Cosmological Information in Perturbative Forward Modeling

TL;DR

This paper compares perturbative forward modeling with traditional methods for constraining cosmological parameters, showing it can be nearly optimal and suggesting new practical estimators for improved analysis.

Contribution

It demonstrates that perturbative forward modeling retains maximal information content and introduces new estimators that are easier to implement while nearly matching optimal constraints.

Findings

Field-level posterior can be computed analytically in perturbation theory.

Long-short wavelength interactions can degrade constraints in standard analyses.

New estimators inspired by perturbative posterior are nearly optimal and easier to use.

Abstract

We study how well perturbative forward modeling can constrain cosmological parameters compared to conventional analyses. We exploit the fact that in perturbation theory the field-level posterior can be computed analytically in the limit of small noise. In the idealized case where the only relevant parameter for the nonlinear evolution is the nonlinear scale, we argue that information content in this posterior is the same as in the $n$-point correlation functions computed at the same perturbative order. In the real universe other parameters can be important, and there are possibly enhanced effects due to nonlinear interactions of long and short wavelength fluctuations that can either degrade the signal or increase covariance matrices. We identify several different parameters that control these enhancements and show that for some shapes of the linear power spectrum they can be large. This leads to degradation of constraints in the standard analyses, even though the effects are not dramatic for a $\Lambda$CDM-like cosmology. The aforementioned long-short couplings do not affect the field-level inference which remains optimal. Finally, we show how in these examples calculation of the perturbative posterior motivates new estimators that are easier to implement in practice than the full forward modelling but lead to nearly optimal constraints on cosmological parameters.