Probing primordial non-Gaussianity with large - scale structure

By R. Scoccimarro, E. Sefusatti, M. Zaldarriaga. 2003

178 citations recorded by the source corpus.

We consider primordial non-Gaussianity due to quadratic corrections in the gravitational potential parametrized by a nonlinear coupling parameter ${f}_{\mathrm{NL}}.$ We study constraints on ${f}_{\mathrm{NL}}$ from measurements of the galaxy bispectrum in redshift surveys. Using estimates for idealized survey geometries of the 2dF and SDSS surveys and realistic ones from SDSS mock catalogs, we show that it is possible to probe $|{f}_{\mathrm{NL}}|\ensuremath{\simeq}100,$ after marginalization over bias parameters. We apply our methods to the galaxy bispectrum measured from the PSCz survey, and obtain a $2\ensuremath{\sigma}$ constraint $|{f}_{\mathrm{NL}}|\ensuremath{\lesssim}1800.$ We estimate that an all sky redshift survey up to $z\ensuremath{\simeq}1$ can probe $|{f}_{\mathrm{NL}}|\ensuremath{\simeq}1.$ We also consider the use of cluster abundance to constrain ${f}_{\mathrm{NL}}$ and find that in order to be sensitive to $|{f}_{\mathrm{NL}}|\ensuremath{\simeq}100,$ cluster masses need to be determined with an accuracy of a few percent, assuming perfect knowledge of the mass function and cosmological parameters.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c2fb2d76241658638d83e39f0213c8041a9b5e06

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In Astronomy and Astrophysics

1. L. Senatore
2. M. Zaldarriaga
3. Xingang Chen
4. D. Baumann
5. Uros Seljak
6. D. Green
7. E. Komatsu
8. E. Sefusatti

Citations in the corpus

• Primordial non-Gaussianity from the large-scale structure (2010, background): “For general triangles, moreover, it approximately retains this simple behavior, with a dependence on triangle shape through F2(k1, k2) [12].”
• Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, methodology): “The issue of bispectrum covariance has been studied in (Scoccimarro, 2000a; Scoccimarro et al., 2004; Sefusatti et al., 2006; Sefusatti & Scoccimarro, 2005).”
• Single-field consistency relations of large scale structure part II: resummation and redshift space (2013, background): “The signal to noise calculation closely follows the standard calculation for the case of primordial nonGaussianities (see for example [19]).”
• 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): “…constrains on the strength 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,…”
• Testing Inflation with Large Scale Structure: Connecting Hopes with Reality (2014, background): “Based on idealized survey geometry assumptions and ignoring the redshift evolution, [118] estimate that an all-sky redshift survey with n̄ ∼ 3×10−3 (h/Mpc)3 up to z ∼ 1 will probe σ(f loc NL) ∼ 1.”
• Prospects for cosmological collider physics (2016, background): “The Fisher matrix is (see for example [52, 53])”
• Effects of scale-dependent non-Gaussianity on cosmological structures (2007, unknown): “Contents”
• 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).”
• PRIMORDIAL NON-GAUSSIANITY, SCALE-DEPENDENT BIAS, AND THE BISPECTRUM OF GALAXIES (2009, unknown): “Specifically, they calculate the bispectrum of the three-dimensional distribution of galaxies, Bg(k1, k2, k3), 1 on large scales as (see also Scoccimarro et al. (2004)) Bg(k1, k2, k3, z) =3b31fNLΩmH 2 0 [ Pm(k1, z) k21T (k1) Pm(k2, z) k22T (k2) k23T (k3) D(z) + (2 cyclic) ] +2b31 [ F (s) 2 (k1,…”
• The bispectrum of galaxies from high-redshift galaxy surveys: Primordial non-Gaussianity and non-linear galaxy bias (2007, methodology): “Also, the same function is defined in Scoccimarro et al. (2004) in terms of the gravitational potential (i.e., the 0-0 component of the metric perturbations) during radiation domination, so that M(k; a) = − 9 10 MSSZ(k; a) leading to a different definition of the non-Gaussian parameter, fNL = − 10…”
• On the statistics of biased tracers in the Effective Field Theory of Large Scale Structures (2015, unknown): “[29, 28, 31, 30]): [ ∆B(k1, k2, θ) ]2 = s123 Lbox ntriangles P (hh) NL (k1)P (xx) NL (k2)P (yy) NL (k3) , (61)”
• The shape of non-Gaussianities (2004, background): “These non-Gaussianities are not scale invariant, a fact that can be used to separate them from the primordial contributions [23].”