星系原星系团的LCDM预言I：z~6星系、原星系团和类星体之间的关系
LCDM predictions for galaxy protoclusters I: the relation between galaxies, protoclusters and quasars at z~6
摘要：
受最近对z~6类星体环境的观测研究的启发，我们利用Millennium Run（MR）模拟构建了一个非常大的（~20 deg^2）z~6恒星形成星系的模拟红移巡天。我们使用这个模拟调查，以研究密度增强的i-辍学和Lya-发射体的分布之间的关系，以及它们与z~6处的最大质量晕和原星系团区域的关系。我们的模拟预测了整个天空中表面密度的显着变化，其中一些空洞和细丝延伸到1度的尺度上，比目前的调查大得多。大约三分之一的z~6晕中的i-dropout比z=26.5等（z=6时~M*）亮，成为z=0星系团的一部分。与原星系团区域有关的i-脱落现象出现在表面密度在天空中从几角分到几十角分的尺度上增强的区域。我们分析了斯巴鲁望远镜观测到的两种i-dropouts和Lya-emitter结构，并表明这些结构必须是大质量星系团形成的种子。与此形成鲜明对比的是，用HST观测到的6个z~6类星体场的i-dropout数没有明显的增加。根据目前的数据，我们不能排除类星体由最大质量的晕所承载。然而，我们也不能证实这一广泛使用的假设。最后，我们给出了详细的建议，解释和规划的意见，目前和未来的地面和空间为基础的仪器，将揭示新的光在z~6的大尺度结构相关的问题。
英文摘要：
Motivated by recent observational studies of the environment of z~6 QSOs, we have used the Millennium Run (MR) simulations to construct a very large (~20 deg^2) mock redshift survey of star-forming galaxies at z~6. We use this simulated survey to study the relation between density enhancements in the distribution of i-dropouts and Lya-emitters, and their relation to the most massive halos and protocluster regions at z~6. Our simulation predicts significant variations in surface density across the sky with some voids and filaments extending over scales of 1 degree, much larger than probed by current surveys. Approximately one third of all z~6 halos hosting i-dropouts brighter than z=26.5 mag (~M* at z=6) become part of z=0 galaxy clusters. i-dropouts associated with protocluster regions are found in regions where the surface density is enhanced on scales ranging from a few to several tens of arcminutes on the sky. We analyze two structures of i-dropouts and Lya-emitters observed with the Subaru Telescope and show that these structures must be the seeds of massive clusters-in-formation. In striking contrast, six z~6 QSO fields observed with HST show no significant enhancements in their i-dropout number counts. With the present data, we cannot rule out the QSOs being hosted by the most massive halos. However, neither can we confirm this widely used assumption. We conclude by giving detailed recommendations for the interpretation and planning of observations by current and future ground- and space based instruments that will shed new light on questions related to the large-scale structure at z~6.
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