Model independent approach towards measuring expansion and growth factor from next generation galaxy clustering and lensing angular power spectrum

TL;DR

This paper develops a model-independent method to measure the universe's expansion and growth factors using galaxy clustering and lensing data, demonstrating high-precision constraints with future surveys.

Contribution

It introduces a parametrization approach for the matter power spectrum components, enabling model-independent constraints from 3x2pt analysis on linear and non-linear scales.

Findings

High precision (percent level) constraints on the expansion factor E(z)

Order of magnitude improvement in growth factor G(z) constraints with non-linear scales

Combining multiple surveys enhances the constraints significantly

Abstract

In this work we perform Fisher forecasts on the expansion and the growth factors following model independent approaches from 3x2pt joint analysis of the galaxy lensing, clustering, and their cross-correlated spectra at the linear, and extending as well to non linear scales. For that, instead of choosing a specific model for the matter power spectrum, the main ingredient of these probes, we express it by parametrizing its components, such as the expansion and the growth factor, and those of the standard halo model and excursion set theory in several z bins, besides to the different bias and non-linear bias modelling functions. We apply the technique to Euclid, Rubin and SKA public specifications in the range 0.2 < z < 1.8 and show that one can then obtain model-independent constraints of the expansion E(z i ) and the growth factor G(z i ). We also show the change in gain in precision at each z- shell when going from pessimistic cut at linear scales to more optimistic non-linear settings, or the difference between using each survey alone or a combination of all of them, or the impact from fixing or adding more degrees of freedom in the non-linear modeling. We found that, in the most agnostic case, one can still reach high precision on E(z i ) in the order of the percent level when combining the three surveys at once while the growth factor G(z i ) has for the same settings one order of magnitude weaker constraints. We also found for both factors, an improvement that can reach one order of magnitude in precision when passing from linear to non-linear scales. We conclude that we will be able to constrain the two important factors of the background evolution and structure formation of the Universe when using non linear scales and the combined power of future surveys even in the most agnostic approaches.