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arxiv: 2606.13359 · v1 · pith:REEORWYJnew · submitted 2026-06-11 · 🌌 astro-ph.GA

Galaxy clusters in the VIDEO fields: detection and characterisation in the context of MOONRISE

Pierre Galois , Christophe Benoist , Gianluca Castignani , Matteo Maturi , Sophie Maurogordato , Pascale Jablonka , Yannick Bah\'e , Derek McLeod
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Rebecca Bowler Olga Cucciati Lauro Moscardini Manuela Magliocchetti Mario Radovich Michele Cirasuolo Giovani Covone Fergus Cullen Callum Donnan Hector Flores William Hartley Roberto Maiolino Ross McLure Nicolarosario Napolitano Maurizio Paolillo Mattia Vaccari
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Pith reviewed 2026-06-27 06:35 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy clustersphotometric redshiftsred sequencepassive evolutionVIDEO fieldsMOONRISE surveycluster detection
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The pith

Galaxy clusters at z up to 3 in VIDEO fields have red sequences consistent with passive evolution already in place at z=1.5-2.0

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper identifies 519 galaxy cluster candidates in the VIDEO fields using two photometric redshift-based finders, AMICO and WaZP. It assigns spectroscopic redshifts to many candidates and shows that those with radio-loud members are recovered by another finder. The red-sequence galaxies in these clusters match models of passive evolution with high-redshift formation and are already established by z=1.5-2.0. The work also assesses that MOONRISE survey strategies can confirm and characterize clusters spectroscopically up to z approximately 1.7.

Core claim

A sample of 519 cluster candidates is constructed from overlapping detections by AMICO and WaZP in the redshift range 0.1 to 3, with 74 at z>1.5. The red-sequence component of their color-magnitude diagrams is consistent with passive evolution models formed at high redshift and already in place at z=1.5-2.0. Cluster spectroscopic confirmation is feasible up to z~1.7 with MOONRISE even using the shallowest strategy.

What carries the argument

Overlap between independent photometric cluster finders AMICO and WaZP to select reliable candidates, together with analysis of the red sequence in apparent colour-magnitude diagrams.

If this is right

  • Candidates with radio-loud members are efficiently recovered by the prior-based finder PPM.
  • The galaxy population supports passive evolution with formation at high redshift.
  • Cluster confirmation and characterization up to z~1.7 is possible with shallow MOONRISE survey strategies.
  • This provides insight into physical properties of high-redshift clusters and galaxy formation in dense environments.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar overlap methods could be applied to other multi-finder cluster searches to reduce false positives.
  • Extending the analysis to deeper data might reveal evolution beyond z=2.
  • Connection to radio-loud AGN could inform models of cluster assembly.

Load-bearing premise

The overlap of detections from AMICO and WaZP reliably identifies real physical clusters instead of projection effects or spurious overdensities.

What would settle it

Spectroscopic observations of a significant fraction of the z>1.5 candidates showing no coherent velocity structure or member galaxies would indicate many are not real clusters.

Figures

Figures reproduced from arXiv: 2606.13359 by Callum Donnan, Christophe Benoist, Derek McLeod, Fergus Cullen, Gianluca Castignani, Giovani Covone, Hector Flores, Lauro Moscardini, Manuela Magliocchetti, Mario Radovich, Matteo Maturi, Mattia Vaccari, Maurizio Paolillo, Michele Cirasuolo, Nicolarosario Napolitano, Olga Cucciati, Pascale Jablonka, Pierre Galois, Rebecca Bowler, Roberto Maiolino, Ross McLure, Sophie Maurogordato, William Hartley, Yannick Bah\'e.

