# Revealing the cosmic web dependent halo bias

## TL;DR

This paper investigates how the clustering bias of dark matter halos varies across different cosmic web environments, revealing significant environmental dependence that impacts cosmological and galaxy formation models.

## Contribution

It introduces a detailed analysis of halo bias dependence on cosmic web environments using high-resolution simulations, highlighting environment-specific variations.

## Key findings

- Halos in clusters have lower biases in the 10^{11} to 10^{13.5} h^{-1} M_sun range.
- Halos in voids show up to 10 times higher bias for ~10^{12} h^{-1} M_sun halos.
- Halo bias dependence on age is significant only in clusters and filaments for small halos.

## Abstract

Halo bias is the one of the key ingredients of the halo models. It was shown at a given redshift to be only dependent, to the first order, on the halo mass. In this study, four types of cosmic web environments: clusters, filaments, sheets and voids are defined within a state of the art high resolution $N$-body simulation. Within those environments, we use both halo-dark matter cross-correlation and halo-halo auto correlation functions to probe the clustering properties of halos. The nature of the halo bias differs strongly among the four different cosmic web environments we describe. With respect to the overall population, halos in clusters have significantly lower biases in the {$10^{11.0}\sim 10^{13.5}h^{-1}\rm M_\odot$} mass range. In other environments however, halos show extremely enhanced biases up to a factor 10 in voids for halos of mass {$\sim 10^{12.0}h^{-1}\rm M_\odot$}. Such a strong cosmic web environment dependence in the halo bias may play an important role in future cosmological and galaxy formation studies. Within this cosmic web framework, the age dependency of halo bias is found to be only significant in clusters and filaments for relatively small halos $\la 10^{12.5}\msunh$.