An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5

Jun Toshikawa; Stijn Wuyts; Nobunari Kashikawa; Chengze Liu; Marcin Sawicki; Roderik Overzier; Mariko Kubo; Hisakazu Uchiyama; Kei Ito; Malcolm Bremer; Yoshiaki Ono; Tadayuki Kodama; Yen-Ting Lin; Tomoki Saito

doi:10.1093/mnras/stad3162

An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5

Jun Toshikawa, Stijn Wuyts, Nobunari Kashikawa, Chengze Liu, Marcin Sawicki, Roderik Overzier, Mariko Kubo, Hisakazu Uchiyama, Kei Ito, Malcolm Bremer, Yoshiaki Ono, Tadayuki Kodama, Yen-Ting Lin, Tomoki Saito

Department of Physics

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Abstract

We present a protocluster search covering z ∼3 to z ∼5 based on the combination of the Hyper SuprimeCam Subaru Strategic Programme and the CFHT Large Area U-band Deep Survey. We identify about 30 protocluster candidates per unit redshift over the area of the Deep/UltraDeep layer. Protocluster candidates are selected as regions with a significantly enhanced surface density of dropout galaxies. With this large sample, we characterize the properties of their individual member galaxies. We compare the number counts of dropout galaxies in protocluster candidates with that of coeval field galaxies. Rest-frame ultraviolet (UV) bright galaxies are overabundant in protocluster candidates, a trend seen across the full redshift range studied. We do not find evidence for their spatial distribution within protocluster candidates to be distinct from their fainter counterparts, nor for their UV colour to be different from that of field galaxies with the same brightness. Cosmological simulations predict this bright-end excess, with the main cause being a richer population of massive galaxies, with only a minor contribution from an enhancement in star formation activity (and therefore UV emission) at fixed mass. U-to-K SED modelling of our observed samples supports this interpretation. This environmental differentiation in number counts is already in place at z ∼5, with no significant redshift dependence over the range in lookback times probed. These observational results and model predictions suggest that the cosmic clock is ahead in high-density environments.

Original language	English
Article number	stad3162
Pages (from-to)	6276-6291
Number of pages	16
Journal	Monthly Notices of the Royal Astronomical Society
Volume	527
Issue number	3
Early online date	14 Oct 2023
DOIs	https://doi.org/10.1093/mnras/stad3162
Publication status	Published - 31 Jan 2024

Bibliographical note

ACKNOWLEDGEMENTS
We thank the anonymous referee for valuable comments and suggestions that improved the manuscript. JT and SW acknowledge support from STFC through grant ST/T000449/1. CL acknowledges support from the National Natural Science Foundation of China (NSFC, Grant No. 12173025, 11833005, 11933003), 111 project (No. B20019), and Key Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry of Education. MK acknowledges supports from JSPS KAKENHI Grant Numbers 20K14530 & 21H044902 and Tohoku University Center for Gender Equality Promotion (TUMUG). TK acknowledges financial support from JSPS KAKENHI Grant Number 18H03717. The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the
Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope (LSST). We thank the LSST Project for making their code available as free software at http://dm.lsst.org. These data were obtained and processed as part of the CFHT Large Area U-band Deep Survey (CLAUDS), which is a collaboration between astronomers from Canada, France, and China described in Sawicki et al. (2019). CLAUDS is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii CLAUDS uses data obtained in part through the Telescope Access Program (TAP), which has been funded by the National Astronomical Observatories, Chinese Academy of Sciences, and the Special Fund for Astronomy from the Ministry of Finance of China. CLAUDS uses data products from TERAPIX and the Canadian Astronomy Data Centre (CADC) and was carried out using resources from Compute Canada and Canadian Advanced Network For Astrophysical Research (CANFAR).

DATA AVAILABILITY: The data underlying this article will be shared on reasonable request to the corresponding author.

