Impact of cosmological signatures in two-point statistics beyond the linear regime

Abstract

Some beyond $\Lambda$CDM cosmological models have dark-sector energy densities that suffer phase transitions. Fluctuations entering the horizon during such a transition can receive enhancements that ultimately show up as a distinctive bump in the power spectrum relative to a model with no phase transition. In this work, we study the non-linear evolution of such signatures in the matter power spectrum and correlation function using N-body simulations, perturbation theory and HMcode - a halo-model based method. We focus on modelling the response, computed as the ratio of statistics between a model containing a bump and one without it, rather than in the statistics themselves. Instead of working with a specific theoretical model, we inject a parametric family of Gaussian bumps into otherwise standard $\Lambda$CDM spectra. We find that even when the primordial bump is located at linear scales, non-linearities tend to produce a second bump at smaller scales. This effect is understood within the halo model due to a more efficient halo formation. In redshift space these nonlinear signatures are partially erased because of the damping along the line-of-sight direction produced by non-coherent motions of particles at small scales. In configuration space, the bump modulates the correlation function reflecting as oscillations in the response, as it is clear in linear Eulerian theory; however, they become damped because large scale coherent flows have some tendency to occupy regions more depleted of particles. This mechanism is explained within Lagrangian Perturbation Theory and well captured by our simulations.

arXiv comment15 pages, 8 figures

References in corpus (71)

• The cosmological simulation code GADGET-2
• Dynamics of dark energy
• Exploring the Expansion History of the Universe
• Accelerating Universes with Scaling Dark Matter
• Stable clustering, the halo model and nonlinear cosmological power spectra
• Halo Models of Large Scale Structure
• Large-Scale Structure of the Universe and Cosmological Perturbation Theory
• Essentials of k-essence
• Cosmological Tracking Solutions
• The Sixteenth Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra
• Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing
• Tensions between the Early and the Late Universe
• Revising the Halofit Model for the Nonlinear Matter Power Spectrum
• Analytic model for galaxy and dark matter clustering
• Early Dark Energy Can Resolve The Hubble Tension
• Halo occupation numbers and galaxy bias
• Cosmological Non-Linearities as an Effective Fluid
• Redshift-Space Distortions, Pairwise Velocities and Nonlinearities
• Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data
• An accurate halo model for fitting non-linear cosmological power spectra and baryonic feedback models
• Baryon Acoustic Oscillations in 2D: Modeling Redshift-space Power Spectrum from Perturbation Theory
• Dark Energy Anisotropic Stress and Large Scale Structure Formation
• HMcode-2020: Improved modelling of non-linear cosmological power spectra with baryonic feedback
• nbodykit: an open-source, massively parallel toolkit for large-scale structure
• Accurate halo-model matter power spectra with dark energy, massive neutrinos and modified gravitational forces
• The Scale Dependence of Halo and Galaxy Bias: Effects in Real Space
• Convolution Lagrangian perturbation theory for biased tracers
• Equivalence Principle and the Baryon Acoustic Peak
• The Coyote Universe III: Simulation Suite and Precision Emulator for the Nonlinear Matter Power Spectrum
• A Lagrangian effective field theory
• Nonlinear Cosmological Power Spectra in Real and Redshift--Space
• General Scalar Fields as Quintessence
• The Mira-Titan Universe II: Matter Power Spectrum Emulation
• On the road to percent accuracy: nonlinear reaction of the matter power spectrum to dark energy and modified gravity
• Measuring the Speed of Dark: Detecting Dark Energy Perturbations
• What can Cosmology tell us about Gravity? Constraining Horndeski with Sigma and Mu
• Limits on Dark Radiation, Early Dark Energy, and Relativistic Degrees of Freedom
• Analytic model for the matter power spectrum, its covariance matrix, and baryonic effects
• A marked correlation function for constraining modified gravity models
• Non-linear Structure Formation in Cosmologies with Early Dark Energy
• A hydrodynamical halo model for weak-lensing cross correlations
• Structure formation in inhomogeneous Early Dark Energy models
• Clustering and Halo Abundances in Early Dark Energy Cosmological Models
• The impact of Early Dark Energy on non-linear structure formation
• Phenomenology of dark energy: general features of large-scale perturbations
• Lagrangian or Eulerian; Real or Fourier? Not All Approaches to Large-Scale Structure Are Created Equal
• Clipping the Cosmos: The Bias and Bispectrum of Large Scale Structure
• Halo Zeldovich model and perturbation theory: dark matter power spectrum and correlation function
• Shifting the Universe: Early Dark Energy and Standard Rulers
• Perturbation theory approach for the power spectrum: from dark matter in real space to massive haloes in redshift space
• Variable sound speed in interacting dark energy models
• Can Early Dark Energy be Detected in Non-Linear Structure?
• Spherical collapse, formation hysteresis and the deeply non-linear cosmological power spectrum
• Quintessence Restrictions on Negative Power and Condensate Potentials
• On the road to percent accuracy III: non-linear reaction of the matter power spectrum to massive neutrinos
• The Effective Halo Model: Creating a Physical and Accurate Model of the Matter Power Spectrum and Cluster Counts
• Extending the Coyote emulator to dark energy models with standard $w_0$-$w_a$ parametrization of the equation of state
• Nonlinear evolution of initially biased tracers in modified gravity
• CMB Constraints on a Baryonic Dark Matter-Dominated Universe
• Semi-analytic galaxy formation in early dark energy cosmologies
• Fine Features in the Primordial Power Spectrum
• Effects of local features of the inflaton potential on the spectrum and bispectrum of primordial perturbations
• Constraining the baryon fraction in the Warm Hot Intergalactic Medium at low redshifts with PLANCK data
• Imprint of a Steep Equation of State in the growth of structure
• Testing the nature of Dark Energy with Precision Cosmological constraints
• Bound Dark Energy: towards understanding the nature of the Dark Energy
• Non-linear Structure Formation for Dark Energy Models with a Steep Equation of State
• Effects of Dark Energy anisotropic stress on the matter power spectrum
• Analytic Fluid Approximation for Warm Dark Matter
• Lagrangian Perturbation Theory : Exact One-Loop Power Spectrum in General Dark Energy Models
• Dark matter candidate induced by Horndeski theory: dark matter halo and cosmological evolution

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