Guo Hong, Zheng Zheng, Behroozi Peter S, Zehavi Idit, Chuang Chia-Hsun, Comparat Johan, Favole Ginevra, Gottloeber Stefan, Klypin Anatoly, Prada Francisco, Rodríguez-Torres Sergio A, Weinberg David H, Yepes Gustavo
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Shanghai 200030, China; Department of Physics and Astronomy, University of Utah, UT 84112, USA.
Department of Physics and Astronomy, University of Utah, UT 84112, USA.
Mon Not R Astron Soc. 2016 Apr 13;459(3):3040-3058. doi: 10.1093/mnras/stw845. eCollection 2016 Jul 1.
We model the luminosity-dependent projected and redshift-space two-point correlation functions (2PCFs) of the Sloan Digital Sky Survey (SDSS) Data Release 7 Main galaxy sample, using the halo occupation distribution (HOD) model and the subhalo abundance matching (SHAM) model and its extension. All the models are built on the same high-resolution -body simulations. We find that the HOD model generally provides the best performance in reproducing the clustering measurements in both projected and redshift spaces. The SHAM model with the same halo-galaxy relation for central and satellite galaxies (or distinct haloes and subhaloes), when including scatters, has a best-fitting χ/dof around 2-3. We therefore extend the SHAM model to the subhalo clustering and abundance matching (SCAM) by allowing the central and satellite galaxies to have different galaxy-halo relations. We infer the corresponding halo/subhalo parameters by jointly fitting the galaxy 2PCFs and abundances and consider subhaloes selected based on three properties, the mass at the time of accretion, the maximum circular velocity at the time of accretion, and the peak maximum circular velocity over the history of the subhaloes. The three subhalo models work well for luminous galaxy samples (with luminosity above ). For low-luminosity samples, the model stands out in reproducing the data, with the model slightly worse, while the model fails to fit the data. We discuss the implications of the modelling results.
我们使用晕族占据分布（HOD）模型、次晕丰度匹配（SHAM）模型及其扩展，对斯隆数字巡天（SDSS）数据释放7主星系样本的光度依赖投影和红移空间两点相关函数（2PCFs）进行建模。所有模型均基于相同的高分辨率N -体模拟构建。我们发现，HOD模型在再现投影空间和红移空间中的聚类测量方面通常表现最佳。对于中心星系和卫星星系（或不同的晕和次晕）具有相同晕-星系关系的SHAM模型，在包含散射时，最佳拟合χ²/dof约为2 - 3。因此，我们通过允许中心星系和卫星星系具有不同的星系-晕关系，将SHAM模型扩展到次晕聚类和丰度匹配（SCAM）。我们通过联合拟合星系2PCFs和丰度来推断相应的晕/次晕参数，并考虑基于三个属性选择的次晕，即吸积时的质量、吸积时的最大圆周速度以及次晕历史上的峰值最大圆周速度。这三个次晕模型对发光星系样本（光度高于 ）效果良好。对于低光度样本， 模型在再现数据方面表现突出， 模型稍差，而 模型无法拟合数据。我们讨论了建模结果的含义。
