations and theoretical predictions based on renormalized perturbation theory (RPT) indicate that the BAO peak in the correlation function is shifted and distorted in a non-trivial manner”
Modelling the anisotropic two-point galaxy correlation function on small scales and single-probe measurements of H(z), DA(z) and f(z)σ8(z) from the Sloan Digital Sky Survey DR7 luminous red galaxies (2012, methodology): “…damping effect of the wiggled part in redshift space can be well approximated by (Eisenstein, Seo & White 2007) P nlBAO(k, μk) = P linBAO(k) exp ( − k 2 2k2∗ [ 1 + μ2k(2f + f 2) ]) , (2) where k could be computed by (Crocce & Scoccimarro 2006; Matsubara 2008) k∗ = [ 1 3π2 ∫ Plin(k) dk ]−1/2 .”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space (2016, background): “The leading contribution to the shift in the BAO scale results from the product of the first and second term (Crocce & Scoccimarro 2006; Sherwin & Zaldarriaga 2012).”
Bayesian physical reconstruction of initial conditions from large-scale structure surveys (2012, background): “Also note that unique recovery of initial conditions is generally not possible on all scales due to the chaotic nature of the dynamical large scale structure formation process on small scales (see e.g. Nusser & Dekel 1992; Crocce & Scoccimarro 2006).”
The bispectrum of galaxies from high-redshift galaxy surveys: Primordial non-Gaussianity and non-linear galaxy bias (2007, methodology): “New promising techniques such as a renormalized perturbation theory approach (Crocce & Scoccimarro 2006b,a, 2007; McDonald 2007; Matarrese & Pietroni 2007) may be used to obtain bet- 7 ter predictions for the power spectrum and bispectrum.”
Improved Forecasts for the Baryon Acoustic Oscillations and Cosmological Distance Scale (2007, background): “…ruler test is that the BAO signature is reduced with time by the nonlinear growth of density fields into present-day structures (Meiksin et al. 1999; Springel et al. 2005; Angulo et al. 2005; Seo & Eisenstein 2005; White 2005; Crocce & Scoccimarro 2006; Jeong & Komatsu 2006; Huff et al. 2007).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…from https://academ ic.oup.com /m nras/article-abstract/461/4/3781/2608598 by guest on 15 M arch 2020 where μk is the cosine of the angle between k and the LOS, f is the growth rate, and k is computed following Crocce & Scoccimarro (2006) and Matsubara (2008) by k = [ 1 3π2 ∫ Plin(k)dk ]−1/2 .”
Multipoint propagators in cosmological gravitational instability (2008, methodology): “It was shown in [4] that this decay can be computed exactly in the high-k limit, where a subset of diagrams is expected to provide the dominant contribution.”
The bispectrum in the Effective Field Theory of Large Scale Structure (2014, methodology): “[17–20]), we use already the time integrated kernels as vertices.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, methodology): “…we want to make use of the power spectrum beyond k = 0.10 h Mpc−1 we cannot rely on standard PT which seems to break down at low redshift for k > 0.10 h Mpc−1, where the 2-loop term turns out to be larger than the 1-loop term (Crocce & Scoccimarro 2006; Carlson et al. 2009; Taruya et al. 2009).”
Inflation and String Theory (2014, background): “Hence, while N ∝ `(2)max for the CMB, we have N LSS ∝ k(3) max for LSS (but see [159,160]), where kmax is associated with the smallest scale that is both measurable and under theoretical control.”