Reducing Noise in Cosmological N-body Simulations with Neutrinos

Abstract

We present a new method for generating initial conditions for numerical cosmological simulations in which massive neutrinos are treated as an extra set of N-body (collisionless) particles. It allows us to accurately follow the density field for both Cold Dark Matter (CDM) and neutrinos at both high and low redshifts. At high redshifts, the new method is able to reduce the shot noise in the neutrino power spectrum by a factor of more than $10^7$ compared to previous methods, where the power spectrum was dominated by shot noise at all scales. We find that our new approach also helps to reduce the noise on the total matter power spectrum on large scales, whereas on small scales the results agree with previous simulations. Our new method also allows for a systematic study of clustering of the low velocity tail of the distribution function of neutrinos. This method also allows for the study of the evolution of the overall velocity distribution as a function of the environment determined by the CDM field.

To be submitted to JCAP

References in corpus (18)

• Observation of electron-antineutrino disappearance at Daya Bay
• The DESI Experiment Part I: Science,Targeting, and Survey Design
• Massive neutrinos and cosmology
• Measurement of Neutrino Oscillation by the K2K Experiment
• Impact of massive neutrinos on nonlinear matter power spectrum
• The Mira-Titan Universe II: Matter Power Spectrum Emulation
• Constraint on neutrino masses from SDSS-III/BOSS Ly$\alpha$ forest and other cosmological probes
• The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Signs of neutrino mass in current cosmological datasets
• Simulating nonlinear cosmological structure formation with massive neutrinos
• Massive Neutrinos in Cosmology: Analytic Solutions and Fluid Approximation
• DEMNUni: ISW, Rees-Sciama, and weak-lensing in the presence of massive neutrinos
• Relativistic N-body simulations with massive neutrinos
• The halo model in a massive neutrino cosmology
• Scale-dependent bias and bispectrum in neutrino separate universe simulations
• An exact general remeshing scheme applied to physically conservative voxelization
• Precision reconstruction of the dark matter-neutrino relative velocity from N-body simulations
• The Effective Field Theory of Large-Scale Structure in the presence of Massive Neutrinos
• The kinematic Sunyaev-Zel'dovich effect of the large-scale structure (I): dependence on neutrino mass

Cited by in corpus (43)

• The Quijote simulations
• Neutrino Mass Ordering from Oscillations and Beyond: 2018 Status and Future Prospects
• Large-scale dark matter simulations
• Euclid preparation: IX. EuclidEmulator2 -- Power spectrum emulation with massive neutrinos and self-consistent dark energy perturbations
• Constraining $M_{\nu }$ with the Bispectrum II: The Total Information Content of the Galaxy Bispectrum
• Detecting Neutrino Mass by Combining Matter Clustering, Halos, and Voids
• An Efficient and Accurate Hybrid Method for Simulating Non-Linear Neutrino Structure
• An optimal nonlinear method for simulating relic neutrinos
• Cosmology with galaxy-galaxy lensing on non-perturbative scales: Emulation method and application to BOSS LOWZ
• $\nu \mathrm{CO}N\mathrm{CEPT}$: Cosmological neutrino simulations from the non-linear Boltzmann hierarchy
• A Lagrangian Perturbation Theory in the presence of massive neutrinos
• Fully relativistic treatment of light neutrinos in $N$-body simulations
• Tree-Level Bispectrum in the Effective Field Theory of Large-Scale Structure extended to Massive Neutrinos
• Aemulus $\nu$: Precise Predictions for Matter and Biased Tracer Power Spectra in the Presence of Neutrinos
• A fast particle-mesh simulation of non-linear cosmological structure formation with massive neutrinos
• Clustering in Massive Neutrino Cosmologies via Eulerian Perturbation Theory
• Beware of Fake $\nu$s: The Effect of Massive Neutrinos on the Nonlinear Evolution of Cosmic Structure
• A new approach to cosmological structure formation with massive neutrinos
• Euclid: Modelling massive neutrinos in cosmology -- a code comparison
• One line to run them all: SuperEasy massive neutrino linear response in $N$-body simulations
• Spoon or slide? The non-linear matter power spectrum in the presence of massive neutrinos
• Fast simulations of cosmic large-scale structure with massive neutrinos
• The cosmic neutrino background as a collection of fluids in large-scale structure simulations
• Cosmological Vlasov-Poisson Simulations of Structure Formation with Relic Neutrinos: Nonlinear Clustering and the Neutrino Mass
• Finding closure: approximating Vlasov-Poisson using finitely generated cumulants
• Geodesic motion and phase-space evolution of massive neutrinos
• Measuring dark matter-neutrino relative velocity on cosmological scales
• Momentum space sampling of neutrinos in $N$-body simulations
• Signatures of Light Massive Relics on nonlinear structure formation
• Relativistic Corrections to the Growth of Structure in Modified Gravity
• A Minimal Model for Massive Neutrinos in Newtonian N-body Simulations
• Hybrid multi-fluid-particle simulations of the cosmic neutrino background
• Improving initialization and evolution accuracy of cosmological neutrino simulations
• Significance of void shape: Neutrino mass from Voronoi void halos?
• Quantum algorithm for the Vlasov simulation of the large-scale structure formation with massive neutrinos
• Massive $\nu$s through the CNN lens: interpreting the field-level neutrino mass information in weak lensing
• Neutrinos in N-body simulations
• Measuring neutrino mass and asymmetry with matter pairwise velocities
• Including relativistic and primordial Non-Gaussianity contributions in cosmological simulations by modifying the initial condition
• The Power of the Cosmic Web
• Enhanced Small-Scale Structure in the Cosmic Dark Ages
• Slow neutrinos: non-linearity and momentum-space emulation
• A 400 Trillion-Grid Vlasov Simulation on Fugaku Supercomputer: Large-Scale Distribution of Cosmic Relic Neutrinos in a Six-dimensional Phase Space