Non-Gaussian Shape Discrimination with Spectroscopic Galaxy Surveys

TL;DR

This paper explores how upcoming galaxy surveys can distinguish between different inflationary models by analyzing non-Gaussian bispectrum shapes through galaxy clustering data across various scales and redshifts.

Contribution

It introduces a detailed method for using galaxy clustering and halo bias to differentiate non-Gaussian bispectrum shapes beyond the squeezed limit, with forecasts for Euclid and DESI surveys.

Findings

ELG samples better probe divergent shapes in the squeezed limit.

LRG constraints are stronger for scale-independent bias shapes.

Combined LSS and CMB data can differentiate bispectra with similar large-scale properties.

Abstract

[Abridged] We consider how galaxy clustering data, from Mpc to Gpc scales, from upcoming large scale structure surveys, such as Euclid and DESI, can provide discriminating information about the bispectrum shape arising from a variety of inflationary scenarios. Through exploring in detail the weighting of shape properties in the calculation of the halo bias and halo mass function we show how they probe a broad range of configurations, beyond those in the squeezed limit, that can help distinguish between shapes with similar large scale bias behaviors. We assess the impact, on constraints for a diverse set of non-Gaussian shapes, of galaxy clustering information in the mildly non-linear regime, and surveys that span multiple redshifts and employ different galactic tracers of the dark matter distribution. Fisher forecasts are presented for a Euclid-like spectroscopic survey of H$\alpha$-selected emission line galaxies (ELGs) using recent revisions of the expected H$\alpha$ luminosity function, and a DESI-like survey, of luminous red galaxies (LRGs) and [O-II] doublet-selected ELGs, in combination with Planck-like CMB temperature and polarization data. While ELG samples provide better probes of shapes that are divergent in the squeezed limit, LRG constraints, centered below $z<1$, yield stronger constraints on shapes with scale-independent large-scale halo biases, such as the equilateral template. The ELG and LRG samples provide complementary degeneracy directions for distinguishing between different shapes. If the Gaussian galaxy bias is constrained to better than a percent level, such as can be determined from the galaxy bispectrum or weak lensing, then the LSS and CMB data could provide complementary constraints that will enable differentiation of bispectra with distinct theoretical origins but with similar large scale, squeezed-limit properties.