Primordial non-Gaussianity: large-scale structure signature in the perturbative bias model

By P. Mcdonald. 2008

153 citations recorded by the source corpus.

I compute the effect on the power spectrum of tracers of the large-scale mass-density field (e.g., galaxies) of primordial non-Gaussianity of the form {phi}={phi}+f{sub NL}({phi}{sup 2}- )+g{sub NL}{phi}{sup 3}+..., where {phi} is proportional to the initial potential fluctuations and {phi} is a Gaussian field, using beyond-linear-order perturbation theory. I find that the need to eliminate large higher-order corrections necessitates the addition of a new term to the bias model, proportional to {phi}, i.e., {delta}{sub g}=b{sub {delta}}{delta}+b{sub {phi}}f{sub NL}{phi}+..., with all the consequences this implies for clustering statistics, e.g., P{sub gg}(k)=b{sub {delta}}{sup 2}P{sub {delta}}{sub {delta}}(k)+2b{sub {delta}}b{sub {phi}}f{sub NL}P{sub {phi}}{sub {delta}}(k)+b{sub {phi}}{sup 2}f{sub NL}{sup 2}P{sub {phi}}{sub {phi}}(k)+.... This result is consistent with calculations based on a model for dark matter halo clustering, showing that the form is quite general, not requiring assumptions about peaks, or the formation or existence of halos. The halo model plays the same role it does in the usual bias picture, giving a prediction for b{sub {phi}} for galaxies known to sit in a certain type of halo. Previous projections for future constraints based on this effect have been very conservative--there is enough volume at z < or approx. 2 to measure f{sub NL} to {approx}{+-}1, with muchmore » more volume at higher z. As a prelude to the bias calculation, I point out that the beyond-linear (in {phi}) corrections to the power spectrum of mass-density perturbations are naively infinite, so it is dangerous to assume they are negligible; however, the infinite part can be removed by a renormalization of the fluctuation amplitude, with the residual k-dependent corrections negligible for models allowed by current constraints.« less

Subfields: Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/c9231f4cfbdb605d75ae5dbf3b90daabc3391e3d

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Citations in the corpus

Halo mass function and scale-dependent bias from N-body simulations with non-Gaussian initial conditions (2008, methodology): “Similar calculations have been presented by Matarrese & Verde (2008), Slosar et al. (2008), Afshordi & Tolley (2008) and McDonald (2008).”
How to evade the sample variance limit on measurements of redshift-space distortions (2008, methodology): “renormalization of perturbation theory that local non-linear transformations of the density field can do nothing but change the bias parameters on large scales [22, 31, 32].”
Renormalized halo bias (2014, background): “To analyze this self-consistently, we must consider the effects of these non-Gaussian contributions on the renormalization of the biasing model [18, 19].”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, background): “[206], and, with a somehow different derivation, by McDonald [207].”
Large-scale non-Gaussian mass function and halo bias: tests on N-body simulations (2009, methodology): “Finally, Taruya, Koyama & Matsubara (2008) – see also McDonald (2008) – used a perturbation theory approach to consider at the same time non-linear bias, second-order gravitational evolution and non-Gaussianity.”
Formation of Galaxy Clusters (2012, result): “As was discovered by Dalal et al. (2008) and confirmed in subsequent analytical (Afshordi & Tolley 2008; Matarrese & Verde 2008; McDonald 2008; Slosaret al. 2008; Taruya, Koyama & Matsubara 2008) and numerical studies (Desjacques, S ljak & Iliev 2009; Grossi et al. 2009; Pillepich, Porciani & Hahn…”
Scale-dependent bias induced by local non-Gaussianity: a comparison to N-body simulations (2008, background): “Further work has confirmed the basic picture (Afshordi & Tolley 2008; McDonald 2008; Taruya et al. 2008).”
PRIMORDIAL NON-GAUSSIANITY, SCALE-DEPENDENT BIAS, AND THE BISPECTRUM OF GALAXIES (2009, background): “…in light of recent analytical (Dalal et al. 2008; Matarrese & Verde 2008; Slosar et al. 2008; Afshordi & Tolley 2008; Taruya et al. 2008; McDonald 2008) and numerical (Dalal et al. 2008; Desjacques et al. 2008; Pillepich et al. 2008; Grossi et al. 2009) studies of the effects of…”
DESI and other Dark Energy experiments in the era of neutrino mass measurements (2013, methodology): “We simply give the estimated constraining power for the main redshift surveys, based on the power spectrum, for the local model of non-Gaussianity, following [65, 145].”
Primordial non-Gaussianity from the large-scale structure (2010, methodology): “Using this approach, it can be shown that the halo power spectrum arising from the first-order terms of the local bias expansion can be cast into the form [158] Ph(k) = [ b1(M) + f loc NL bφ(k) ]2 PR(k).”