Nonlinear structure formation in Bound Dark Energy

Abstract

We study nonlinear structure formation in the Bound Dark Energy model (BDE), where dark energy (DE) corresponds to a light scalar meson particle $\varphi$ dynamically formed at a condensation energy scale ${\Lambda }_c$. The evolution of this dark-energy meson is determined by the potential $V(\varphi )={\Lambda }_c^{4+2/3}{\varphi }^{-2/3}$, with a distinguishing phenomenology from other quintessence scenarios. Particularly, the expansion rate of the universe is affected not only at late times, but also when the condensation of $\varphi$ occurs, which in linear theory leads to an enhancement (with respect to standard $\Lambda$CDM) of matter perturbations on small scales. We study how much of this signature is still present at late times as well as the properties of dark matter halos in the nonlinear regime through N-body simulations. Our results show that nonlinear corrections wash out this feature from the matter power spectrum even before DE becomes dominant. There is, however, a small but clear suppression of the BDE spectrum of $2\%$ today on the largest scales due to the distinct late-time dynamics of DE. The differences on the clustering power between BDE and $\Lambda$CDM are reflected in the halo mass function, where small halos are more abundant in BDE as opposed to large heavy structures, whose formation is delayed because of the expansion history of the universe. This result is well captured by the semi-analytical Sheth-Tormen formula. However, despite these differences, the halo concentration parameter is essentially the same in both models, which suggest that clustering inside the halos decouple from the general expansion once the halos form.

arXiv commentAccepted version. Extended discussions in sections 2, 3.2 & 4.3. More references added

References in corpus (71)

• Planck 2015 results. XIII. Cosmological parameters
• A Universal Density Profile from Hierarchical Clustering
• Dynamics of dark energy
• Efficient Computation of CMB anisotropies in closed FRW models
• Modified Gravity and Cosmology
• Cosmological parameters from CMB and other data: a Monte-Carlo approach
• Cosmology and the Fate of Dilatation Symmetry
• The 6dF Galaxy Survey: Baryon Acoustic Oscillations and the Local Hubble Constant
• Dark energy cosmology: the equivalent description via different theoretical models and cosmography tests
• Profiles of dark haloes: evolution, scatter, and environment
• Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
• Halo Models of Large Scale Structure
• Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples
• The Clustering of the SDSS DR7 Main Galaxy Sample I: A 4 per cent Distance Measure at z=0.15
• Ellipsoidal collapse and an improved model for the number and spatial distribution of dark matter haloes
• Cosmological Perturbation Theory in the Synchronous vs. Conformal Newtonian Gauge
• Cosmological Perturbation Theory in the Synchronous and Conformal Newtonian Gauges
• Mass function of dark matter halos
• The Rockstar Phase-Space Temporal Halo Finder and the Velocity Offsets of Cluster Cores
• Observational Probes of Cosmic Acceleration
• Beyond the Cosmological Standard Model
• Cosmological Parameters from Observations of Galaxy Clusters
• Semi-Analytic Modelling of Galaxy Formation: The Local Universe
• Big Bang Nucleosynthesis: 2015
• Halos and galaxies in the standard cosmological model: results from the Bolshoi simulation
• Everything You Always Wanted To Know About The Cosmological Constant Problem (But Were Afraid To Ask)
• Quintessence: A Review
• Transients from Initial Conditions in Cosmological Simulations
• Halo concentrations in the standard LCDM cosmology
• Accurate universal models for the mass accretion histories and concentrations of dark matter halos
• How many cosmological parameters?
• A universal model for halo concentrations
• Cosmological constant and vacuum energy: old and new ideas
• Numerical study of halo concentrations in dark-energy cosmologies
• Dark energy two decades after: Observables, probes, consistency tests
• Probing dark energy perturbations: the dark energy equation of state and speed of sound as measured by WMAP
• Cosmic Structure Growth and Dark Energy
• PArthENoPE: Public Algorithm Evaluating the Nucleosynthesis of Primordial Elements
• Large Scale Cosmic Microwave Background Anisotropies and Dark Energy
• A new determination of the primordial He abundance using the HeI 10830A emission line: cosmological implications
• The mass of a halo
• The Redshift Evolution of LCDM Halo Parameters: Concentration, Spin, and Shape
• Simulating the Universe with MICE: The abundance of massive clusters
• Mass Function Predictions Beyond LCDM
• The Mass Power Spectrum in Quintessence Cosmological Models
• The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: BAO measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies
• The primordial helium abundance from updated emissivities
• Exhaustive Study of Cosmic Microwave Background Anisotropies in Quintessential Scenarios
• Cosmological structure formation in a homogeneous dark energy background
• Imprints of dark energy on cosmic structure formation: II) Non-Universality of the halo mass function
• Accurate estimators of power spectra in N-body simulations
• Halo properties in models with dynamical Dark Energy
• Spherical collapse model in dark energy cosmologies
• Imprints of Dark Energy on Cosmic Structure Formation I) Realistic Quintessence Models and the Non-Linear Matter Power Spectrum
• Modeling Dynamical Dark Energy
• The impact of Early Dark Energy on non-linear structure formation
• A robust deuterium abundance; Re-measurement of the z=3.256 absorption system towards the quasar PKS1937-1009
• How clustering dark energy affects matter perturbations
• Dynamical Dark Energy simulations: high accuracy Power Spectra at high redshift
• How well do we know the Halo Mass Function?
• The nonlinear matter power spectrum
• The primordial deuterium abundance at z = 2.504 from a high signal-to-noise spectrum of Q1009+2956
• Cluster mass functions in the quintessential Universe
• Natural Quintessence with Gauge Coupling Unification
• Quintessence Restrictions on Negative Power and Condensate Potentials
• Quintessence Unification Models from Non-Abelian Gauge Dynamics
• Non linear predictions from linear theories in models with Dark Energy
• Power Spectra to 1% Accuracy between Dynamical Dark Energy Cosmologies
• A Realistic Particle Physics Dark Energy Model
• Testing the nature of Dark Energy with Precision Cosmological constraints
• Bound Dark Energy: towards understanding the nature of the Dark Energy

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• Impact of a Rapid Diluted Energy Density on the halo mass function