Scale dependence of halo bispectrum from non-Gaussian initial conditions in cosmological N-body simulations

被引：39

作者：

Nishimichi, Takahiro ^{[1
,3
]}

Taruya, Atsushi ^{[2
,3
]}

Koyama, Kazuya ^{[4
]}

Sabiu, Cristiano ^{[4
,5
]}

机构：

[1] Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan

[2] Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan

[3] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan

[4] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[5] UCL, Dept Phys & Astron, London, England

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2010年 / 07期

关键词：

cosmological simulations; cosmological parameters from LSS; redshift surveys; PRIMORDIAL NON-GAUSSIANITY; MASS FUNCTION; NONLINEAR EVOLUTION; BIAS; STATISTICS; ABUNDANCE; UNIVERSE; PROBE;

D O I：

10.1088/1475-7516/2010/07/002

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the halo bispectrum from non-Gaussian initial conditions. Based on a set of large N-body simulations starting from initial density fields with local type non-Gaussianity, we find that the halo bispectrum exhibits a strong dependence on the shape and scale of Fourier space triangles near squeezed configurations at large scales. The amplitude of the halo bispectrum roughly scales as f(NL)(2). The resultant scaling on the triangular shape is consistent with that predicted by Jeong & Komatsu based on perturbation theory. We systematically investigate this dependence with varying redshifts and halo mass thresholds. It is shown that the f(NL) dependence of the halo bispectrum is stronger for more massive haloes at higher redshifts. This feature can be a useful discriminator of inflation scenarios in future deep and wide galaxy redshift surveys.

引用

页数：27