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Peer-reviewedCC BYAstronomy and Astrophysics

JWST COSMOS-3D: Spectroscopic census and luminosity function of [O III] emitters at 6.75 < z < 9.05 in COSMOS

  • R. A. Meyer1
  • Feige Wang2
  • Koki Kakiichi3
  • Gabe Brammer3
  • Jackie Champagne4
  • Katharina Jurk5
  • Zihao Li6,3
  • Z. X. Li6,3
  • Marat Musin6
  • Sindhu Satyavolu7
  • Jan–Torge Schindler5
  • Marko Shuntov3,8
30 more authors
  • Yi Xu3,9
  • Siwei Zou6,10
  • Fuyan Bian6,11
  • Caitlin Casey3,12
  • Eiichi Egami4
  • Xiaohui Fan4
  • Danyang Jiang13,14
  • Nicolas Laporte15
  • Weizhe Liu4
  • Pascal A. Oesch3,1
  • Lidia A. M. Tasca15
  • Jinyi Yang2
  • Zijian Zhang13,14
  • Hollis B. Akins16
  • Zheng Cai17
  • Dave A. Coulter18,19
  • Jiamu Huang12
  • Mingyu Li17
  • Weizhe Liu4
  • Yongming Liang20,9
  • Bingcheng 秉诚 Jin 金2
  • Xiangyu Jin2
  • Jeyhan S. Kartaltepe21
  • Anton M. Koekemoer19
  • Jasleen Matharu22
  • Maria Pudoka4
  • Wei Leong Tee23
  • Callum Witten1
  • Haowen Zhang24
  • Yongda Zhu4
24 affiliations
  1. 1Department of Astronomy, University of Geneva
  2. 2Department of Astronomy, University of Michigan
  3. 3Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen
  4. 4Steward Observatory, University of Arizona
  5. 5Hamburger Sternwarte, Universität Hamburg
  6. 6Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories
  7. 7Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Edifici Cn, Campus UAB
  8. 8University of Geneva, 24 rue du Général-Dufour
  9. 9National Astronomical Observatory of Japan
  10. 10Departamento de Astronomía, Universidad de Chile
  11. 11European Southern Observatory
  12. 12Department of Physics, University of California, Santa Barbara
  13. 13Department of Astronomy, School of Physics, Peking University
  14. 14Kavli Institute for Astronomy and Astrophysics, Peking University
  15. 15Aix Marseille Université, CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326
  16. 16Department of Astronomy, The University of Texas at Austin
  17. 17Department of Astronomy, Tsinghua University
  18. 18Physics and Astronomy Department, Johns Hopkins University
  19. 19Space Telescope Science Institute
  20. 20Institute for Cosmic Ray Research, The University of Tokyo
  21. 21Laboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology
  22. 22Max-Planck-Institut für Astronomie
  23. 23Department of Astronomy and Astrophysics, The Pennsylvania State University
  24. 24Canadian Institute for Theoretical Astrophysics
Open at sourceDOICite

Abstract

We present a catalogue of spectroscopically selected [O III ]+H β emitters at 6.75 < z < 9.05 and the resulting [O III ] 5008 Å luminosity function (LF) in the COSMOS field. We leveraged the 0.33 deg 2 covered by COSMOS-3D using NIRCam/WFSS F444W to perform the largest spectroscopic search for [O III ] emitters at 6.75 < z < 9.05. We present our catalogue of 249 [O III ] emitters and their associated completeness function. The inferred constraints on the [O III ] LF enabled us to characterise the knee of the [O III ] 5008 Å LF, resulting in improved [O III ] 5008 Å LF constraints at z ∼ 7, 8. Notably, we find evidence for a decline of the [O III ] luminosity density between z ∼ 6 − 8, which could be expected if the metallicity of [O III ] emitters, as well as the cosmic star-formation rate density, is declining at these redshifts. We find that theoretical models that reproduce the z ∼ 7, 8 [O III ] 5008 Å LF do not reproduce well the [O III ] equivalent width distribution, pointing to potential challenges in the modelling of [O III ] and other nebular lines in the early Universe. Finally, we provide the first constraints on the cosmic variance of [O III ] emitters, estimating at 15% the fractional uncertainty for the z ∼ 7, 8 [O III ] 5008 Å LF in the 0.33 deg 2 field. This estimate is in good agreement with that inferred from clustering, and it shows that the [O III ] 5008 Å LF derived from smaller extragalactic legacy fields is strongly affected by cosmic variance. Our results highlight the fundamental role that wide-area JWST slitless surveys play to map the galaxy large-scale structure down into the reionisation era, serving as a springboard for a variety of science cases.

