Modeling the clustering of dark-matter haloes in resummed perturbation theories

Understand

We address the issue of the cosmological bias between matter and galaxy distributions, looking at dark-matter haloes as a first step to characterize galaxy clustering.

• Starting from the linear density field at high redshift, we follow the centre of mass trajectory of the material that will form each halo at late times (proto-halo).
• We adopt a fluid-like description for the evolution of perturbations in the proto-halo distribution, which is coupled to the matter density field via gravity.
• We present analytical solutions for the density and velocity fields, in the context of renormalized perturbation theory.