Gaussianisation for fast and accurate inference from cosmological data

TL;DR

This paper introduces a method to transform complex non-Gaussian cosmological posteriors into Gaussian forms, enabling efficient analysis, accurate evidence computation, and better data combination, outperforming existing density estimation techniques.

Contribution

The paper presents a novel Gaussianisation technique using non-linear transformations for cosmological posteriors, facilitating analytical reconstruction and evidence calculation from MCMC samples.

Findings

Outperforms kernel density estimates in Gaussianisation quality.

Successfully reproduces non-Gaussian features in Planck data posteriors.

Accurately computes model evidence, aligning with other methods.

Abstract

We present a method to transform multivariate unimodal non-Gaussian posterior probability densities into approximately Gaussian ones via non-linear mappings, such as Box--Cox transformations and generalisations thereof. This permits an analytical reconstruction of the posterior from a point sample, like a Markov chain, and simplifies the subsequent joint analysis with other experiments. This way, a multivariate posterior density can be reported efficiently, by compressing the information contained in MCMC samples. Further, the model evidence integral (i.e. the marginal likelihood) can be computed analytically. This method is analogous to the search for normal parameters in the cosmic microwave background, but is more general. The search for the optimally Gaussianising transformation is performed computationally through a maximum-likelihood formalism; its quality can be judged by how well the credible regions of the posterior are reproduced. We demonstrate that our method outperforms kernel density estimates in this objective. Further, we select marginal posterior samples from Planck data with several distinct strongly non-Gaussian features, and verify the reproduction of the marginal contours. To demonstrate evidence computation, we Gaussianise the joint distribution of data from weak lensing and baryon acoustic oscillations (BAO), for different cosmological models, and find a preference for flat $\Lambda$CDM. Comparing to values computed with the Savage-Dickey density ratio, and Population Monte Carlo, we find good agreement of our method within the spread of the other two.