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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

The connection between massive galaxies and their dark matter haloes from z = 0.25 to z ∼ 4 from the combined COSMOS, XMM-LSS and ECDF-S fields

  • N Stylianou1
  • Matt J Jarvis1,2
  • R G Varadaraj1
  • P W Hatfield1
  • J Hamlett1
  • C L Hale1,3
  • T Yasin1
  1. 1University of Oxford Astrophysics, Department of Physics, , Keble Road, Oxford OX1 3RH ,
  2. 2University of the Western Cape Department of Physics, , Bellville 7535, Cape Town ,
  3. 3Institute for Astronomy, University of Edinburgh , Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ ,
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Abstract

Understanding how galaxies populate and grow within dark matter haloes is essential for linking the observed evolution of galaxies to the hierarchical growth of structure. We present a galaxy clustering analysis using optical and near-infrared data from the UltraVISTA and VIDEO surveys covering 9.3 deg2 across the COSMOS, XMM-LSS and ECDF-S fields, ∼5 × larger than previous comparable studies, providing sufficient volume to determine the halo occupation of the most massive galaxies to z ∼ 4. We measure the angular two-point correlation function for stellar-mass-selected galaxies over 0.25 < z < 4 and by combining the three fields, we reduce the cosmic variance by a factor of ∼2 compared to the individual fields. The stellar-to-halo mass ratio peaks at a halo mass of Mh ≈ 1012 M⊙ and is a maximum at z ∼ 1. For the most massive galaxies, the peak halo mass (Mhpeak) increases from z = 1 → 0, while the peak stellar mass in such haloes remains approximately constant, indicating that at z < 1 massive galaxy formation becomes less efficient. We also find a steady increase in the satellite fraction since z ∼ 1, from which we infer that massive halos continue to grow hierarchically while their central galaxies experience suppressed stellar-mass growth. We suggest this is due to the central massive galaxies having their growth controlled by feedback from active galactic nuclei feedback, likely from low-power stochastic radio emission.

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Cite

BibTeXRIS
BibTeX
@article{stylianou2026connection,
  title = {{The connection between massive galaxies and their dark matter haloes from z = 0.25 to z ∼ 4 from the combined COSMOS, XMM-LSS and ECDF-S fields}},
  author = {N Stylianou and Matt J Jarvis and R G Varadaraj and P W Hatfield and J Hamlett and C L Hale and T Yasin},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag1966},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1966/8943800},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - The connection between massive galaxies and their dark matter haloes from z = 0.25 to z ∼ 4 from the combined COSMOS, XMM-LSS and ECDF-S fields
AU  - N Stylianou
AU  - Matt J Jarvis
AU  - R G Varadaraj
AU  - P W Hatfield
AU  - J Hamlett
AU  - C L Hale
AU  - T Yasin
PY  - 2026
DA  - 2026/10/19
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1966
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1966/8943800
AB  - Understanding how galaxies populate and grow within dark matter haloes is essential for linking the observed evolution of galaxies to the hierarchical growth of structure. We present a galaxy clustering analysis using optical and near-infrared data from the UltraVISTA and VIDEO surveys covering 9.3 deg2 across the COSMOS, XMM-LSS and ECDF-S fields, ∼5 × larger than previous comparable studies, providing sufficient volume to determine the halo occupation of the most massive galaxies to z ∼ 4. We measure the angular two-point correlation function for stellar-mass-selected galaxies over 0.25 < z < 4 and by combining the three fields, we reduce the cosmic variance by a factor of ∼2 compared to the individual fields. The stellar-to-halo mass ratio peaks at a halo mass of Mh ≈ 1012 M⊙ and is a maximum at z ∼ 1. For the most massive galaxies, the peak halo mass (M_h^peak) increases from z = 1 → 0, while the peak stellar mass in such haloes remains approximately constant, indicating that at z < 1 massive galaxy formation becomes less efficient. We also find a steady increase in the satellite fraction since z ∼ 1, from which we infer that massive halos continue to grow hierarchically while their central galaxies experience suppressed stellar-mass growth. We suggest this is due to the central massive galaxies having their growth controlled by feedback from active galactic nuclei feedback, likely from low-power stochastic radio emission.
SN  - 0035-8711
SN  - 1365-2966
ER  -