Improving initialization and evolution accuracy of cosmological neutrino simulations

TL;DR

This paper improves the accuracy and efficiency of cosmological neutrino simulations by implementing a new sampling strategy, artifact removal techniques, and a refined initial conditions method, leading to better modeling of neutrino effects in large-scale structure.

Contribution

It introduces a modified neutrino sampling strategy, artifact removal via Fourier filtering, and an improved backscaling method for initial conditions in neutrino cosmology simulations.

Findings

The new sampling strategy induces ~1% artifacts on small scales.

Fourier-space filtering effectively removes these artifacts.

The improved backscaling method achieves sub-percent accuracy in matter growth predictions.

Abstract

Neutrino mass constraints are a primary focus of current and future large-scale structure (LSS) surveys. Non-linear LSS models rely heavily on cosmological simulations -- the impact of massive neutrinos should therefore be included in these simulations in a realistic, computationally tractable, and controlled manner. A recent proposal to reduce the related computational cost employs a symmetric neutrino momentum sampling strategy in the initial conditions. We implement a modified version of this strategy into the Hardware/Hybrid Accelerated Cosmology Code (HACC) and perform convergence tests on its internal parameters. We illustrate that this method can impart $\mathcal{O}(1\%)$ numerical artifacts on the total matter field on small scales, similar to previous findings, and present a method to remove these artifacts using Fourier-space filtering of the neutrino density field. Moreover, we show that the converged neutrino power spectrum does not follow linear theory predictions on relatively large scales at early times at the $15\%$ level, prompting a more careful study of systematics in particle-based neutrino simulations. We also present an improved method for backscaling linear transfer functions for initial conditions in massive neutrino cosmologies that is based on achieving the same relative neutrino growth as computed with Boltzmann solvers. Our self-consistent backscaling method yields sub-percent accuracy in the total matter growth function. Comparisons for the non-linear power spectrum with the Mira-Titan emulator at a neutrino mass of $m_{\nu}=0.15~\mathrm{eV}$ are in very good agreement with the expected level of errors in the emulator and in the direct N-body simulation.