Primordial non-Gaussianity in the bispectrum of the halo density field

被引:86
作者
Baldauf, Tobias [1 ]
Seljak, Uros [1 ,2 ,3 ,4 ]
Senatore, Leonardo [5 ,6 ]
机构
[1] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland
[2] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[3] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA
[4] Ewha Womans Univ, Inst Early Universe, Seoul 120750, South Korea
[5] Stanford Univ, Stanford Inst Theoret Phys, Stanford, CA 94305 USA
[6] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA
关键词
galaxy clustering; non-gaussianity; inflation; power spectrum; LARGE-SCALE STRUCTURE; INFLATIONARY UNIVERSE; BIAS; FLUCTUATIONS; EVOLUTION; GALAXIES; CLUSTERS; FLATNESS; HORIZON; PROBE;
D O I
10.1088/1475-7516/2011/04/006
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The bispectrum vanishes for linear Gaussian fields and is thus a sensitive probe of non-linearities and non-Gaussianities in the cosmic density field. Hence, a detection of the bispectrum in the halo density field would enable tight constraints on non-Gaussian processes in the early Universe and allow inference of the dynamics driving inflation. We present a tree level derivation of the halo bispectrum arising from non-linear clustering, non-linear biasing and primordial non-Gaussianity. A diagrammatic description is developed to provide an intuitive understanding of the contributing terms and their dependence on scale, shape and the non-Gaussianity parameter f(NL). We compute the terms based on a multivariate bias expansion and the peak-background split method and show that non-Gaussian modifications to the bias parameters lead to amplifications of the tree level bispectrum that were ignored in previous studies. Our results are in a good agreement with published simulation measurements of the halo bispectrum. Finally, we estimate the expected signal to noise on f(NL) and show that the constraint obtainable from the bispectrum analysis significantly exceeds the one obtainable from the power spectrum analysis.
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页数:38
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