Modeling Luminosity-dependent Galaxy Clustering through Cosmic Time

  title={Modeling Luminosity-dependent Galaxy Clustering through Cosmic Time},
  author={Charlie Conroy and Risa H. Wechsler and Andrey V. Kravtsov},
  journal={The Astrophysical Journal},
  pages={201 - 214}
We employ high-resolution dissipationless simulations of the concordance ΛCDM cosmology (Ω0 = 1 - ΩΛ = 0.3, h = 0.7, σ8 = 0.9) to model the observed luminosity dependence and evolution of galaxy clustering through most of the age of the universe, from z ~ 5 to z ~ 0. We use a simple, nonparametric model, which monotonically relates galaxy luminosities to the maximum circular velocity of dark matter halos (Vmax) by preserving the observed galaxy luminosity function in order to match the halos in… 
The stellar-to-halo mass relation over the past 12 Gyr
Aims. Understanding the link between the galaxy properties and the dark matter halos they reside in and their coevolution is a powerful tool for constraining the processes related to galaxy
Modelling the tightest relation between galaxy properties and dark matter halo properties from hydrodynamical simulations of galaxy formation
  • Jian-hua He
  • Physics
    Monthly Notices of the Royal Astronomical Society
  • 2020
We investigate how a property of a galaxy correlates most tightly with a property of its host dark matter halo, using state-of-the-art hydrodynamical simulations of galaxy formation: EAGLE,
We present results of self-consistent, high-resolution cosmological simulations of galaxy formation at z ∼ 3. The simulations employ a recently developed recipe for star formation based on the local
Virial scaling of galaxies in clusters: bright to faint is cool to hot
By combining galaxy tracers from high-resolution N-body and hydrodynamical simulations, we present a consistent picture of the behaviour of galaxy velocities in massive clusters. In haloes above ~
Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations
We report and provide fitting functions for the abundance of dark matter halos and subhalos as a function of mass, circular velocity, and redshift from the new Bolshoi- Planck and MultiDark-PlanckCDM
Constraining the physics of galaxy formation and evolution using galaxy clustering
We model the evolution of galaxy clustering through cosmic time to investigate the nature of the power-law shape of ξ(r), the galaxy two-point correlation function. While ξ(r) on large scales is set
Probing the galaxy–halo connection in UltraVISTA to z ∼ 2
We use percent-level precision photometric redshifts in the UltraVISTA-DR1 near-infrared survey to investigate the changing relationship between galaxy stellar mass and the dark matter haloes hosting
We use high-resolution N-body simulations, combined with a halo occupation model of galaxy bias, to investigate voids in the galaxy distribution. Our goal is to address the “void phenomenon” of
We present a new model to describe the galaxy–dark matter connection across cosmic time, which unlike the popular subhalo abundance-matching technique is self-consistent in that it takes account of
A model for cosmological simulations of galaxy formation physics: multi-epoch validation
We present a multi-epoch analysis of the galaxy populations formed within the cosmological hydrodynamical simulations presented in Vogelsberger et al. (2013). These simulations explore the


Modeling Galaxy-Mass Correlations in Dissipationless Simulations
We use high-resolution, dissipationless simulations of the concordance flat ΛCDM model to make predictions for the galaxy-mass correlations and compare them with the recent Sloan Digital Sky Survey
The Clustering of High-Redshift Galaxies in the Cold Dark Matter Scenario
We investigate the clustering of high-redshift galaxies in five variants of the cold dark matter (CDM) scenario, using hydrodynamic cosmological simulations that resolve the formation of systems with
Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies
We use the conditional luminosity function �(L|M)dL, which gives the number of galaxies with luminosities in the range L±dL/2 that reside in a halo of mass M, to link the distribution of galaxies to
Breaking the hierarchy of galaxy formation
Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because
The nature of high-redshift galaxies
Abstract Using semi-analytic models of galaxy formation, we investigate the properties of z∼3 galaxies and compare them with the observed population of Lyman-break galaxies (LBGs). In addition to the
Halo model at its best: constraints on conditional luminosity functions from measured galaxy statistics
Using the conditional luminosity function (CLF; the luminosity distribution of galaxies in a dark matter halo) as the fundamental building block, we present an empirical model for the galaxy
The Halo Occupation Distribution and the Physics of Galaxy Formation
The halo occupation distribution (HOD) describes the bias between galaxies and dark matter by specifying (1) the probability P(N|M) that a halo of virial mass M contains N galaxies of a particular
Clustering of galaxies in a hierarchical universe — II. Evolution to high redshift
In hierarchical cosmologies the evolution of galaxy clustering depends both on cosmological quantities such as Ω, Λ and P(k), which determine how collapsed structures – dark matter haloes – form and
Radial distribution and strong lensing statistics of satellite galaxies and substructure using high‐resolution ΛCDM hydrodynamical simulations
We analyse the number density and radial distribution of substructures and satellite galaxies using cosmological simulations that follow the gas dynamics of a baryonic component, including shock
Evolution of Bias in Different Cosmological Models
We study the evolution of the halo-halo correlation function and small-scale (≈0.2-7 h-1 Mpc) bias in four cosmological models (ΛCDM, OCDM, τCDM, and SCDM) using very high resolution n-body