Galaxy and Halo Assembly Bias in Alternative Dark Matter Models
Abstract
The clustering of dark matter halos depends not only on halo mass but also on secondary halo properties, a phenomenon known as halo assembly bias. Coupled with variations in halo occupation, this dependence impacts galaxy clustering, an effect termed galaxy assembly bias. While previous studies have found only weak cosmological dependence of assembly bias within the ΛCDM framework, its sensitivity to the underlying dark matter physics remains largely unexplored. We use the matched dark-matter-only and hydrodynamical simulations from the AIDA-TNG suite to measure assembly bias across four dark matter models: cold dark matter, warm dark matter, and self-interacting dark matter with constant cross-sections and velocity-dependent cross-sections. We find that at z = 0, halo assembly bias is nearly identical across the four models for concentration-selected halos, as is the concentration dependence of the halo occupation distribution. The resulting galaxy assembly bias signals likewise show only weak model dependence. For stellar-mass-selected galaxy samples with n = 0.0586 h3 Mpc−3 at z = 0, the velocity-dependent self-interacting dark matter scenario exhibits the largest deviation from the fiducial cold dark matter model: its assembly bias contribution to galaxy clustering is enhanced by up to ∼ 6%, corresponding to a ∼ 3% difference in the assembly bias amplitude. Although statistically distinguishable, this difference is small and unlikely to be detected in current analyses. The weak model dependence persists across different galaxy number densities and redshifts. Overall, within the TNG galaxy-formation framework, these results indicate that assembly bias is largely insensitive to the dark matter models explored here, providing a robust baseline for future studies of the galaxy-halo connection in alternative dark matter scenarios.
Related
- The Role of Cluster Environments in Quiescent Galaxy Stellar Halo Assembly
- A Graph Attention Network Framework for Simultaneous Prediction of Galaxy and Dark Matter Halo Properties in GAMA DR4
- The Contribution of Mergers and Accretion to Dark Matter Halo Assembly: An Excursion Set Theory Approach
- Correlation between baryonic process and galaxy assembly bias
- JADES: Dynamical Measurements of Dark Matter Halo Masses at z ≈ 7 Using Galaxy Pairs
BibTeX
@misc{wang2026galaxy,
title = {{Galaxy and Halo Assembly Bias in Alternative Dark Matter Models}},
author = {Yikun Wang and Idit Zehavi and Sergio Contreras and Jonás Chaves-Montero and Giulia Despali and Carlo Giocoli and Lauro Moscardini and Massimiliano Romanello and Mark Vogelsberger},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.32086},
eprint = {2609.32086},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.32086},
}
RIS
TY - UNPB
TI - Galaxy and Halo Assembly Bias in Alternative Dark Matter Models
AU - Yikun Wang
AU - Idit Zehavi
AU - Sergio Contreras
AU - Jonás Chaves-Montero
AU - Giulia Despali
AU - Carlo Giocoli
AU - Lauro Moscardini
AU - Massimiliano Romanello
AU - Mark Vogelsberger
PY - 2026
DA - 2026/09/25
PB - arXiv
DO - 10.48550/arxiv.2609.32086
UR - https://arxiv.org/abs/2609.32086
AB - The clustering of dark matter halos depends not only on halo mass but also on secondary halo properties, a phenomenon known as halo assembly bias. Coupled with variations in halo occupation, this dependence impacts galaxy clustering, an effect termed galaxy assembly bias. While previous studies have found only weak cosmological dependence of assembly bias within the ΛCDM framework, its sensitivity to the underlying dark matter physics remains largely unexplored. We use the matched dark-matter-only and hydrodynamical simulations from the AIDA-TNG suite to measure assembly bias across four dark matter models: cold dark matter, warm dark matter, and self-interacting dark matter with constant cross-sections and velocity-dependent cross-sections. We find that at z = 0, halo assembly bias is nearly identical across the four models for concentration-selected halos, as is the concentration dependence of the halo occupation distribution. The resulting galaxy assembly bias signals likewise show only weak model dependence. For stellar-mass-selected galaxy samples with n = 0.0586 h^3 Mpc^−3 at z = 0, the velocity-dependent self-interacting dark matter scenario exhibits the largest deviation from the fiducial cold dark matter model: its assembly bias contribution to galaxy clustering is enhanced by up to ∼ 6%, corresponding to a ∼ 3% difference in the assembly bias amplitude. Although statistically distinguishable, this difference is small and unlikely to be detected in current analyses. The weak model dependence persists across different galaxy number densities and redshifts. Overall, within the TNG galaxy-formation framework, these results indicate that assembly bias is largely insensitive to the dark matter models explored here, providing a robust baseline for future studies of the galaxy-halo connection in alternative dark matter scenarios.
ER -