Funding

We thank the anonymous referee for valuable comments and suggestions that improved the manuscript. JT and SW acknowledge support from Science and Technology Facilities Council (STFC) through grant ST/T000449/1. CL acknowledges support from the National Natural Science Foundation of China (NSFC, grant numbers 12173025, 11833005, 11933003), 111 project (no. B20019), and Key Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry of Education. MK acknowledges supports from Japan Society for the Promotion of Science (JSPS) KAKENHI grant numbers 20K14530 and 21H044902 and Tohoku University Center for Gender Equality Promotion (TUMUG). TK acknowledges financial support from JSPS KAKENHI grant number 18H03717. The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope (LSST). We thank the LSST Project for making their code available as free software at http://dm.lsst.org . These data were obtained and processed as part of the CFHT Large Area U-band Deep Survey (CLAUDS), which is a collaboration between astronomers from Canada, France, and China described in Sawicki et al. (). CLAUDS is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. CLAUDS uses data obtained in part through the Telescope Access Program (TAP), which has been funded by the National Astronomical Observatories, Chinese Academy of Sciences, and the Special Fund for Astronomy from the Ministry of Finance of China. CLAUDS uses data products from TERAPIX and the Canadian Astronomy Data Centre (CADC) and was carried out using resources from Compute Canada and Canadian Advanced Network For Astrophysical Research (CANFAR).

Funders	Funder number
ASIAA
Kavli IPMU
Ministry of Finance of China
Princeton University
Science and Technology Facilities Council	ST/T000449/1
Japan Society for the Promotion of Science	21H044902, 20K14530
Ministry of Education, Culture, Sports, Science and Technology
National Natural Science Foundation of China	12173025, 11833005, 11933003
Japan Science and Technology Agency
National Astronomical Observatory of Japan
High Energy Accelerator Research Organization
Tohoku University Center for Gender Equality Promotion	18H03717
Higher Education Discipline Innovation Project
National Astronomical Observatories, Chinese Academy of Sciences
Toray Science Foundation

Keywords

galaxies: evolution
galaxies: high-redshift

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1093/mnras/stad3162Licence: CC BY

https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stad3162/7317707Licence: CC BY

Cite this

Toshikawa, J., Wuyts, S., Kashikawa, N., Liu, C., Sawicki, M., Overzier, R., Kubo, M., Uchiyama, H., Ito, K., Bremer, M., Ono, Y., Kodama, T., Lin, Y.-T., & Saito, T. (2024). An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5. Monthly Notices of the Royal Astronomical Society, 527(3), 6276-6291. Article stad3162. https://doi.org/10.1093/mnras/stad3162

Toshikawa, J, Wuyts, S, Kashikawa, N, Liu, C, Sawicki, M, Overzier, R, Kubo, M, Uchiyama, H, Ito, K, Bremer, M, Ono, Y, Kodama, T, Lin, Y-T & Saito, T 2024, 'An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5', Monthly Notices of the Royal Astronomical Society, vol. 527, no. 3, stad3162, pp. 6276-6291. https://doi.org/10.1093/mnras/stad3162

@article{585c845ec034439d97ed5b590d318790,

title = "An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5",

abstract = "We present a protocluster search covering z ∼3 to z ∼5 based on the combination of the Hyper SuprimeCam Subaru Strategic Programme and the CFHT Large Area U-band Deep Survey. We identify about 30 protocluster candidates per unit redshift over the area of the Deep/UltraDeep layer. Protocluster candidates are selected as regions with a significantly enhanced surface density of dropout galaxies. With this large sample, we characterize the properties of their individual member galaxies. We compare the number counts of dropout galaxies in protocluster candidates with that of coeval field galaxies. Rest-frame ultraviolet (UV) bright galaxies are overabundant in protocluster candidates, a trend seen across the full redshift range studied. We do not find evidence for their spatial distribution within protocluster candidates to be distinct from their fainter counterparts, nor for their UV colour to be different from that of field galaxies with the same brightness. Cosmological simulations predict this bright-end excess, with the main cause being a richer population of massive galaxies, with only a minor contribution from an enhancement in star formation activity (and therefore UV emission) at fixed mass. U-to-K SED modelling of our observed samples supports this interpretation. This environmental differentiation in number counts is already in place at z ∼5, with no significant redshift dependence over the range in lookback times probed. These observational results and model predictions suggest that the cosmic clock is ahead in high-density environments.",

keywords = "galaxies: evolution, galaxies: high-redshift",

author = "Jun Toshikawa and Stijn Wuyts and Nobunari Kashikawa and Chengze Liu and Marcin Sawicki and Roderik Overzier and Mariko Kubo and Hisakazu Uchiyama and Kei Ito and Malcolm Bremer and Yoshiaki Ono and Tadayuki Kodama and Yen-Ting Lin and Tomoki Saito",

