期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 475, 期 1, 页码 676-698出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx3304
关键词
methods: numerical; galaxy formation; large-scale structure of Universe
资金
- European Research Council [EXAGAL-308037]
- subproject EXAMAG of the Priority Programme 'Software for Exascale Computing' of the German Science Foundation [1648]
- MIT RSC award
- Alfred P. Sloan Foundation
- NASA ATP grant [NNX17AG29G]
- NSF AARF award [AST-1402480]
- NASA through Hubble Fellowship - STScI [HST-HF2-51341.001-A, HST-HF2-51384.001-A]
- NASA [NAS5-26555]
- Simons Foundation
- TACC/XSEDE [AST140063]
Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here, we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies, and haloes over an exceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k similar to 10 h Mpc(-1) by 20 per cent. The non-linear two-point correlation function of the stellar mass is close to a power-law over a wide range of scales and approximately invariant in time from very high redshift to the present. The two-point correlation function of the simulated galaxies agrees well with Sloan Digital Sky Survey at its mean redshift z similar or equal to 0.1, both as a function of stellar mass and when split according to galaxy colour, apart from a mild excess in the clustering of red galaxies in the stellar mass range of 10(9)-10(10) h(-2) M circle dot. Given this agreement, the TNG simulations can make valuable theoretical predictions for the clustering bias of different galaxy samples. We find that the clustering length of the galaxy autocorrelation function depends strongly on stellar mass and redshift. Its power-law slope gamma is nearly invariant with stellar mass, but declines from gamma similar to 1.8 at redshift z = 0 to y gamma similar to 1.6 at redshift z similar to 1, beyond which the slope steepens again. We detect significant scale dependences in the bias of different observational tracers of large-scale structure, extending well into the range of the baryonic acoustic oscillations and causing nominal (yet fortunately correctable) shifts of the acoustic peaks of around similar to 5 per cent.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据