A galaxy-halo model of large-scale structure

Abstract

We present a new, galaxy-halo model of large-scale structure, in which the galaxies entering a given sample are the fundamental objects. Haloes attach to galaxies, in contrast to the standard halo model, in which galaxies attach to haloes. The galaxy-halo model pertains mainly to the relationships between the power spectra of galaxies and mass, and their cross-power spectrum. With surprisingly little input, an intuition-aiding approximation to the galaxy-matter cross-correlation coefficient R(k) emerges, in terms of the halo mass dispersion. This approximation seems valid to mildly non-linear scales (k < ~3 h/Mpc), allowing measurement of the bias and the matter power spectrum from measurements of the galaxy and galaxy-matter power spectra (or correlation functions). This is especially relevant given the recent advances in precision in measurements of the galaxy-matter correlation function from weak gravitational lensing. The galaxy-halo model also addresses the issue of interpreting the galaxy-matter correlation function as an average halo density profile, and provides a simple description of galaxy bias as a function of scale.

13 pages, 9 figures, submitted to MNRAS. Minor changes, suggested by referee

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• The Galaxy-mass Correlation Function Measured from Weak Lensing in the SDSS
• Modeling Galaxy-Mass Correlations in Dissipationless Simulations
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Cited by in corpus (9)

• Modeling Luminosity-Dependent Galaxy Clustering Through Cosmic Time
• Clustering of dark matter tracers: generalizing bias for the coming era of precision LSS
• Cosmology with Void-Galaxy Correlations
• Cross-Correlation Lensing: Determining Galaxy and Cluster Mass Profiles from Statistical Weak Lensing Measurements
• A halo bias function measured deeply into voids without stochasticity
• COSMOS: Stochastic bias from measurements of weak lensing and galaxy clustering
• Scale-dependent Galaxy Bias
• Effects of biasing on the galaxy power spectrum at large scales
• $\text{PineTree}$: A generative, fast, and differentiable halo model for wide-field galaxy surveys