Evidence for quadratic tidal tensor bias from the halo bispectrum

@article{Baldauf2012EvidenceFQ,
  title={Evidence for quadratic tidal tensor bias from the halo bispectrum},
  author={Tobias Baldauf and Uros Seljak and Vincent Desjacques and Patrick Mcdonald},
  journal={Physical Review D},
  year={2012},
  volume={86},
  pages={083540}
}
The relation between the clustering properties of luminous matter in the form of galaxies and the underlying dark matter distribution is of fundamental importance for the interpretation of ongoing and upcoming galaxy surveys. The so-called local bias model, where galaxy density is a function of local matter density, is frequently discussed as a means to infer the matter power spectrum or correlation function from the measured galaxy correlation. However, gravitational evolution generates a term… 

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References

SHOWING 1-10 OF 61 REFERENCES

Gravity and Large-Scale Nonlocal Bias

The relationship between galaxy and matter overdensities, bias, is most often assumed to be local. This is however unstable under time evolution, we provide proofs under several sets of assumptions.

Clustering of dark matter tracers: Renormalizing the bias parameters

A commonly used perturbative method for computing large-scale clustering of tracers of mass density, like galaxies, is to model the tracer density field as a Taylor series in the local smoothed mass

Clustering of dark matter tracers: generalizing bias for the coming era of precision LSS

On very large scales, density fluctuations in the Universe are small, suggesting a perturbative model for large-scale clustering of galaxies (or other dark matter tracers), in which the galaxy

Large-scale bias in the Universe: bispectrum method

Evidence that the Universe may be close to the critical density, required for its expansion eventually to be halted, comes principally from dynamical studies of large-scale structure. These studies

Modeling Scale-Dependent Bias on the Baryonic Acoustic Scale with the Statistics of Peaks of Gaussian Random Fields

Models of galaxy and halo clustering commonly assume that the tracers can be treated as a continuous field locally biased with respect to the underlying mass distribution. In the peak model pioneered

Calibrating the baryon oscillation ruler for matter and halos

We characterize the nonlinear evolution of the baryon acoustic feature as traced by the dark matter and halos, using a combination of perturbation theory and N-body simulations. We confirm that the

Clipping the cosmos: the bias and bispectrum of large scale structure.

The results strongly suggest that this method increases the range of scales where the relation between the bispectrum and power spectrum in tree-level perturbation theory may be applied, from k(max) ∼ 0.1 to ∼0.7 hMpc(-1), which leads to correspondingly large improvements in the determination of galaxy bias.

Minimizing the stochasticity of halos in large-scale structure surveys

In recent work (Seljak, Hamaus, and Desjacques 2009) it was found that weighting central halo galaxies by halo mass can significantly suppress their stochasticity relative to the dark matter, well

Two ways of biasing galaxy formation

We calculate the galaxy bispectrum in both real and redshift space, adopting the most common prescriptions for local Eulerian biasing and the Lagrangian evolving-bias model. We show that the two

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
...