Galaxy clusters in the VIDEO fields: detection and characterisation in the context of MOONRISE
Abstract
We analyse the cluster content of the ∼ 4.5 deg2 XMM-LSS and CDFS VIDEO fields which are expected to be partially covered by the upcoming MOONRISE survey. Using AMICO and WaZP photometric redshift-based cluster finders, we construct a sample of $519$ cluster candidates detected by both finders in the redshift range z = 0.1−3, including $74$ detections at z > 1.5. For all detections, we identify the Brightest Central Galaxy (BCG) and compute a list of probabilistic cluster memberships. Our photometric redshift measurements of the clusters agree well with spectroscopic redshifts from the literature, when available. From ancillary spectroscopic data, we assign zspec measurements to $116$ cluster candidates based on their spectroscopic members and to $204$ based on their likely BCGs. We also show that candidates containing Radio-Loud members are efficiently recovered using the prior-based cluster finder PPM. We perform a preliminary analysis of the galaxy content of these candidates, focusing on the Red-Sequence components of their apparent Colour-Magnitude Diagram. By comparing with models of galaxy evolution, we show that this population is consistent with a model of passive evolution with a formation at high redshift, and is already in place at z = 1.5−2.0. Finally, our cluster sample is used to evaluate how these clusters would be detected and characterised, according to various MOONRISE strategies. We show that cluster spectroscopic confirmation and characterisation could be efficiently achieved up to z∼1.7 even with the shallowest survey strategy. This open unprecedented insight into the physical properties of high-redshift galaxy clusters and into galaxy formation in dense environments.
Related
- Tighter dark-matter constraints from the projected mass method: A neural-network-enhanced method for galaxy groups and clusters
- Impact of f(R) gravity models on hydrostatic mass of galaxy clusters
- A deep learning approach to member identification and mass estimation in galaxy clusters
- Pinpointing the cosmic web between massive galaxy clusters. I. The incidence of H i and O vi as WHIM tracers
- Characterising the formation and evolution of S0-galaxies (CaFES-0): Their formation pathways around galaxy clusters
BibTeX
@misc{galois2026galaxy,
title = {{Galaxy clusters in the VIDEO fields: detection and characterisation in the context of MOONRISE}},
author = {Pierre Galois and Christophe Benoist and Gianluca Castignani and Matteo Maturi and Sophie Maurogordato and Pascale Jablonka and Yannick Bahé and Derek McLeod and Rebecca Bowler and Olga Cucciati and Lauro Moscardini and Manuela Magliocchetti and Mario Radovich and Michele Cirasuolo and Giovani Covone and Fergus Cullen and Callum Donnan and Hector Flores and William Hartley and Roberto Maiolino and Ross McLure and Nicolarosario Napolitano and Maurizio Paolillo and Mattia Vaccari},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2606.13359},
eprint = {2606.13359},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.13359},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Galaxy clusters in the VIDEO fields: detection and characterisation in the context of MOONRISE
AU - Pierre Galois
AU - Christophe Benoist
AU - Gianluca Castignani
AU - Matteo Maturi
AU - Sophie Maurogordato
AU - Pascale Jablonka
AU - Yannick Bahé
AU - Derek McLeod
AU - Rebecca Bowler
AU - Olga Cucciati
AU - Lauro Moscardini
AU - Manuela Magliocchetti
AU - Mario Radovich
AU - Michele Cirasuolo
AU - Giovani Covone
AU - Fergus Cullen
AU - Callum Donnan
AU - Hector Flores
AU - William Hartley
AU - Roberto Maiolino
AU - Ross McLure
AU - Nicolarosario Napolitano
AU - Maurizio Paolillo
AU - Mattia Vaccari
PY - 2026
DA - 2026/09/09
PB - arXiv
DO - 10.48550/arxiv.2606.13359
UR - https://arxiv.org/abs/2606.13359
AB - We analyse the cluster content of the ∼ 4.5 deg^2 XMM-LSS and CDFS VIDEO fields which are expected to be partially covered by the upcoming MOONRISE survey. Using AMICO and WaZP photometric redshift-based cluster finders, we construct a sample of $519$ cluster candidates detected by both finders in the redshift range z = 0.1−3, including $74$ detections at z > 1.5. For all detections, we identify the Brightest Central Galaxy (BCG) and compute a list of probabilistic cluster memberships. Our photometric redshift measurements of the clusters agree well with spectroscopic redshifts from the literature, when available. From ancillary spectroscopic data, we assign z_spec measurements to $116$ cluster candidates based on their spectroscopic members and to $204$ based on their likely BCGs. We also show that candidates containing Radio-Loud members are efficiently recovered using the prior-based cluster finder PPM. We perform a preliminary analysis of the galaxy content of these candidates, focusing on the Red-Sequence components of their apparent Colour-Magnitude Diagram. By comparing with models of galaxy evolution, we show that this population is consistent with a model of passive evolution with a formation at high redshift, and is already in place at z = 1.5−2.0. Finally, our cluster sample is used to evaluate how these clusters would be detected and characterised, according to various MOONRISE strategies. We show that cluster spectroscopic confirmation and characterisation could be efficiently achieved up to z∼1.7 even with the shallowest survey strategy. This open unprecedented insight into the physical properties of high-redshift galaxy clusters and into galaxy formation in dense environments.
ER -