The Probability Distribution Function of Light in the Universe: Results from Hydrodynamic Simulations

  title={The Probability Distribution Function of Light in the Universe: Results from Hydrodynamic Simulations},
  author={Jeremiah P. Ostriker and Kentaro Nagamine and Renyue Cen and Masataka Fukugita IoA and Cambridge and Princeton and Harvard-CfA and Icrr},
  journal={The Astrophysical Journal},
While second and higher order correlations of the light distribution have received extensive study, the lowest order probability distribution function (PDF)—the probability that a unit volume of space will emit a given amount of light—has received very little attention. We estimate this function with the aid of hydrodynamic simulations of the ΛCDM model, finding it significantly different from the mass density PDF, and not simply related to it by linear bias or any of the other prescriptions… 

Figures from this paper

The VIMOS VLT deep survey: testing the gravitational instability paradigm at z ~ 1
We have reconstructed the three-dimensional density fluctuation maps to z˜ 1.5 using the distribution of galaxies observed in the VVDS-Deep survey. We use this overdensity field to measure the
Light-to-Mass Variations with Environment
Large and well-defined variations exist between the distribution of mass and the light of stars on extragalactic scales. Mass concentrations in the range 1012-1013 M☉ manifest the most light per unit
It is believed that the global baryon content of clusters of galaxies is representative of the matter distribution of the universe, and can, therefore, be used to reliably determine the
The Cosmological Mean Density and Its Local Variations Probed by Peculiar Velocities
Peculiar velocities throughout the region of the Local Supercluster are reconstructed by two different orbit-retracing methods. The requirement of optimal correlation between the radial components of
Linking halo mass to galaxy luminosity
In this paper we present a new, essentially empirical, model for the relation between the mass of a dark matter halo/subhalo and the luminosity of a galaxy hosted in it. To estimate this, we replace
Securing the Faint End of the Galaxy Luminosity Function
Abstract The history of the formation of galaxies must leave an imprint in the properties of the mass function of collapsed objects and in its observational manifestation, the galaxy luminosity
A Subhalo-Galaxy Correspondence Model of Galaxy Biasing
We propose a model for allocating galaxies in cosmological N-body simulations. We identify each subhalo with a galaxy and assign luminosity and morphological type, assuming that the galaxy luminosity
Near-Infrared Properties of Moderate-Redshift Galaxy Clusters. II. Halo Occupation Number, Mass-to-Light Ratios, and Ωm
Using K-band imaging for 15 of the Canadian Network for Observational Cosmology (CNOC1) clusters we examine the near-infrared properties of moderate-redshift (0.19 < z < 0.55) galaxy clusters. We
K-Band Properties of Galaxy Clusters and Groups: Luminosity Function, Radial Distribution, and Halo Occupation Number
We explore the near-infrared (NIR) K-band properties of galaxies within 93 galaxy clusters and groups using data from the Two Micron All Sky Survey. We use X-ray properties of these clusters to
CAIRNS: The Cluster and Infall Region Nearby Survey. II. Environmental Dependence of Infrared Mass-to-Light Ratios
CAIRNS (Cluster and Infall Region Nearby Survey) is a spectroscopic survey of the infall regions surrounding nine nearby rich clusters of galaxies. In our previous paper, we used redshifts within ~10


Evolution of the cosmological density distribution function
ABSTRA C T We present a new calculation for the evolution of the one-point probability distribution function (PDF) of the cosmological density field based on an exact statistical treatment. Using the
Evolution of one-point distributions from Gaussian initial fluctuations
We study the quasilinear evolution of the one-point probability density functions (PDFs) of the smoothed density and velocity fields in a cosmological gravitating system beginning with Gaussian
Probability Distribution Function of Cosmological Density Fluctuations from a Gaussian Initial Condition: Comparison of One-Point and Two-Point Lognormal Model Predictions with N-Body Simulations
We quantitatively study the probability distribution function (PDF) of cosmological nonlinear density fluctuations from N-body simulations with a Gaussian initial condition. In particular, we examine
A lognormal model for the cosmological mass distribution.
The use of a lognormal (LN) random field is discussed as a model for the distribution of matter in the Universe. A number of difficulties with the statistical treatment of density perturbations are
The Physical Origin of Scale-dependent Bias in Cosmological Simulations
Using a large-scale hydrodynamic simulation with heuristic criteria for galaxy formation, we investi- gate how the galaxy —eld is related to physical parameters such as the mass density and the gas
Stochastic Nonlinear Galaxy Biasing
We propose a general formalism for galaxy biasing and apply it to methods for measuring cosmological parameters, such as regression of light versus mass, the analysis of redshift distortions,
We present an estimate of the global budget of baryons in all states, with conservative estimates of the uncertainties, based on all relevant information we have been able to marshal. Most of the
Measuring the nonlinear biasing function from a galaxy redshift survey
We present a simple method for evaluating the nonlinear biasing function of galaxies from a redshift survey. The nonlinear biasing is characterized by the conditional mean of the galaxy density
Galaxy voids in cold dark matter universes
We present predictions for numerous statistics related to the presence of voids in the distribution of galaxies in a cold dark matter model of structure formation using a semi-analytic model of
Cold Dark Matter Cosmology with Hydrodynamics and Galaxy Formation: The Evolution of the Intergalactic Medium and Background Radiation Fields
We have supplemented our code, which computes the evolution of the physical state of a representative piece of the universe to include, not only the dynamics of dark matter (with a standard PM code),