Quintessential Isocurvature in Separate Universe Simulations

Abstract

In a universe with quintessence isocurvature, or perturbations in dark energy that are independent from the usual curvature perturbations, structure formation is changed qualitatively. The existence of two independent fields, curvature and isocurvature, causes the growth rate of matter perturbations to depend on their initial conditions. The quintessence perturbations cause their growth to depend on scale. We perform the first separate universe simulations for this cosmology. We demonstrate that the power spectrum response and the halo bias depend on scale and initial conditions and that the presence of the isocurvature mode changes the mapping from these quantities to the halo auto- and cross-power spectra, and the squeezed-limit bispectrum. We compare the bias to several models, finding reasonable agreement with both a power-spectrum-response model with one free parameter and a model that fits two independent bias parameters for curvature and isocurvature sourced fluctuations. We also verify that simulation responses to pure isocurvature and pure curvature modes can be linearly combined to reproduce responses with different ratios of isocurvature and curvature. This allows our results to be used to predict the halo power spectrum and stochasticity with arbitrary large-scale curvature and isocurvature power spectra. In an appendix, we study the generation of quintessence isocurvature during inflation and show that a modified kinetic term is typically required to produce observable isocurvature modes in a field with $w_Q\approx -1$.

arXiv comment21 pages, 8 figures

References in corpus (49)

• The cosmological simulation code GADGET-2
• Non-Gaussian features of primordial fluctuations in single field inflationary models
• The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation schemes
• A Dynamical Solution to the Problem of a Small Cosmological Constant and Late-time Cosmic Acceleration
• The Rockstar Phase-Space Temporal Halo Finder and the Velocity Offsets of Cluster Cores
• Generating the curvature perturbation without an inflaton
• Perturbations in k-inflation
• Adiabatic CMB perturbations in pre-big bang string cosmology
• Effects of Cosmological Moduli Fields on Cosmic Microwave Background
• Nongaussian Isocurvature Perturbations from Inflation
• Transients from Initial Conditions in Cosmological Simulations
• Single field consistency relation for the 3-point function
• A new mechanism for generating density perturbations from inflation
• Power Spectrum Super-Sample Covariance
• Toward a Measurement of the Cosmological Geometry at z~2: Predicting Lyman-alpha Forest Correlation in Three Dimensions, and the Potential of Future Data Sets
• Renormalized Halo Bias
• Cosmological Perturbations From Inhomogeneous Reheating, Freeze-Out, and Mass Domination
• Super-Sample Covariance in Simulations
• Perturbation Theory Reloaded: Analytical Calculation of Non-linearity in Baryonic Oscillations in the Real Space Matter Power Spectrum
• Initial conditions to cosmological N-body simulations, or how to run an ensemble of simulations
• Galaxy Bias and non-Linear Structure Formation in General Relativity
• Precision measurement of the local bias of dark matter halos
• A Low CMB Quadrupole from Dark Energy Isocurvature Perturbations
• Separating the Early Universe from the Late Universe: cosmological parameter estimation beyond the black box
• Modeling scale-dependent bias on the baryonic acoustic scale with the statistics of peaks of Gaussian random fields
• Separate Universe Simulations
• The Atacama Cosmology Telescope: a measurement of the primordial power spectrum
• Position-dependent power spectrum of the large-scale structure: a novel method to measure the squeezed-limit bispectrum
• Halo bias in mixed dark matter cosmologies
• Stochasticity of Bias and Nonlocality of Galaxy Formation: Linear Scales
• Super-Sample Signal
• On Separate Universes
• Implementing the DC Mode in Cosmological Simulations with Supercomoving Variables
• Scale-dependent bias and bispectrum in neutrino separate universe simulations
• Compensated Isocurvature Perturbations and the Cosmic Microwave Background
• Separate Universe Consistency Relation and Calibration of Halo Bias
• Linear response to long wavelength fluctuations using curvature simulations
• The Evolution of Bias - Generalized
• Scale-dependent halo bias from scale-dependent growth
• First detection of scale-dependent linear halo bias in $N$-body simulations with massive neutrinos
• The nonlinear matter power spectrum
• Local stochastic non-Gaussianity and N-body simulations
• Angular averaged consistency relations of large-scale structures
• Super-Sample CMB Lensing
• Can a spectator scalar field enhance inflationary tensor mode?
• Separating the Universe into the Real and Fake
• Halo assembly bias from Separate Universe simulations
• Quintessential Scale Dependence from Separate Universe Simulations
• On Dark Energy Isocurvature Perturbation

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• Large-scale dark matter simulations
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• The position-dependent matter density probability distribution function
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• Super-sample tidal modes on the celestial sphere
• Position-dependent Voronoi probability distribution functions for matter and halos
• Scale-dependent halo bias and the squeezed limit bispectrum in the presence of radiation
• Large-scale structure with superhorizon isocurvature dark energy