Precision measurement of the local bias of dark matter halos

@article{Lazeyras2015PrecisionMO,
  title={Precision measurement of the local bias of dark matter halos},
  author={Titouan Lazeyras and Christian Wagner and Tobias Baldauf and Fabian Schmidt},
  journal={Journal of Cosmology and Astroparticle Physics},
  year={2015},
  volume={2016},
  pages={018 - 018}
}
We present accurate measurements of the linear, quadratic, and cubic local bias of dark matter halos, using curved “separate universe” N-body simulations which effectively incorporate an infinite-wavelength overdensity. This can be seen as an exact implementation of the peak-background split argument. We compare the results with the linear and quadratic bias measured from the halo-matter power spectrum and bispectrum, and find good agreement. On the other hand, the standard peak-background… 
Large-scale assembly bias of dark matter halos
We present precise measurements of the assembly bias of dark matter halos, i.e. the dependence of halo bias on other properties than the mass, using curved “separate universe” N-body simulations
Squeezing the halo bispectrum: a test of bias models
We study the halo-matter cross bispectrum in the presence of primordial non-Gaussianity of the local type. We restrict ourselves to the squeezed limit, for which the calculation are straightforward,
Beyond LIMD bias: a measurement of the complete set of third-order halo bias parameters
We present direct measurements of cubic bias parameters of dark matter halos from the halo-matter-matter-matter trispectrum. We measure this statistic efficiently by cross-correlating the halo field
Assembly bias in quadratic bias parameters of dark matter halos from forward modeling
We use the forward modeling approach to galaxy clustering combined with the likelihood from the effective-field theory of large-scale structure to measure assembly bias, i.e. the dependence of halo
A robust measurement of the first higher-derivative bias of dark matter halos
We present a new simulation technique in which any chosen mode k of the density contrast field can be amplified by an amplitude Δ. These amplified-mode simulations allow us to study the response of
Renormalization of linear halo bias in N-body simulations
The interpretation of redshift surveys requires modelling the relationship between large-scale fluctuations in the observed number density of tracers, δh, and the underlying matter density, δ. Bias
Linear and non-linear bias: predictions versus measurements
We study the linear and non-linear bias parameters which determine the mapping between the distributions of galaxies and the full matter density fields, comparing different measurements and
A fully Lagrangian, non-parametric bias model for dark matter halos
We present a non-parametric Lagrangian biasing model and fit the ratio of the halo and mass densities at the field level using the mass-weighted halo field in the AbacusSummit simulations at z=0.5.
Measurement of Void Bias Using Separate Universe Simulations
Cosmic voids are biased tracers of the large-scale structure of the universe. Separate universe simulations (SUS) enable accurate measurements of this biasing relation by implementing the
Primordial non-Gaussianity from biased tracers: likelihood analysis of real-space power spectrum and bispectrum
Upcoming galaxy redshift surveys promise to significantly improve current limits on primordial non-Gaussianity (PNG) through measurements of 2- and 3-point correlation functions in Fourier space.
...
...

References

SHOWING 1-10 OF 52 REFERENCES
THE LARGE-SCALE BIAS OF DARK MATTER HALOS: NUMERICAL CALIBRATION AND MODEL TESTS
We measure the clustering of dark matter halos in a large set of collisionless cosmological simulations of the flat ΛCDM cosmology. Halos are identified using the spherical overdensity algorithm,
The local bias model in the large-scale halo distribution
We explore the biasing in the clustering statistics of haloes as compared to dark matter (DM) in simulations. We look at the second- and third-order statistics at large scales of the (intermediate)
Large-scale bias and the inaccuracy of the peak-background split
The peak-background split argument is commonly used to relate the abundance of dark matter haloes to their spatial clustering. Testing this argument requires an accurate determination of the halo
Linear response to long wavelength fluctuations using curvature simulations
We study the local response to long wavelength fluctuations in cosmological N-body simulations, focusing on the matter and halo power spectra, halo abundance and non-linear transformations of the
The assembly bias of dark matter haloes to higher orders
We use an extremely large volume (2.4h 3 Gpc 3 ), high resolution N-body simulation to measure the higher order clustering of dark matter haloes as a function of mass and internal structure. As a
Large scale bias and the peak background split
Dark matter haloes are biased tracers of the underlying dark matter distribution. We use a simple model to provide a relation between the abundance of dark matter haloes and their spatial
Separate universe consistency relation and calibration of halo bias
Linear halo bias is the response of dark matter halo number density to a long wavelength fluctuation in the dark matter density. Using abundance matching between separate universe simulations which
Understanding Higher-Order Nonlocal Halo Bias at Large Scales by Combining the Power Spectrum with the Bispectrum
Understanding the relation between underlying matter distribution and biased tracers such as galaxy or dark matter halo is essential to extract cosmological information from ongoing or future galaxy
Peak-background split, renormalization, and galaxy clustering
We present a derivation of two-point correlations of general tracers in the peak-background split (PBS) framework by way of a rigorous definition of the PBS argument. Our expressions only depend on
An analytic model for the spatial clustering of dark matter haloes
We develop a simple analytic model for the gravitational clustering of dark matter haloes to understand how their spatial distribution is biased relative to that of the mass. The statistical
...
...