The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release
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DOI：
10.1093/mnras/stv2826
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发表时间：
2015-09
影响因子：
4.8
通讯作者：
F. Kitaura;Sergio A. Rodríguez-Torres;C. Chuang;Cheng Zhao;F. Prada;H. Gil-Marín;Hong Guo;G. Yepe
中科院分区：
文献类型：
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作者：
F. Kitaura;Sergio A. Rodríguez-Torres;C. Chuang;Cheng Zhao;F. Prada;H. Gil-Marín;Hong Guo;G. Yepe
我们从SDSS-III重子振动光谱调查最终数据发布(BOSS DR11&DR12)中复制了所有相关尺度的高保真星系团星表，以便能够对重子声振荡和红移空间扭曲进行可靠的分析。我们已经产生了(6000)12288个多暗斑块BOSS(DR11)DR12光锥，其有效体积类似于192 000[h(-1)GPC](3)(有史以来最大的模拟体积)，包括从0.15到0.75红移范围内的宇宙演化。根据BOSS DR11和DR12星系团数据的晕丰度匹配模型和数据本身，使用参考星系星表对模型进行了校准。制作过程分三步走。首先，我们应用Patchy代码来生成暗物质场和包含非线性随机星系偏差的天体分布。其次，我们运行晕/恒星分布重建强子程序来分配各种物体的质量。这一步骤使用质量分布作为局域密度和非局域指标(即潮汐场张量本征值和大质量物体的相对晕排除分离)的函数，该参考模拟应用于相应的片状暗物质和星系分布。最后，我们应用糖码来构建光锥。由此产生的MultiDarkPATCHY模拟光锥重现了任意恒星质量箱的数密度、选择函数、观测几何和一般在1西格玛以内的功率谱，直到k=0.3h MPC(-1)，两点关联函数精确到几个MPC尺度，以及BOSS DR11和DR12星系样本的三点统计数据。
We reproduce the galaxy clustering catalogue from the SDSS-III Baryon Oscillation Spectroscopic Survey Final Data Release (BOSS DR11&DR12) with high fidelity on all relevant scales in order to allow a robust analysis of baryon acoustic oscillations and redshift space distortions. We have generated (6000) 12 288 MultiDark PATCHY BOSS (DR11) DR12 light cones corresponding to an effective volume of similar to 192 000 [h(-1) Gpc](3) (the largest ever simulated volume), including cosmic evolution in the redshift range from 0.15 to 0.75. The mocks have been calibrated using a reference galaxy catalogue based on the halo abundance matching modelling of the BOSS DR11&DR12 galaxy clustering data and on the data themselves. The production follows three steps. First, we apply the PATCHY code to generate a dark matter field and an object distribution including non-linear stochastic galaxy bias. Secondly, we run the halo/stellar distribution reconstruction HADRON code to assign masses to the various objects. This step uses the mass distribution as a function of local density and non-local indicators (i.e. tidal field tensor eigenvalues and relative halo exclusion separation for massive objects) from the reference simulation applied to the corresponding patchy dark matter and galaxy distribution. Finally, we apply the SUGAR code to build the light cones. The resulting MultiDarkPATCHY mock light cones reproduce the number density, selection function, survey geometry, and in general within 1 sigma, for arbitrary stellar mass bins, the power spectrum up to k = 0.3 h Mpc(-1), the two-point correlation functions down to a few Mpc scales, and the three-point statistics of the BOSS DR11&DR12 galaxy samples.