Figure 1
Figure 1. Figure 1: Left: VISTA H-magnitude galaxy counts for the XMM-LSS and CDFS fields. The vertical dashed line represent the mH = 24 completeness limit. Right: Distribution of the photometric redshifts of galaxies with mH < 24 in the XMM-LSS and the CDFS within the redshift range zphot ∈ [0, 3]. Each of the VIDEO (Jarvis et al. 2013) XMM-LSS and CDFS fields spans approximately ≃ 4.5 deg2 . For both of these fields, McLeo… view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of the mean bias ¯ε in bins of zspec in the XMM-LSS (left panel) and the CDFS (right panel). The y-axis error bars represent the standard deviation σϵ computed in the corresponding redshift bin. The x-axis error bars represent the bin widths. All data points are shown in the background, with density reconstructed using a Gaussian kernel. The filled red area represents the estimated scatter of the… view at source ↗
Figure 3
Figure 3. Figure 3: Evolution of the redshift scatter εcl between the AM￾ICO and WaZP matched detections for a projected physical sep￾aration criterion of R = 150 kpc. The black dots represent the mean bias computed per bins of redshift, with the associated bins width and standard deviation as x and y-error bars, respectively. The gray envelops represent the estimated dispersion σcl(z) of the offset between the AMICO and WaZP… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of the AMICO and WaZP S/N of the matched cluster candidates compared to all the detections in the XMM-LSS and CDFS [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of the photometric redshifts of the AMICO￾WaZP joint cluster candidates in the XMM-LSS (red) and CDFS (blue). These distributions appear similar in both fields. The filtering kernel is automatically derived via a constrained minimisation procedure, producing an unbiased minimum￾variance estimate of the cluster amplitude A. AMICO scans the sky with an angular and redshift resolution of 0.3 arcm… view at source ↗
Figure 7
Figure 7. Figure 7: Spatial distribution of the cluster candidates within the XMM-LSS (left) and the CDFS (right). The black backgrounds represent the footprints of both fields. The colours indicate the mean photometric redshift of the AMICO-WaZP joint detections. The red rectangle marks the limit of the footprint of the UDS subfield, the region which will be covered by MOONRISE in the XMM-LSS [PITH_FULL_IMAGE:figures/full_f… view at source ↗
Figure 9
Figure 9. Figure 9: They all present a significant concentration of galaxies. [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 8
Figure 8. Figure 8: Coloured cutouts of three XMM-LSS (top) and three CDFS (bottom) cluster candidates from the joint catalogue in the redshift range zphot, joint ∼ 1−1.6. All images are built using HSC R, I, and VIDEO H bands. The field of view is 0.6×0.6 Mpc2 . We display the position of the members with membership probabilities of 0.75-1.0, 0.5-0.75 and 0.25-0.5 by green, yellow and orange circles, respectively. The locati… view at source ↗
Figure 9
Figure 9. Figure 9: Same as Fig.8 but for two XMM-LSS (left) and two CDFS (right) cluster candidates from the joint catalogue at zphot, joint ∼ 2. The FoV was adapted for each candidate to avoid perturbation of the image dynamic by bright foreground sources. The physical scale is indicated by the white line on the bottom of each image. tify which one corresponds to the detection made by the cluster finder in photometric redsh… view at source ↗
Figure 10
Figure 10. Figure 10: Left: Relation between zphot, joint and the estimated zspec, Gaussian. The x-axis error bars are derived using a Gaussian kernel bandwidth, while the y-axis error bars are derived from the galaxies photometric redshift metrics (1σ confidence level). The inset panel shows the probability distribution function of the offset (zphot, joint − zspec, Gaussian)/(1 + zspec, Gaussian) between the two redshift meas… view at source ↗
Figure 11
Figure 11. Figure 11: Relation between the redshift of PPM overdensities and cluster candidates for the associated pairs in the XMM-LSS (red) and CDFS (blue). The inset panel shows the probability distri￾bution function of the offset (zphot, PPM − zphot, joint)/(1 + z¯). We observe an overall good agreement between the redshifts of the matched candidates. terloper contamination). Only measurements with more than five members a… view at source ↗
Figure 13
Figure 13. Figure 13: Relation between the spectroscopic redshift from the literature, zlit, and the mean AMICO-WaZP redshift, zphot, joint, for candidates that match with the ancillary cluster catalogues. The inset panel shows the distribution of the offset (zphot, joint − zlit)/(1 + zlit). The error bars are derived from the galaxies pho￾tometric redshift metrics, at 1σ level. The standard deviation of the relation is approx… view at source ↗
Figure 14
Figure 14. Figure 14: Examples of Colour-magnitude diagrams (CMDs) for candidates at different redshifts. Each example corresponds to one combination of filters, as described in [PITH_FULL_IMAGE:figures/full_fig_p013_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Evolution of the apparent mean colour of the Red￾Sequence for the AMICO-WaZP joint candidates as a func￾tion of redshift. The coloured envelopes represent the expected colours derived from models within the metallicity range Z ∈ [0.004, 0.05] for a formation redshift at zf = 10, for a folding time of τf = 0.75 Gyr, without any subsequent burst of star for￾mation. The error bars for the x-axis represent th… view at source ↗
Figure 16
Figure 16. Figure 16: Stacked UVJ diagram of galaxies with zphot ∈ [0.8 − 2.0] (left) and zphot ∈ [2.0 − 2.3]. The red line represents the limit between quiescent and star-forming galaxies empirically derived, as defined by Eqs. 4 and 5. structure (the Shallow-Wide strategy). To meet scientific ob￾jectives, observational requirements in terms of redshift cov￾erage, magnitude limits, and sampling rate were derived from mock cat… view at source ↗
Figure 17
Figure 17. Figure 17: Mean weighted distribution of the H-band magnitude of the detected members (in red for passive galaxies, in blue for star￾forming galaxies. The dashed black bars are for all members) per cluster candidate when applying the Shallow-Wide MOONRISE strategy to the CDFS + XMM-LSS. From left to right, redshift ranges [0.8, 1.2], [1.2, 1.7] and [2.0, 2.3] are shown. In each box, a legend describing the mean numb… view at source ↗
Figure 18
Figure 18. Figure 18: Same as Fig.17 but for the UDS when applying the Medium-Deep strategy. dom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Humanities, Science and Technology of Mexico (CONAH￾CYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl.gov/… view at source ↗
read the original abstract

