Understanding Higher-Order Nonlocal Halo Bias at Large Scales by Combining the Power Spectrum with the Bispectrum

By S. Saito, T. Baldauf, Z. Vlah, Urovs Seljak Teppei Okumura, P. Mcdonald. 2014

148 citations recorded by the source corpus.

Understanding the relation between underlying matter distribution and biased tracers such as galaxy or dark matter halo is essential to extract cosmological information from ongoing or future galaxy redshift surveys. At sufficiently large scales such as the BAO scale, a standard approach for the bias problem on the basis of the perturbation theory (PT) is to assume the `local bias' model in which the density field of biased tracers is deterministically expanded in terms of matter density field at the same position. The higher-order bias parameters are then determined by combining the power spectrum with higher-order statistics such as the bispectrum. As is pointed out by recent studies, however, nonlinear gravitational evolution naturally induces nonlocal bias terms even if initially starting only with purely local bias. As a matter of fact, previous works showed that the second-order nonlocal bias term, which corresponds to the gravitational tidal field, is important to explain the characteristic scale-dependence of the bispectrum. In this paper we extend the nonlocal bias term up to third order, and investigate whether the PT-based model including nonlocal bias terms can simultaneously explain the power spectrum and the bispectrum of simulated halos in $N$-body simulations. We show that the power spectrum, including density and momentum, and the bispectrum between halo and matter in $N$-body simulations can be simultaneously well explained by the model including up to third-order nonlocal bias terms up to k~0.1h/Mpc. Also, the results seem in a good agreement with theoretical predictions of a simple coevolution picture, although the agreement is not perfect. These demonstration clearly shows a failure of the local bias model even at such large scales, and we conclude that nonlocal bias terms should be consistently included in order to model statistics of halos. [abridged]

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d823aa9c93ffc59f7f55d11c382498d4769e5d8c

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Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release (2015, background): “Non-local bias has been recently found to be relevant (McDonald & Roy 2009; Baldauf et al. 2012; Chan, Scoccimarro & Sheth 2012; Sheth, Chan & Scoccimarro 2013; Saito et al. 2014).”
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): “This allows us to set the values of bs2 and b3nl as functions of b1 (Baldauf et al. 2012; Chan et al. 2012; Saito et al. 2014), bs2 = −4/7(b1 − 1) and b3nl = 32/315(b1 − 1), meaning that only two bias parameters need to be fitted.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, background): “…Lagrangian bias (Sheth, Chan & Scoccimarro 2013), a bispectrum analysis of dark matter haloes shows that the γ 2(b1) relation in equation (13) is at least a reasonable first approximation (Baldauf et al. 2012; Chan et al. 2012; Sheth et al. 2013; Saito et al. 2014; Bel, Hoffmann & Gaztañaga 2015).”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: a tomographic measurement of cosmic structure growth and expansion rate based on optimal redshift weights (2018, unknown): “We have eliminated the second-order non-local bias bs2 and the third-order non-local bias b3nl using the following relation (Chan, Scoccimarro & Sheth 2012; Baldauf et al. 2012; Saito et al. 2014), bs2 = −4 7 (b1 − 1) , b3nl = 32 315 (b1 − 1) .”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, background): “…bias picture in which the initial non-local bias is neglected, we can predict the amplitude of the non-local bias as (Baldauf et al. 2012; Chan et al. 2012; Saito et al. 2014) bs2 = −4 7 (b1 − 1), (54) b3nl = 32 315 (b1 − 1), (55) which are in good agreement with the values measured in simulations.”
Consistent modeling of velocity statistics and redshift-space distortions in one-loop perturbation theory (2020, unknown): “[75, 76]).”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “Note also that modeling the galaxy bias is another important issue to use RSD for precision cosmology because the galaxy bias is known to suffer from nonlinearity (See, e.g.,Saito et al. (2014) for one of the latest studies to formulate the nonlinear bias).”