The Role of the Cosmic Web in Galaxy Evolution Across 0.4<z<4

@misc{taamoli2026role,
  title = {{The Role of the Cosmic Web in Galaxy Evolution Across 0.4<z<4}},
  author = {Sina Taamoli and Bahram Mobasher and Hossein Hatamnia and Nima Chartab and John R. Weaver and Ghassem Gozaliasl and Anton M. Koekemoer and Caitlin M. Casey and Jeyhan S. Kartaltepe and Aryana Haghjoo and Olivier Ilbert and Henry J. McCracken and David B. Sanders and Nicholas Scoville and Sune Toft},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.07710},
  eprint = {2610.07710},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.07710},
}

TY  - UNPB
TI  - The Role of the Cosmic Web in Galaxy Evolution Across 0.4<z<4
AU  - Sina Taamoli
AU  - Bahram Mobasher
AU  - Hossein Hatamnia
AU  - Nima Chartab
AU  - John R. Weaver
AU  - Ghassem Gozaliasl
AU  - Anton M. Koekemoer
AU  - Caitlin M. Casey
AU  - Jeyhan S. Kartaltepe
AU  - Aryana Haghjoo
AU  - Olivier Ilbert
AU  - Henry J. McCracken
AU  - David B. Sanders
AU  - Nicholas Scoville
AU  - Sune Toft
PY  - 2026
DA  - 2026/10/06
PB  - arXiv
DO  - 10.48550/arxiv.2610.07710
UR  - https://arxiv.org/abs/2610.07710
AB  - We investigate the dependence of stellar mass and star formation activity on the topology of hosting large-scale structures using mass-complete galaxy samples in four redshift bins spanning from z = 0.4 to z = 4 using the COSMOS2020 catalog. Cosmic web components (clusters, filaments, and field) are identified by applying the Multiscale Morphology Filter to galaxy density maps, and group memberships (central, satellite, isolated) are assigned to each galaxy by the Friends of Friends (FoF) algorithm. Out to z < 1, we find that stellar mass increases toward denser structures, driven primarily by central and satellite galaxies, with differences up to ~0.35 dex between field and clusters. At these redshifts, star formation rate (SFR) is suppressed by ~0.1 dex in clusters compared to field galaxies, particularly for centrals, while the SFR of star-forming galaxies shows a much weaker dependence on the type of host structure, indicating that the quenched population primarily drives the observed environmental dependence. Specific SFR (sSFR) shows the strongest decline for centrals in clusters at z<1, consistent with enhanced quenching in dense environments. At 1<z<2, star formation activity becomes largely independent of environment, suggesting a transitional regime in the role of large-scale structure. At z>2, we observe a mild increase in SFR (~+0.1 dex) and sSFR (~+0.13 dex) from field to cluster galaxies, pointing to a possible reversal of environmental trends during early cosmic epochs. These results highlight the evolving influence of environment on galaxy evolution and set the stage for deeper investigations with upcoming wide-field surveys.
ER  -