The biasing phenomenon

Abstract

{We study biasing as a physical phenomenon by analysing geometrical and clustering properties of density fields of matter and galaxies.} {Our goal is to determine the bias function using a combination of geometrical and power spectrum analysis of simulated and real data.} {We apply an algorithm based on local densities of particles, $\delta$, to form simulated biased models using particles with $\delta \ge {\delta }_0$. We calculate the bias function of model samples as functions of the particle density limit ${\delta }_0$. We compare the biased models with Sloan Digital Sky Survey (SDSS) luminosity limited samples of galaxies using the extended percolation method. We find density limits ${\delta }_0$ of biased models, which correspond to luminosity limited SDSS samples.} {Power spectra of biased model samples allow to estimate the bias function $b(>L)$ of galaxies of luminosity $L$. We find the estimated bias parameter of $L_{\ast }$ galaxies, $b_{\ast }=1.85\pm 0.15$. } {The absence of galaxy formation in low-density regions of the Universe is the dominant factor of the biasing phenomenon. Second largest effect is the dependence of the bias function on the luminosity of galaxies. Variations in gravitational and physical processes during the formation and evolution of galaxies have the smallest influence to the bias function. }

arXiv comment20 pages, 16 figures. Submitted to Astronomy & Astrophysics

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• A Forecast for Large Scale Structure Constraints on Horndeski Gravity with Line Intensity Mapping
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• The time evolution of bias
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• Collapse, connectivity, and galaxy populations in supercluster cocoons: the case of A2142