Imprints of primordial non-Gaussianities on large-scale structure: Scale-dependent bias and abundance of virialized objects

By N. Dalal, O. Dor'e, D. Huterer, A. Shirokov. 2007

714 citations recorded by the source corpus.

We study the effect of primordial non-Gaussianity on large-scale structure, focusing upon the most massive virialized objects. Using analytic arguments and N-body simulations, we calculate the mass function and clustering of dark matter halos across a range of redshifts and levels of non-Gaussianity. We propose a simple fitting function for the mass function valid across the entire range of our simulations. We find pronounced effects of non-Gaussianity on the clustering of dark matter halos, leading to strongly scale-dependent bias. This suggests that the large-scale clustering of rare objects may provide a sensitive probe of primordial non-Gaussianity. We very roughly estimate that upcoming surveys can constrain non-Gaussianity at the level of |f{sub NL}| < or approx. 10, which is competitive with forecasted constraints from the microwave background.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f50dd73575d2bdd0d0776bdae08b59de0d57ad95

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Citations in the corpus

MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, background): “In addition, it also depends on the assembly history of the halos (Dalal et al. 2008).”
Scale-dependent bias induced by local non-Gaussianity: a comparison to N-body simulations (2008, methodology): “While we confirm the basic c© 0000 RAS, MNRAS 000, 1–13 effect reported in Dalal et al. (2008), we emphasize the importance of including a scale-independent term ∆bI and, to a lesser extent, a contribution induced by the matter power spectrum b(M)βm, to the scale-dependent shift ∆bκ when comparing…”
A SUNYAEV–ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS IN THE 2500 deg2 SOUTH POLE TELESCOPE SURVEY (2011, methodology): “The likelihood calculation was implemented as in V10, with the effect of fNL on cluster abundance added following the prescription of Dalal et al. (2008).”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, methodology): “See section 2.1 in Sefusatti et al. (2007) for an brief overview of previous work andAfshordi & Tolley (2008); Dalal et al. (2008); Desjacques et al. (2009); Fedeli et al. (2009); Grossi et al. (2009); Lam & Sheth (2009); Lo Verde et al. (2008); Maggiore & Riotto (2009); Oguri (2009); Pillepich et…”
Cosmology with Phase 1 of the Square Kilometre Array Red Book 2018: Technical specifications and performance forecasts (2018, neutral): “In particular, PNG of the local type fNL introduces a scale-dependent correction to clustering bias (Dalal et al. 2008; Matarrese & Verde 2008) such that bHI ∝ fNL/k2.”
Observational probes of cosmic acceleration (2012, background): “A final caveat related to the halo mass function is that primordial non-Gaussianity could alter its form (e.g., Weinberg and Cole, 1992; Dalal et al., 2008; Grossi et al., 2009; LoVerde and Smith, 2011; D’Amico et al., 2011) and thereby change the cluster abundances predicted for a given dark…”
Formation of Galaxy Clusters (2012, background): “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…”
The clustering of the SDSS main galaxy sample – II. Mock galaxy catalogues and a measurement of the growth of structure from redshift space distortions at z = 0.15 (2014, background): “…the comoving clustering pattern was encoded in the early Universe and thus depends on the physical energy densities (e.g. Peebles & Yu 1970; Sunyaev & Zel’dovich 1970; Doroshkevich, Zel’dovich & Sunyaev 1978), while the bias on large scales encodes primordial non-Gaussianity (Dalal et al. 2008).”