Halo formation and distribution around cosmic web
Abstract
We use the ELUCID simulation to study how the local environment affects the formation of dark matter halos and their spatial distribution around the cosmic web. We describe the environment by local density and cosmic-web type. At fixed web type, the halo mass function (HMF) depends strongly on the local density, whereas at fixed density it depends only weakly, though significantly, on the web type; the character of both dependencies changes around the mean density. The halo formation redshift is primarily driven by local density rather than cosmic web. We then introduce the three-dimensional cosmic-web cross-correlation function (3D-WCCF), which expresses the distribution of halos around cosmic web in the local tidal eigenframe. The 3D-WCCF provides numerous anisotropic characteristics. Around all web types, halos are most strongly correlated along the axis of weakest compression, e3, and least along the axis of strongest compression, e1. Nearly all cluster-sized halos reside in knots and lie preferentially in the plane perpendicular to bf e1. The 3D-WCCF also provides important information on the geometry and size of filaments, sheets and voids. Moreover, early-forming halos are more strongly correlated with the web than late-forming ones, and this assembly bias is anisotropic around filaments, sheets, and voids, being strongest along e3, but nearly isotropic around knots.
Related
- Developing Environments: Formation and Quenching at Cosmic Noon Traced by the Large-scale Distribution of Gas and Galaxies
- Galactic Cosmic-Ray Transport in the Giant Circumgalactic Medium Halo
- Caught in the act: diffuse stellar and Lyα emission around a halo-less quasar in the assembling cluster CARLA J0800+4029 at z=2
- Connecting galaxy structure, quenching, and halo environments during cosmic noon
- Radial dependence of galaxy and halo properties in cosmic voids: SDSS DR7 and the ELUCID constrained simulation
BibTeX
@misc{yu2026halo,
title = {{Halo formation and distribution around cosmic web}},
author = {Hongfei Yu and Huiyuan Wang and Yangyao Chen and Ziwen Zhang and Hao Li},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.34042},
eprint = {2610.34042},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.34042},
}
RIS
TY - UNPB
TI - Halo formation and distribution around cosmic web
AU - Hongfei Yu
AU - Huiyuan Wang
AU - Yangyao Chen
AU - Ziwen Zhang
AU - Hao Li
PY - 2026
DA - 2026/10/25
PB - arXiv
DO - 10.48550/arxiv.2610.34042
UR - https://arxiv.org/abs/2610.34042
AB - We use the ELUCID simulation to study how the local environment affects the formation of dark matter halos and their spatial distribution around the cosmic web. We describe the environment by local density and cosmic-web type. At fixed web type, the halo mass function (HMF) depends strongly on the local density, whereas at fixed density it depends only weakly, though significantly, on the web type; the character of both dependencies changes around the mean density. The halo formation redshift is primarily driven by local density rather than cosmic web. We then introduce the three-dimensional cosmic-web cross-correlation function (3D-WCCF), which expresses the distribution of halos around cosmic web in the local tidal eigenframe. The 3D-WCCF provides numerous anisotropic characteristics. Around all web types, halos are most strongly correlated along the axis of weakest compression, e_3, and least along the axis of strongest compression, e_1. Nearly all cluster-sized halos reside in knots and lie preferentially in the plane perpendicular to bf e_1. The 3D-WCCF also provides important information on the geometry and size of filaments, sheets and voids. Moreover, early-forming halos are more strongly correlated with the web than late-forming ones, and this assembly bias is anisotropic around filaments, sheets, and voids, being strongest along e_3, but nearly isotropic around knots.
ER -