Constraining equilateral-type primordial non-Gaussianities from imaging surveys

TL;DR

This paper assesses how future imaging surveys can constrain equilateral-type primordial non-Gaussianities, focusing on parameters related to the bispectrum and trispectrum, using Fisher analysis and theoretical modeling.

Contribution

It introduces a method to forecast constraints on primordial non-Gaussianity parameters from imaging surveys, including trispectrum effects, using integrated perturbation theory and Fisher analysis.

Findings

LSST can constrain f_NL^{equil} to 700 and g_NL^{( abla \sigma)^4} to 4.9×10^7.

Constraints are comparable to CMB limits but provide independent cross-checks.

Discusses potential improvements for tighter future constraints.

Abstract

We investigate expected constraints on equilateral-type primordial non-Gaussianities from future/ongoing imaging surveys, making use of the fact that they enhance the halo/galaxy bispectrum on large scales. As model parameters to be constrained, in addition to $f_{\rm NL}^{\rm equil}$, which is related to the primordial bispectrum, we consider $g_{\rm NL}^{(\partial \sigma)^4}$, which is related to the primordial trispectrum that appeared in the effective field theory of inflation. After calculating the angular bispectra of the halo/galaxy clustering and weak gravitational lensing based on the integrated perturbation theory, we perform Fisher matrix analysis for three representative surveys. We find that among the three surveys, the tightest constraints come from Large Synoptic Survey Telescope ; its expected $1\sigma$ errors on $f_{\rm NL}^{\rm equil}$ and $g_{\rm NL}^{(\partial \sigma)^4}$ are respectively given by $7.0 \times 10^2$ and $4.9 \times 10^7$. Although this constraint is somewhat looser than the one from the current cosmic microwave background observation, since we obtain it independently, we can use this constraint as a cross check. We also evaluate the uncertainty with our results caused by using several approximations and discuss the possibility to obtain tighter constraint on $f_{\rm NL}^{\rm equil}$ and $g_{\rm NL}^{(\partial \sigma)^4}$.