Efficient Construction of Mock Catalogs for Baryon Acoustic Oscillation Surveys

TL;DR

This paper presents a rapid, efficient method for generating high-fidelity mock catalogs for large-scale structure surveys, accurately reproducing key properties with significantly reduced computational cost.

Contribution

We introduce a derated N-body simulation scheme that accurately reproduces large-scale structure and halo properties while requiring four times less CPU time.

Findings

Halo masses recovered within 0.5% accuracy

Power spectrum matches within 1% up to k=1h/Mpc

Redshift spacing of 0.05 allows precise interpolation

Abstract

Precision measurements of the large scale structure of the Universe require large numbers of high fidelity mock catalogs to accurately assess, and account for, the presence of systematic effects. We introduce and test a scheme for generating mock catalogs rapidly using suitably derated N-body simulations. Our aim is to reproduce the large scale structure and the gross properties of dark matter halos with high accuracy, while sacrificing the details of the internal structure of the halos. By adjusting global and local time-steps in an N-body code, we demonstrate that we recover halo masses to better than 0.5% and the power spectrum to better than 1% both in real and redshift space for k = 1h/Mpc, while requiring a factor of 4 less CPU time. We also calibrate the redshift spacing of outputs required to generate simulated light cones. We find that outputs separated by every z = 0.05 allow us to interpolate particle positions and velocities to reproduce the real and redshift space power spectra to better than 1% (out to k = 1h/Mpc). We apply these ideas to generate a suite of simulations spanning a range of cosmologies, motivated by the Baryon Oscillation Spectroscopic Survey (BOSS) but broadly applicable to future large scale structure surveys including eBOSS and DESI. As an initial demonstration of the utility of such simulations, we calibrate the shift in the baryonic acoustic oscillation peak position as a function of galaxy bias with higher precision than has been possible so far. This paper also serves to document the simulations, which we make publicly available.