Resumming cosmic perturbations

By S. Matarrese, M. Pietroni. 2007

184 citations recorded by the source corpus.

Renormalization group (RG) techniques have been successfully employed in quantum field theory and statistical physics. Here we apply RG methods to study the non-linear stages of structure formation in the universe. Exact equations for the power spectrum, the bispectrum, and all higher order correlation functions can be derived for any underlying cosmological model. A remarkable feature of the RG flow is the emergence of an intrinsic UV cut-off, due to dark matter velocity dispersion, which improves the convergence of the equations at small scales. As a consequence, the method is able to follow the non-linear evolution of the power spectrum down to zero redshift and to length scales where perturbation theory fails. Our predictions accurately fit the results of N-body simulations in reproducing the ‘baryon acoustic oscillation’ features of the power spectrum, which will be accurately measured in future galaxy surveys and will provide a probe for distinguishing among different dark energy models.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/06845475ef5d45e302faf8de0c44f904db80d84e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. L. Senatore
2. M. Zaldarriaga
3. D. Baumann
4. D. Green
5. E. Pajer
6. Uros Seljak
7. Xingang Chen
8. M. White

In Statistical and Nonlinear Physics

1. L. Senatore
2. Uros Seljak
3. E. Sefusatti
4. E. Pajer
5. Martín Crocce
6. V. Desjacques
7. E. Shellard
8. J. Fergusson

Citations in the corpus

• Primordial non-Gaussianity from the large-scale structure (2010, background): “Extensions of the renormalization group description of dark matter clustering [68] to non-Gaussian initial density and velocity perturbations can improve the agreement up to wavenumbers k .”
• Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, background): “…R T H E MO D E L F O R TH E S H A P E O F ξ (r) In recent years, substantial progress has been made in understanding the non-linear gravitational evolution of density fluctuations (Crocce & Scoccimarro 2006a, 2008; Matarrese & Pietroni 2007; Matsubara 2008; Pietroni 2008; Taruya & Hiramatsu 2008).”
• The effective field theory of cosmological large scale structures (2012, background): “An incomplete sample of these works is given by [5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20, 21, 22, 23, 24, 25].”
• Cosmological non-linearities as an effective fluid (2010, background): “Our work builds on a long history of studies in non-linear perturbation theory [23, 24, 25, 26, 27, 28, 29, 30, 31, 2], numerical simulations [32, 33, 34, 35], and effective field theory [5, 6, 8, 37].”
• Flowing with time: a new approach to non-linear cosmological perturbations (2008, methodology): “0 dη′eη ′ gad(k , η, η )gbe(−q , η, η)gcf(q − k , η, η′) × [γdgh(k, −q, q − k)Peg(q , η)Pfh(q − k , η′) + γegh(−q, q − k, k)Pfg(q − k , η)Pdh(k , η′) +γfgh(q − k, k, −q)Pdg(k , η)Peh(q , η′)] , (14) where gab(k , η, η ′) is the linear propagator [22, 23, 13, 14] which gives the η-evolution of the fi”
• The Phenomenology of Right Handed Neutrinos (2013, unknown): “[313–319]).”
• A Closure Theory for Nonlinear Evolution of Cosmological Power Spectra (2007, methodology): “Very recently, there appear several works on the statistical treatment going beyond the perturbation theory (Valageas 2004; Crocce & Scoccimarro 2006a,b; McDonald 2007; Valageas 2007a; Matarrese & Pietroni 2007; Izumi & Soda 2007).”
• Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, methodology): “A step in the direction of improved predictions is offered by the promising results of the Renormalized Perturbation Theory [173–175] and of the Renormalization Group approach [176, 177].”
• Multipoint propagators in cosmological gravitational instability (2008, methodology): “[28] An alternative approach has been advocated in [11] based on a Renormalization Group Theory like approach.”
• Testing Inflation with Large Scale Structure: Connecting Hopes with Reality (2014, methodology): “the quasi-linear scale, where aforementioned PT can be applied, is quite limited. Various techniques to improve upon the PT are suggested: Renormalization group approach [168], Resumming perturbation [169], Renormalized Perturbation 23 Theory [170{172], Closure theory [173], Lagrangian perturbation ”