The Effect of Primordial Non-Gaussianity on Halo Bias

Matarrese, S.; Verde, Licia

doi:10.1086/587840

Cited by 422 publications

(673 citation statements)

References 26 publications

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“…The Fourier space formalism was used by a majority of papers on non-Gaussian bias (e.g. [45,57,58,59,60]). However, an arguably more intuitive measure of the bias is in real space, where the density fluctuation in peaks (i.e.…”

Section: Biasmentioning

confidence: 99%

Primordial non-Gaussianity and extreme-value statistics of galaxy clusters

Chongchitnan¹,

Silk

2012

Phys. Rev. D

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What is the size of the most massive object one expects to find in a survey of a given volume? In this paper, we present a solution to this problem using Extreme-Value Statistics, taking into account primordial non-Gaussianity and its effects on the abundance and the clustering of rare objects. We calculate the probability density function (pdf) of extreme-mass clusters in a survey volume, and show how primordial non-Gaussianity shifts the peak of this pdf. We also study the sensitivity of the extreme-value pdfs to changes in the mass functions, survey volume, redshift coverage and the normalization of the matter power spectrum, σ8. For 'local' non-Gaussianity parametrized by f NL , our correction for the extreme-value pdf due to the bias is important when f NL 100, and becomes more significant for wider and deeper surveys. Applying our formalism to the massive high-redshift cluster XMMUJ0044.0-2-33, we find that its existence is consistent with f NL = 0, although the conclusion is sensitive to the assumed values of f sky and σ8. We also discuss the convergence of the extreme-value distribution to one of the three possible asymptotic forms, and argue that the convergence is insensitive to the presence of non-Gaussianity.

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Section: Biasmentioning

confidence: 99%

Primordial non-Gaussianity and extreme-value statistics of galaxy clusters

Chongchitnan¹,

Silk

2012

Phys. Rev. D

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“…This excess power at large scale can be induced by primordial non-Gaussianity (see e.g. Matarrese & Verde 2008;Dalal et al 2008;Slosar et al 2008;Desjacques & Seljak 2010;Xia et al 2010) or exotic physics (Thomas et al 2010); however Samushia et al 2011 found that the redshift dependence of the excess power is different from what would be caused by non-Gaussianity, and Ross et al (2011) suggest that this is likely to be due to masking effects from stellar sources. After correcting for systematics, Ross et al (2012) found consistency at better than 2σ between the BOSS CMASS DR9 large-scale clustering data and the WMAP LCDM cosmological model.…”

Section: A4 Las Damas Mocksmentioning

confidence: 99%

Testing gravity using large-scale redshift-space distortions

Raccanelli

Bertacca

Pietrobon

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We use Luminous Red Galaxies from the Sloan Digital Sky Survey II to test the cosmological structure growth in two alternatives to the standard ΛCDM+GR cosmological model. We compare observed three-dimensional clustering in SDSS DR7 with theoretical predictions for the standard vanilla ΛCDM+GR model, Unified Dark Matter cosmologies and the normal branch DGP. In computing the expected correlations in UDM cosmologies, we derive a parameterized formula for the growth factor in these models. For our analysis we apply the methodology tested in Raccanelli et al. (2010) and use the measurements of Samushia et al. (2011), that account for survey geometry, non-linear and wide-angle effects and the distribution of pair orientation. We show that the estimate of the growth rate is potentially degenerate with wide-angle effects, meaning that extremely accurate measurements of the growth rate on large scales will need to take such effects into account. We use measurements of the zeroth and second order moments of the correlation function from SDSS DR7 data and the Large Suite of Dark Matter Simulations (LasDamas: McBride et al. 2011), and perform a likelihood analysis to constrain the parameters of the models. Using information on the clustering up to r max = 120 Mpc/h, and after marginalizing over the bias, we find, for UDM models, a speed of sound c ∞ 6.1e-4, and, for the nDGP model, a cross-over scale r c 340 Mpc, at 95% confidence level.

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“…Following the approach of Kaiser (1984), Matarrese & Verde (2008) also computed the effect of local-type nonGaussianity (1) on the halo two-point correlation. Drawing on earlier work by Matarrese et al (1986), who computed the n-point halo correlations by expanding the relevant pathintegrals and next resumming the series within a large-distance and rare-event approximation, they obtained expressions of the form (72) without the prefactor (1 + δ LM ) and (84) without the terms in the first line, which arise from this prefactor, and the last term f 1;11 in the second bracket.…”

Section: Bias Of Dark Matter Halosmentioning

confidence: 99%

Mass function and bias of dark matter halos for non-Gaussian initial conditions

Valageas

2010

A&A

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Aims. We revisit the derivation of the mass function and the bias of dark matter halos for non-Gaussian initial conditions. Methods. We use a steepest-descent approach to point out that exact results can be obtained for the high-mass tail of the halo mass function and the two-point correlation of massive halos. Focusing on primordial non-Gaussianity of the local type, we check that these results agree with numerical simulations. Results. The high-mass cutoff of the halo mass function takes the same form as the one obtained from the Press-Schechter formalism, but with a linear threshold δ L that depends on the definition of the halo (i.e. δ L 1.59 for a nonlinear density contrast of 200). We show that a simple formula, which obeys this high-mass asymptotic and uses the fit obtained for Gaussian initial conditions, matches numerical simulations while keeping the mass function normalized to unity. Next, by deriving the real-space halo two-point correlation in the spirit of Kaiser (1984, ApJ, 284, L9) and taking a Fourier transform, we obtain good agreement with simulations for the correction to the halo bias, Δb M (k, f NL ), due to primordial non-Gaussianity. Therefore, neither the halo mass function nor the bias require an ad-hoc parameter q (such as δ c → δ c √ q), provided one uses the correct linear threshold δ L and pays attention to halo displacements. The nonlinear real-space expression can be useful for checking that the "linearized" bias is a valid approximation. Moreover, it clearly shows how the baryon acoustic oscillation at ∼100 h −1 Mpc is amplified by the bias of massive halos and modified by primordial non-Gaussianity. On smaller scales, 30 < x < 90 h −1 Mpc, the correction to the real-space bias roughly scales asThe low-k behavior of the halo bias does not imply a divergent real-space correlation, so that one does not need to introduce counterterms that depend on the survey size.

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The Effect of Primordial Non-Gaussianity on Halo Bias

Cited by 422 publications

References 26 publications

Primordial non-Gaussianity and extreme-value statistics of galaxy clusters

Primordial non-Gaussianity and extreme-value statistics of galaxy clusters

Testing gravity using large-scale redshift-space distortions

Mass function and bias of dark matter halos for non-Gaussian initial conditions

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