The N5K Challenge: Non-Limber Integration for LSST Cosmology

TL;DR

This paper evaluates non-Limber integration methods for calculating the angular power spectrum in LSST cosmology, comparing their accuracy and speed to improve theoretical predictions for large-scale structure analysis.

Contribution

It benchmarks three non-Limber integration approaches, identifying the fastest accurate method and discussing their suitability for LSST cosmological parameter inference.

Findings

FKEM (CosmoLike) is the fastest accurate method for LSST Year 10 3x2pt analysis.

Second-order Limber approximation is sufficient for scales $\, ext{ell}=200-1000$ in LSST analysis.

First-order Limber approximation is inadequate for the specified scales and data.

Abstract

The rapidly increasing statistical power of cosmological imaging surveys requires us to reassess the regime of validity for various approximations that accelerate the calculation of relevant theoretical predictions. In this paper, we present the results of the 'N5K non-Limber integration challenge', the goal of which was to quantify the performance of different approaches to calculating the angular power spectrum of galaxy number counts and cosmic shear data without invoking the so-called 'Limber approximation', in the context of the Rubin Observatory Legacy Survey of Space and Time (LSST). We quantify the performance, in terms of accuracy and speed, of three non-Limber implementations: ${\tt FKEM (CosmoLike)}$, ${\tt Levin}$, and ${\tt matter}$, themselves based on different integration schemes and approximations. We find that in the challenge's fiducial 3x2pt LSST Year 10 scenario, ${\tt FKEM (CosmoLike)}$ produces the fastest run time within the required accuracy by a considerable margin, positioning it favourably for use in Bayesian parameter inference. This method, however, requires further development and testing to extend its use to certain analysis scenarios, particularly those involving a scale-dependent growth rate. For this and other reasons discussed herein, alternative approaches such as ${\tt matter}$ and ${\tt Levin}$ may be necessary for a full exploration of parameter space. We also find that the usual first-order Limber approximation is insufficiently accurate for LSST Year 10 3x2pt analysis on $\ell=200-1000$, whereas invoking the second-order Limber approximation on these scales (with a full non-Limber method at smaller $\ell$) does suffice.