A cosmic filament catalog for COSMOS-Web Data Release 1 across 0.5 < z < 3.5
Abstract
Cosmic filaments represent the environments in which most galaxies form and evolve. However, the spatial distribution of filaments and the link between galaxy properties and their positions relative to filaments remains unclear, particularly at high redshifts. In this work, using the deep-field catalog COSMOS-Web Data Release 1, we construct a filament catalog spanning 0.5 < z < 3.5 that can be directly applied to studies of galaxy evolution and the galaxy--large-scale-structure connection at the peak epoch of galaxy and black hole formation. We developed a new procedure based on the DisPerSE method that fully incorporates the probability distribution functions (PDFs) of galaxy photometric redshifts by generating multiple realizations for each tomographic 2D slice. We then stacked these realizations to construct ``filament probability maps'' (w_ fil maps), from which filaments were subsequently extracted. The filament extraction parameters were optimized using mock catalogs generated from TNG simulations by minimizing the discrepancies between 3D and projected 2D filaments. Applying this procedure to the COSMOS-Web data, we detected 12,523 filaments (comprising 136,210 segments) across 0.5 < z < 3.5 and released a filament catalog, a companion segment catalog, and filament probability maps for each slice. Validation against astrophysical properties shows a strong agreement between the extracted filaments and those in the simulations, supporting the robustness of the filament extraction. These data products provide a robust foundation for investigating galaxy--environment coevolution at cosmic noon and beyond.
Versions
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BibTeX
@misc{hao2026cosmic,
title = {{A cosmic filament catalog for COSMOS-Web Data Release 1 across 0.5 < z < 3.5}},
author = {Qiaoyang Hao and Tao Wang and Weishan Zhu and Hong Guo and Peng Wang and Tiancheng Yang and Luwenjia Zhou},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.31168},
eprint = {2610.31168},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.31168},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - A cosmic filament catalog for COSMOS-Web Data Release 1 across 0.5 < z < 3.5
AU - Qiaoyang Hao
AU - Tao Wang
AU - Weishan Zhu
AU - Hong Guo
AU - Peng Wang
AU - Tiancheng Yang
AU - Luwenjia Zhou
PY - 2026
DA - 2026/10/22
PB - arXiv
DO - 10.48550/arxiv.2610.31168
UR - https://arxiv.org/abs/2610.31168
AB - Cosmic filaments represent the environments in which most galaxies form and evolve. However, the spatial distribution of filaments and the link between galaxy properties and their positions relative to filaments remains unclear, particularly at high redshifts. In this work, using the deep-field catalog COSMOS-Web Data Release 1, we construct a filament catalog spanning 0.5 < z < 3.5 that can be directly applied to studies of galaxy evolution and the galaxy--large-scale-structure connection at the peak epoch of galaxy and black hole formation. We developed a new procedure based on the DisPerSE method that fully incorporates the probability distribution functions (PDFs) of galaxy photometric redshifts by generating multiple realizations for each tomographic 2D slice. We then stacked these realizations to construct ``filament probability maps'' (w_ fil maps), from which filaments were subsequently extracted. The filament extraction parameters were optimized using mock catalogs generated from TNG simulations by minimizing the discrepancies between 3D and projected 2D filaments. Applying this procedure to the COSMOS-Web data, we detected 12,523 filaments (comprising 136,210 segments) across 0.5 < z < 3.5 and released a filament catalog, a companion segment catalog, and filament probability maps for each slice. Validation against astrophysical properties shows a strong agreement between the extracted filaments and those in the simulations, supporting the robustness of the filament extraction. These data products provide a robust foundation for investigating galaxy--environment coevolution at cosmic noon and beyond.
ER -