Bispectrum and Nonlinear Biasing of Galaxies: Perturbation Analysis, Numerical Simulation, and SDSS Galaxy Clustering
Bispectrum and Nonlinear Biasing of Galaxies: Perturbation Analysis, Numerical Simulation, and SDSS Galaxy Clustering
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DOI：
10.1093/pasj/59.1.93
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发表时间：
2006-09
影响因子：
2.3
通讯作者：
T. Nishimichi;I. Kayo;C. Hikage;Kazuhiro Yahata;A. Taruya;Y. Jing;R. Sheth;Y. Suto
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作者：
T. Nishimichi;I. Kayo;C. Hikage;Kazuhiro Yahata;A. Taruya;Y. Jing;R. Sheth;Y. Suto
我们考虑星系的非线性偏置模型，特别关注线性和二次偏置系数B（1）和B（2）之间的相关性。我们首先推导了晕和峰偏置模型中B（1）和B（2）的微扰表达式。然后讨论了利用N体模拟数据和Sloan数字巡天（SDSS）星系的有限体积子样本计算暗物质粒子和晕的功率谱和双谱，并确定了它们的B（1）和B（2）。我们发现，在线性区域（k <0.2hMpc（-1）），这些系数的值对红移空间畸变和观测体形状相当不敏感。等边三角形的双谱Q的归一化幅度对B（1）的值不敏感，这意味着B（2）确实与B（1）相关。本文的结果解释了Kayo等人（2004，PASJ，56，415）关于SDSS星系三点关联函数的等级关系的发现。虽然B（1）和B（2）之间的关系对于特定的偏置模型是定量不同的，但它们近似相似的相关性表明，在原始高斯密度场中，由于引力而产生的偏置是相当普遍的结果。
We consider nonlinear biasing models of galaxies with particular attention to a correlation between the linear and quadratic biasing coefficients, b(1) and b(2). We first derive perturbative expressions for b(1) and b(2) in halo and peak biasing models. We then discuss our computations of the power spectra and bispectra of dark matter particles and halos using N-body simulation data and of volume-limited subsamples of Sloan Digital Sky Survey (SDSS) galaxies, and determine their b(1) and b(2). We find that the values of those coefficients at linear regimes (k < 0.2 h Mpc(-1)) are fairly insensitive to the redshift-space distortion and the survey volume shape. The resulting normalized amplitudes of the bispectra, Q, for equilateral triangles are insensitive to the values of b(1), implying that b(2) indeed correlates with b(1). The present results explain the previous finding of Kayo et al. (2004, PASJ, 56, 415) for the hierarchical relation of three-point correlation functions of SDSS galaxies. While the relations between b(1) and b(2) are quantitatively different for specific biasing models, their approximately similar correlations indicate a fairly generic outcome of the biasing due to the gravity in primordial Gaussian density fields.