The Effect of Primordial Non-Gaussianity on Halo Bias
The Effect of Primordial Non-Gaussianity on Halo Bias
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DOI：
10.1086/587840
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发表时间：
2008-01
期刊：
影响因子：
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通讯作者：
S. Matarrese;L. Verde
中科院分区：
文献类型：
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作者：
S. Matarrese;L. Verde
在高斯初始条件下，如何解析地将坍缩结构（晕）的聚类特性与潜在暗物质分布的聚类特性联系起来，早已为人所知。这里我们将同样的方法应用于物理驱动的非高斯模型。我们使用的技术是在20世纪80年代开发的，用于处理非高斯密度场峰的聚类。在即将到来的大型星系和星团调查的推动下，对非高斯初始条件下晕团的描述最近重新引起了人们的兴趣。对于膨胀激发的非高斯现象，我们发现光晕偏差作为尺度、质量和红移的函数的解析表达式，仅采用高峰和大分离的近似。
It has long been known how to analytically relate the clustering properties of the collapsed structures (halos) to those of the underlying dark matter distribution for Gaussian initial conditions. Here we apply the same approach to physically motivated non-Gaussian models. The techniques we use were developed in the 1980s to deal with the clustering of peaks of non-Gaussian density fields. The description of the clustering of halos for non-Gaussian initial conditions has recently received renewed interest, motivated by the forthcoming large galaxy and cluster surveys. For inflationary-motivated non-Gaussianities, we find an analytic expression for the halo bias as a function of scale, mass, and redshift, employing only the approximations of high peaks and large separations.