Evidence for quadratic tidal tensor bias from the halo bispectrum

By T. Baldauf, Uros Seljak, V. Desjacques, P. Mcdonald. 2012

215 citations recorded by the source corpus.

The relation between the clustering properties of luminous matter in the form of galaxies and the underlying dark matter distribution is of fundamental importance for the interpretation of ongoing and upcoming galaxy surveys. The so-called local bias model, where galaxy density is a function of local matter density, is frequently discussed as a means to infer the matter power spectrum or correlation function from the measured galaxy correlation. However, gravitational evolution generates a term quadratic in the tidal tensor and thus nonlocal in the Eulerian density field, even if this term is absent in the initial conditions (Lagrangian space). Because the term is quadratic, it contributes as a loop correction to the power spectrum, so the standard linear bias picture still applies on very large scales; however, it contributes at leading order to the bispectrum for which it is significant on all scales. Such a term could also be present in Lagrangian space if halo formation were influenced by the tidal field. We measure the corresponding coupling strengths from the matter-matter-halo bispectrum in numerical simulations and find a nonvanishing coefficient for the tidal tensor term. We find no scale dependence of the inferred bias parameters up to k∼0.1h Mpc−1 and that the tidal effect is increasing with halo mass. While the local Lagrangian bias picture is a better description of our results than the local Eulerian bias picture, our results suggest that there might be a tidal tensor bias already in the initial conditions. We also find that the coefficients of the quadratic density term deviate quite strongly from the theoretical predictions based on the spherical collapse model and a universal mass function. Both quadratic density and tidal tensor bias terms must be included in the modeling of galaxy clustering of current and future surveys if one wants to achieve the high precision cosmology promise of these data sets.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/85cf901399188d82be4c370fa8f2d3e74f2318af

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Citations in the corpus

Biased tracers and time evolution (2014, background): “Evidence from numerical simulations as well as phenomenological explanations have been provided in [10, 11].”
Convolution Lagrangian perturbation theory for biased tracers (2012, background): “The corresponding non-local Eulerian bias terms can be most easily seen in their contribution to the bispectrum of halos (Baldauf et al. 2012; Chan, Scoccimarro, & Sheth 2012).”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, background): “The physics of how they trace the dark matter fluctuations is well understood based on arguments about locality of galaxy formation [54, 55, 56].”
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: 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).”
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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): “…case of the local Lagrangian 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…”
Renormalized halo bias (2014, methodology): “For instance, at quadratic order, we have to add the tidal tensor (∇i∇jΦg)(2) [14, 16, 17], where Φg is the gravitational potential, while, at cubic order, the velocity potential Φv has to be introduced as an independent degree of freedom.”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, background): “…in the sense that other non-linear bias parameters at a quadratic and cubic level may be needed to properly model the data (Chan et al. 2012; Baldauf et al. 2012), but these higher order parameters may not be that different in terms of their effect on the scale dependence of the statistics…”
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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).”
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