The bispectrum of galaxies from high-redshift galaxy surveys: Primordial non-Gaussianity and non-linear galaxy bias

By E. Sefusatti, E. Komatsu. 2007

213 citations recorded by the source corpus.

The greatest challenge in the interpretation of galaxy clustering data from any surveys is galaxy bias. Using a simple Fisher matrix analysis, we show that the bispectrum provides an excellent determination of linear and non-linear bias parameters of intermediate and high-z galaxies, when all measurable triangle configurations down to mildly non-linear scales, where perturbation theory is still valid, are included. The bispectrum is also a powerful probe of primordial non-Gaussianity. The planned galaxy surveys at z {approx}> 2 should yield constraints on non-Gaussian parameters, f{sub NL}{sup loc.} and f{sub NL}{sup eq.}, that are comparable to, or even better than, those from CMB experiments. We study how these constraints improve with volume, redshift range, as well as the number density of galaxies. Finally we show that a halo occupation distribution may be used to improve these constraints further by lifting degeneracies between gravity, bias, and primordial non-Gaussianity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8dce6678763941d84acc884ff637362f827b06e8

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, methodology): “From Sefusatti & Komatsu (2007). with ∆B2g given by (IV.180).”
PRIMORDIAL NON-GAUSSIANITY, SCALE-DEPENDENT BIAS, AND THE BISPECTRUM OF GALAXIES (2009, methodology): “The new terms that we have derived in this paper, the BnG f2 NL and BnGgNL terms, are even more important than the term derived by Sefusatti & Komatsu (2007), BnG0fNL , This property makes high-redshift galaxy surveys particularly a powerful probe of primordial non-Gaussianity.”
The Effective Field Theory of Large Scale Structures at two loops (2013, methodology): “onal [28] kind, assuming a cosmic variance limited experiment and assuming the same scaling as in the linear regime, go as k 3=2 max . Preliminary forecasts for these parameters for the Euclid survey [29], using k max ’0:1 hMpc equal1 at redshift z= 0, give constraints of order f ;ortho NL ˘10, whic”
Effects of scale-dependent non-Gaussianity on cosmological structures (2007, unknown): “Contents”
Neutrino Physics from the Cosmic Microwave Background and Large-Scale Structure (2013, background): “erived from the power spectrum. Constraining these correlation functions is especially important for equilateral and orthogonal type non-Gaussianity, which cannot be tested through the power spectrum [92]. While we do not have a reliable code to project non-Gaussianity constraints in this way, it is”
The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity (2012, background): “Primordial non-Gaussianity can also be measured from the bispectrum of cosmic microwave background (CMB) anisotropies (see, e.g., Bartolo et al. 2004; Komatsu 2010 and references therein) and, in principle, galaxies (see e.g. Sefusatti & Komatsu 2007; Scoccimarro et al. 2012).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies (2016, background): “…of the primordial non-Gaussian signal, for example through fNL (Gangui et al. 1994; Fry & Scherrer 1994; Verde et al. 2000; Scoccimarro et al. 2004; Sefusatti & Komatsu 2007; Sefusatti 2009; Sefusatti et al. 2010, 2012; Scoccimarro et al. 2012; Tellarini et al. 2015, 2016; Welling et al. 2016).”
Large-scale bias and efficient generation of initial conditions for nonlocal primordial non-Gaussianity (2011, background): “[25] E.”
Primordial non-Gaussianity from the large-scale structure (2010, methodology): “In the original derivation of [169], the large scale (unfiltered) galaxy bispectrum in the f loc NL model is given by Bh(k1,k2,k3) = b 3 1B0(k1,k2,k3) + b 2 1b2 [”
Constraining primordial non-Gaussianity with future galaxy surveys (2011, unknown): “Moreover, in full analogy with the CMB case, any 3-point statistic of the galaxy distribution is affected by PNG (Sefusatti & Komatsu 2007; Jeong & Komatsu 2009).”
Approaches to understanding cosmic acceleration (2009, background): “In principle, the bias parameters can be determined from higher order correlation functions [219, 220, 221].”
Halo mass function and scale-dependent bias from N-body simulations with non-Gaussian initial conditions (2008, background): “The galaxy bispectrum is thus sensitive to f NL only at high redshift (Verde et al. 2000; Scoccimarro, Sefusatti & Zaldarriaga 2004; Sefusatti & Komatsu 2007).”
Scale-dependent bias induced by local non-Gaussianity: a comparison to N-body simulations (2008, background): “However, recent work has mostly focused on higher order statistics such as the bispectrum (Scoccimarro et al. 2004; Sefusatti & Komatsu 2007).”