note = "ACKNOWLEDGEMENTS We thank the anonymous referee for valuable comments and suggestions that improved the manuscript. JT and SW acknowledge support from STFC through grant ST/T000449/1. CL acknowledges support from the National Natural Science Foundation of China (NSFC, Grant No. 12173025, 11833005, 11933003), 111 project (No. B20019), and Key Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry of Education. MK acknowledges supports from JSPS KAKENHI Grant Numbers 20K14530 & 21H044902 and Tohoku University Center for Gender Equality Promotion (TUMUG). TK acknowledges financial support from JSPS KAKENHI Grant Number 18H03717. The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope (LSST). We thank the LSST Project for making their code available as free software at http://dm.lsst.org. These data were obtained and processed as part of the CFHT Large Area U-band Deep Survey (CLAUDS), which is a collaboration between astronomers from Canada, France, and China described in Sawicki et al. (2019). CLAUDS is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l{\textquoteright}Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii CLAUDS uses data obtained in part through the Telescope Access Program (TAP), which has been funded by the National Astronomical Observatories, Chinese Academy of Sciences, and the Special Fund for Astronomy from the Ministry of Finance of China. CLAUDS uses data products from TERAPIX and the Canadian Astronomy Data Centre (CADC) and was carried out using resources from Compute Canada and Canadian Advanced Network For Astrophysical Research (CANFAR). DATA AVAILABILITY: The data underlying this article will be shared on reasonable request to the corresponding author.",

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N2 - We present a protocluster search covering z ∼3 to z ∼5 based on the combination of the Hyper SuprimeCam Subaru Strategic Programme and the CFHT Large Area U-band Deep Survey. We identify about 30 protocluster candidates per unit redshift over the area of the Deep/UltraDeep layer. Protocluster candidates are selected as regions with a significantly enhanced surface density of dropout galaxies. With this large sample, we characterize the properties of their individual member galaxies. We compare the number counts of dropout galaxies in protocluster candidates with that of coeval field galaxies. Rest-frame ultraviolet (UV) bright galaxies are overabundant in protocluster candidates, a trend seen across the full redshift range studied. We do not find evidence for their spatial distribution within protocluster candidates to be distinct from their fainter counterparts, nor for their UV colour to be different from that of field galaxies with the same brightness. Cosmological simulations predict this bright-end excess, with the main cause being a richer population of massive galaxies, with only a minor contribution from an enhancement in star formation activity (and therefore UV emission) at fixed mass. U-to-K SED modelling of our observed samples supports this interpretation. This environmental differentiation in number counts is already in place at z ∼5, with no significant redshift dependence over the range in lookback times probed. These observational results and model predictions suggest that the cosmic clock is ahead in high-density environments.

AB - We present a protocluster search covering z ∼3 to z ∼5 based on the combination of the Hyper SuprimeCam Subaru Strategic Programme and the CFHT Large Area U-band Deep Survey. We identify about 30 protocluster candidates per unit redshift over the area of the Deep/UltraDeep layer. Protocluster candidates are selected as regions with a significantly enhanced surface density of dropout galaxies. With this large sample, we characterize the properties of their individual member galaxies. We compare the number counts of dropout galaxies in protocluster candidates with that of coeval field galaxies. Rest-frame ultraviolet (UV) bright galaxies are overabundant in protocluster candidates, a trend seen across the full redshift range studied. We do not find evidence for their spatial distribution within protocluster candidates to be distinct from their fainter counterparts, nor for their UV colour to be different from that of field galaxies with the same brightness. Cosmological simulations predict this bright-end excess, with the main cause being a richer population of massive galaxies, with only a minor contribution from an enhancement in star formation activity (and therefore UV emission) at fixed mass. U-to-K SED modelling of our observed samples supports this interpretation. This environmental differentiation in number counts is already in place at z ∼5, with no significant redshift dependence over the range in lookback times probed. These observational results and model predictions suggest that the cosmic clock is ahead in high-density environments.

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An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

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Astrophysics at the University of Bath 2020-2023

Cite this

An enhanced abundance of bright galaxies in protocluster candidates at z ∼ 3-5

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Projects

Astrophysics at the University of Bath 2020-2023

Cite this