Scale-dependent bias induced by local non-Gaussianity: a comparison to N-body simulations

By V. Desjacques, Uros Seljak, Ilian Iliev. 2008

195 citations recorded by the source corpus.

We investigate the effect of primordial non-Gaussianity of the local fNL type on the auto- and cross-power spectra of dark matter haloes using simulations of the cold dark matter cosmology. We perform a series of large N-body simulations of both positive and negative fNL, spanning the range between 10 and 100. Theoretical models predict a scale-dependent bias correction b(k, fNL) that depends on the linear halo bias b(M). We measure the power spectra for a range of halo mass and redshifts covering the relevant range of existing galaxy and quasar populations. We show that auto- and cross-correlation analyses of bias are consistent with each other. We find that for low wavenumbers with k 1.5. We show that a scale-independent bias correction improves the comparison between theory and simulations on smaller scales, where the scale-dependent effect rapidly becomes negligible. The current limits on fNL from Slosar et al. come mostly from very large scales k < 0.01 h Mpc-1 and, therefore, remain valid. For the halo samples with b(M) < 1.5 - 2, we find that the scale-dependent bias from non-Gaussianity actually exceeds the theoretical predictions. Our results are consistent with the bias correction scaling linearly with fNL.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9753af401d28dfc83e08e9618587707515200f0b

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Citations in the corpus

The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity (2012, background): “Various studies (e.g., Desjacques et al. 2009; Wagner & Verde 2012; Scoccimarro et al. 2012) have shown that non-zero f localNL produces corrections to the scale-dependent and -independent halo bias that are more complicated functions of halo mass (and age) than the simple model we have presented…”
Primordial non-Gaussianity from the large-scale structure (2010, background): “However, while a number of numerical studies of the f loc NL model have confirmed the scaling bκ ( k, f loc NL ) ∝ MR(k)−1 and the redshift dependence ∝D(z)−1 [13, 42, 43, 98], the exact amplitude of the non-Gaussian bias correction remains somewhat debatable.”
Constraining primordial non-Gaussianity with future galaxy surveys (2011, unknown): “…Dirac delta to give k3 = −k1 − k2 so that we can define k ≡ |k1 + k2|, this expression can be simplified for the three cases extending the calculation by Desjacques et al. (2009) 〈δ3M〉loc = fNL (2π2)2 ∫ ∞ 0 dk1k21 P(k1) α(k1) ∫ ∞ 0 dk2k22 P(k2) α(k2) × ∫ 1 −1 dµα(k) [ 1 + 2 P(k)α2(k2) P(k2)α2(k) ]…”
Large-scale non-Gaussian mass function and halo bias: tests on N-body simulations (2009, methodology): “1 of Desjacques et al. (2009) (black points) at the values of ν corresponding to 1 × 1013, 1 × 1014 and 1 × 1015 M h−1 (as given in their figure caption).”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, background): “More detailed studies of halo mass distribution of BOSS galaxies, combined with numerical simulations of non-Gaussian models [162] as well as studies of how to mitigate the large-angle”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, background): “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…”