CSST large-scale structure analysis pipeline: I. constructing reference mock galaxy redshift surveys

• Published in: arXiv.org 2024-03
• Main Authors: Gu, Yizhou, Yang, Xiaohu, Han, Jiaxin, Wang, Yirong, Li, Qingyang, Tan, Zhenlin, Jiang, Wenkang, Wang, Yaru, Wang, Jiaqi, Katsianis, Antonios, Xu, Xiaoju, Xu, Haojie, Hong, Wensheng, Mo, Houjun, Wen, Run, Zheng, Xianzhong, Shi, Feng, Zhang, Pengjie, Zhai, Zhongxu, Liu, Chengze, Wang, Wenting, Zu, Ying, Guo, Hong, Zhang, Youcai, Lu, Yi, Zheng, Yi, Han, Yunkun, Zou, Hu, Wang, Xin, Wei, Chengliang, Li, Ming, Luo, Yu
• Format: Article
• Language: English
• Subjects: Dark matter; Galaxies; Large scale structure of the universe; Luminosity; Red shift; Simulation; Stars & galaxies; Structural analysis
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2403.10754

In this paper, we set out to construct a set of reference mock galaxy redshift surveys (MGRSs) for the future Chinese Space-station Survey Telescope (CSST) observation, where subsequent survey selection effects can be added and evaluated. This set of MGRSs is generated using the dark matter subhalos extracted from a high-resolution Jiutian \(N\)-body simulation of the standard \(\Lambda\)CDM cosmogony with \(\Omega_m=0.3111\), \(\Omega_{\Lambda}=0.6889\), and \(\sigma_8=0.8102\). The simulation has a boxsize of \(1~h^{-1} {\rm Gpc}\), and consists of \(6144^3\) particles with mass resolution \(3.723 \times 10^{8} h^{-1} M_\odot \). In order to take into account the effect of redshift evolution, we first use all 128 snapshots in the Jiutian simulation to generate a light-cone halo/subhalo catalog. Next, galaxy luminosities are assigned to the main and subhalo populations using the subhalo abundance matching (SHAM) method with the DESI \(z\)-band luminosity functions at different redshifts. Multi-band photometries, as well as images, are then assigned to each mock galaxy using a 3-dimensional parameter space nearest neighbor sampling of the DESI LS observational galaxies and groups. Finally, the CSST and DESI LS survey geometry and magnitude limit cuts are applied to generate the required MGRSs. As we have checked, this set of MGRSs can generally reproduce the observed galaxy luminosity/mass functions within 0.1 dex for galaxies with \(L > 10^8 L_\odot\) (or \(M_* > 10^{8.5} M_\odot\)) and within 1-\(\sigma\) level for galaxies with \(L < 10^8L_\odot\) (or \(M_* < 10^{8.5} M_\odot\)). Together with the CSST slitless spectra and redshifts for our DESI LS seed galaxies that are under construction, we will set out to test various slitless observational selection effects in subsequent probes.