We analyse the cluster content of the $\sim 4.5 \text{ deg}^{2}$ 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 $z_\text{spec}$ 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 $z\sim1.7$ 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.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The paper analyzes ~4.5 deg² VIDEO fields (XMM-LSS and CDFS) using AMICO and WaZP photometric-redshift cluster finders to identify 519 cluster candidates (including 74 at z>1.5) detected by both algorithms. It assigns BCGs and probabilistic memberships, compares photometric redshifts to available spectroscopic data (116 candidates via members, 204 via BCGs), demonstrates efficient recovery of radio-loud clusters with PPM, analyzes red-sequence galaxies in color-magnitude diagrams, concludes consistency with passive evolution models formed at high redshift and already in place at z=1.5-2.0, and evaluates detection/characterization prospects under various MOONRISE survey strategies, claiming efficient spectroscopic confirmation up to z~1.7 even with the shallowest strategy.

Significance. If the high-redshift sample is robust, the work supplies a sizable catalog of z>1.5 cluster candidates in well-studied fields, enabling studies of galaxy evolution in dense environments and providing practical input for MOONRISE observing strategies. Strengths include the dual-finder overlap approach, direct comparison to spectroscopic redshifts, and the ancillary radio-loud and red-sequence analyses. The central evolutionary and MOONRISE claims, however, rest on the purity of the overlap-selected sample at z>1.5.