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Cite

BibTeXRIS
BibTeX
@article{meyer2026jwst,
  title = {{JWST COSMOS-3D: Spectroscopic census and luminosity function of [O III] emitters at 6.75 < z < 9.05 in COSMOS}},
  author = {R. A. Meyer and Feige Wang and Koki Kakiichi and Gabe Brammer and Jackie Champagne and Katharina Jurk and Zihao Li and Z. X. Li and Marat Musin and Sindhu Satyavolu and Jan–Torge Schindler and Marko Shuntov and Yi Xu and Siwei Zou and Fuyan Bian and Caitlin Casey and Eiichi Egami and Xiaohui Fan and Danyang Jiang and Nicolas Laporte and Weizhe Liu and Pascal A. Oesch and Lidia A. M. Tasca and Jinyi Yang and Zijian Zhang and Hollis B. Akins and Zheng Cai and Dave A. Coulter and Jiamu Huang and Mingyu Li and Weizhe Liu and Yongming Liang and Bingcheng 秉诚 Jin 金 and Xiangyu Jin and Jeyhan S. Kartaltepe and Anton M. Koekemoer and Jasleen Matharu and Maria Pudoka and Wei Leong Tee and Callum Witten and Haowen Zhang and Yongda Zhu},
  journal = {Astronomy and Astrophysics},
  year = {2026},
  month = jun,
  doi = {10.1051/0004-6361/202557671},
  url = {https://doi.org/10.1051/0004-6361/202557671},
  note = {CC BY},
}
RIS
TY  - JOUR
TI  - JWST COSMOS-3D: Spectroscopic census and luminosity function of [O III] emitters at 6.75 < z < 9.05 in COSMOS
AU  - R. A. Meyer
AU  - Feige Wang
AU  - Koki Kakiichi
AU  - Gabe Brammer
AU  - Jackie Champagne
AU  - Katharina Jurk
AU  - Zihao Li
AU  - Z. X. Li
AU  - Marat Musin
AU  - Sindhu Satyavolu
AU  - Jan–Torge Schindler
AU  - Marko Shuntov
AU  - Yi Xu
AU  - Siwei Zou
AU  - Fuyan Bian
AU  - Caitlin Casey
AU  - Eiichi Egami
AU  - Xiaohui Fan
AU  - Danyang Jiang
AU  - Nicolas Laporte
AU  - Weizhe Liu
AU  - Pascal A. Oesch
AU  - Lidia A. M. Tasca
AU  - Jinyi Yang
AU  - Zijian Zhang
AU  - Hollis B. Akins
AU  - Zheng Cai
AU  - Dave A. Coulter
AU  - Jiamu Huang
AU  - Mingyu Li
AU  - Weizhe Liu
AU  - Yongming Liang
AU  - Bingcheng 秉诚 Jin 金
AU  - Xiangyu Jin
AU  - Jeyhan S. Kartaltepe
AU  - Anton M. Koekemoer
AU  - Jasleen Matharu
AU  - Maria Pudoka
AU  - Wei Leong Tee
AU  - Callum Witten
AU  - Haowen Zhang
AU  - Yongda Zhu
PY  - 2026
DA  - 2026/06/24
JO  - Astronomy and Astrophysics
DO  - 10.1051/0004-6361/202557671
UR  - https://doi.org/10.1051/0004-6361/202557671
AB  - We present a catalogue of spectroscopically selected [O III ]+H β emitters at 6.75 < z < 9.05 and the resulting [O III ] 5008 Å luminosity function (LF) in the COSMOS field. We leveraged the 0.33 deg 2 covered by COSMOS-3D using NIRCam/WFSS F444W to perform the largest spectroscopic search for [O III ] emitters at 6.75 < z < 9.05. We present our catalogue of 249 [O III ] emitters and their associated completeness function. The inferred constraints on the [O III ] LF enabled us to characterise the knee of the [O III ] 5008 Å LF, resulting in improved [O III ] 5008 Å LF constraints at z ∼ 7, 8. Notably, we find evidence for a decline of the [O III ] luminosity density between z ∼ 6 − 8, which could be expected if the metallicity of [O III ] emitters, as well as the cosmic star-formation rate density, is declining at these redshifts. We find that theoretical models that reproduce the z ∼ 7, 8 [O III ] 5008 Å LF do not reproduce well the [O III ] equivalent width distribution, pointing to potential challenges in the modelling of [O III ] and other nebular lines in the early Universe. Finally, we provide the first constraints on the cosmic variance of [O III ] emitters, estimating at 15% the fractional uncertainty for the z ∼ 7, 8 [O III ] 5008 Å LF in the 0.33 deg 2 field. This estimate is in good agreement with that inferred from clustering, and it shows that the [O III ] 5008 Å LF derived from smaller extragalactic legacy fields is strongly affected by cosmic variance. Our results highlight the fundamental role that wide-area JWST slitless surveys play to map the galaxy large-scale structure down into the reionisation era, serving as a springboard for a variety of science cases.
SN  - 0004-6361
SN  - 1432-0746
ER  -