The spatial distribution deviation and the power suppression of baryons from dark matter

Abstract

The spatial distribution between dark matter and baryonic matter of the Universe is biased or deviates from each other. In this work, by comparing the results derived from IllustrisTNG and WIGEON simulations, we find that many results obtained from TNG are similar to those from WIGEON data, but differences between the two simulations do exist. For the ratio of density power spectrum between dark matter and baryonic matter, as scales become smaller and smaller, the power spectra for baryons are increasingly suppressed for WIGEON simulations; while for TNG simulations, the suppression stops at $k=15-20h{\mathrm{Mpc}}^{-1}$, and the power spectrum ratios increase when $k>20h{\mathrm{Mpc}}^{-1}$. The suppression of power ratio for WIGEON is also redshift-dependent. From $z=1$ to $z=0$, the power ratio decreases from about 70% to less than 50% at $k=8h{\mathrm{Mpc}}^{-1}$. For TNG simulation, the suppression of power ratio is enhanced with decreasing redshifts in the scale range $k>4h{\mathrm{Mpc}}^{-1}$, but is nearly unchanged with redshifts in $k<4h{\mathrm{Mpc}}^{-1}$ These results indicate that turbulent heating can also have the consequence to suppress the power ratio between baryons and dark matter. Regarding the power suppression for TNG simulations as the norm, the power suppression by turbulence for WIGEON simulations is roughly estimated to be 45% at $k=2h{\mathrm{Mpc}}^{-1}$, and gradually increases to 69% at $k=8h{\mathrm{Mpc}}^{-1}$, indicating the impact of turbulence on the cosmic baryons are more significant on small scales.

References in corpus (11)

• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• The Co-Evolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe
• Properties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids
• Turbulent Heating in Galaxy Clusters Brightest in X-rays
• Modelling baryonic feedback for survey cosmology
• Cosmological Shock Waves in the Large Scale Structure of the Universe: Non-gravitational Effects
• Vorticity of IGM Velocity Field on Large Scales
• Low-Redshift Cosmic Baryon Fluid on Large Scales and She-Leveque Universal Scaling
• Evidence of large scale energy cascade in the spiral galaxy NGC 5236
• Turbulence-induced deviation between baryonic field and dark matter field in the spatial distribution of the Universe
• Statistical and dynamical decoupling of the IGM from Dark Matter

Cited by in corpus (4)

• Connection between galaxy morphology and dark-matter halo structure I: a running threshold for thin discs and size predictors from the dark sector
• Simultaneous Dependence of Matter Clustering on Scale and Environment
• How do baryonic effects on the cosmic matter distribution vary with scale and local density environment?
• Turbulence revealed by wavelet transform: power spectrum and intermittency for the velocity field of the cosmic baryonic fluid