major comments (3)
  1. [Abstract (sample construction)] Abstract (sample construction paragraph): The 74 z>1.5 candidates are selected solely via common detections in AMICO and WaZP; no purity estimate, mock-catalog validation, or multi-wavelength (X-ray/SZ) cross-check is reported for this overlap subsample. This is load-bearing for the passive-evolution conclusion and the MOONRISE strategy assessment.
  2. [Abstract (red-sequence analysis)] Abstract (red-sequence paragraph): The claim that the red-sequence population 'is already in place at z=1.5-2.0' and 'consistent with a model of passive evolution' is presented without quantitative metrics (e.g., number of red-sequence members per cluster, membership probability thresholds, or goodness-of-fit statistics) for the 74 high-z candidates.
  3. [Abstract (MOONRISE evaluation)] Abstract (MOONRISE evaluation paragraph): The assertion that 'cluster spectroscopic confirmation and characterisation could be efficiently achieved up to z∼1.7 even with the shallowest survey strategy' lacks the specific survey-depth parameters, simulation setup, or success-rate metrics used to reach this conclusion.
minor comments (2)
  1. [Abstract] The abstract states photometric redshifts 'agree well' with spectroscopic redshifts but provides neither the number of comparisons, the typical offset, nor the scatter.
  2. [Abstract] No explicit statement of the membership probability threshold or post-detection cleaning cuts applied to the final catalog of 519 candidates.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed review. We address each major comment below and will revise the manuscript to strengthen the presentation of our results, particularly in the abstract and supporting sections.

read point-by-point responses

  1. Referee: Abstract (sample construction paragraph): The 74 z>1.5 candidates are selected solely via common detections in AMICO and WaZP; no purity estimate, mock-catalog validation, or multi-wavelength (X-ray/SZ) cross-check is reported for this overlap subsample. This is load-bearing for the passive-evolution conclusion and the MOONRISE strategy assessment.

    Authors: The overlap between AMICO and WaZP is explicitly chosen to improve sample reliability, and the manuscript validates the overall catalog via direct comparison to spectroscopic redshifts (116 candidates via members, 204 via BCGs). We agree the abstract does not quote a numerical purity for the z>1.5 overlap subsample alone. We will revise the abstract to note the dual-finder validation and add a short paragraph in the main text discussing the expected purity gain from the intersection method together with any available ancillary checks. If new mock runs are not feasible we will state this limitation explicitly. revision: partial

  2. Referee: Abstract (red-sequence analysis paragraph): The claim that the red-sequence population 'is already in place at z=1.5-2.0' and 'consistent with a model of passive evolution' is presented without quantitative metrics (e.g., number of red-sequence members per cluster, membership probability thresholds, or goodness-of-fit statistics) for the 74 high-z candidates.

    Authors: The red-sequence analysis is labelled preliminary and relies on visual comparison of colour-magnitude diagrams against passive-evolution tracks. Quantitative details (member counts, probability thresholds, model fits) appear in the main text for the full sample; the high-redshift subset has lower statistics and is not broken out separately. We will revise the abstract wording to reflect the preliminary character and ensure the main text supplies explicit metrics or thresholds for the z>1.5 objects where possible. revision: yes

  3. Referee: Abstract (MOONRISE evaluation paragraph): The assertion that 'cluster spectroscopic confirmation and characterisation could be efficiently achieved up to z∼1.7 even with the shallowest survey strategy' lacks the specific survey-depth parameters, simulation setup, or success-rate metrics used to reach this conclusion.

    Authors: The MOONRISE assessment applies the observed cluster sample to a set of survey strategies whose depth parameters and success-rate calculations are described in the dedicated section of the manuscript. We will expand the abstract to include the key depth values and the derived confirmation efficiencies so the claim is self-contained. revision: yes

Circularity Check

0 steps flagged

No circularity in derivation chain

full rationale

The paper constructs a cluster candidate sample via overlap of two independent photometric-redshift finders (AMICO and WaZP) and performs a preliminary comparison of the red-sequence population against external galaxy evolution models. No equations, fitted parameters, or self-citations are presented that reduce the reported detections, membership probabilities, or evolutionary conclusions to the inputs by construction. The analysis relies on ancillary spectroscopic data and standard model comparisons without self-definitional steps or load-bearing self-citations.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract alone supplies no explicit free parameters, axioms, or invented entities; cluster finders and passive-evolution models are treated as black boxes whose internal assumptions are not enumerated.

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