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S-PLUS photo-zs recover cluster members and show that faint galaxies stay blue regardless of concentration.

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2026-07-12 07:35 UTC pith:JTWTBOYY

load-bearing objection Solid SCALE infrastructure paper: usable 83-system catalog and photo-z validation; the A4038 concentration-color evolutionary claim is still single-system and multi-halo fragile. the 2 major comments →

arxiv 2607.02704 v1 pith:JTWTBOYY submitted 2026-07-02 astro-ph.CO astro-ph.GA

S-PLUS Clusters And Large-scale Environments (SCALE): I. A catalog of known clusters and groups in DR5 and a pilot study of Abell 4038

C. Mendes de Oliveira , N. M. Cardoso , P. A. A. Lopes , A. L. B. Ribeiro , D. E. Olave-Rojas , A. Krabbe , L. Sodr\'e Jr. , R. Demarco
show 21 more authors
A. V. Smith Castelli R. Cid Fernandes F. R. Herpich S. Torres-Flores E. R. Carrasco E. V. R. Lima G. Oliveira Schwarz A. P. Costa L. Doubrawa G. P. Montaguth C. Lima-Dias E. S. Cypriano M. S. Carvalho C. Lobo M. Fonseca-Faria L. Nakazono A. R. Lopes F. Almeida-Fernandes A. Kanaan T. Ribeiro W. Schoenell
This is my paper
classification astro-ph.CO astro-ph.GA
keywords galaxy clustersgalaxy groupsphotometric redshiftscluster membershiplarge-scale structuregalaxy evolutionS-PLUSAbell 4038
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper launches SCALE by publishing a homogeneous catalog of 83 known nearby groups and clusters (0.008 ≤ z ≤ 0.1) with derived R200, M200, velocity dispersions, and spectroscopic memberships. It shows that S-PLUS 12-band photometric redshifts match literature spectroscopic redshifts closely enough that photometric membership works for systems and their outskirts. As a pilot, the authors apply Reliable Photometric Membership to Abell 4038, recovering hundreds of members (many faint and previously unobserved) and mapping about a dozen substructures within 10 R200, including the additional systems A4038B and A4049. Color–luminosity analysis then finds the expected redder-brighter trend, but concentration modulates it: low-concentration galaxies have a weaker color–luminosity slope, and the faintest galaxies are blue largely independent of concentration. The result is a public reference sample and a concrete demonstration that deep multi-band photo-zs open faint-galaxy studies of environmental processing out to several virial radii.

Core claim

S-PLUS photometric redshifts agree well with spectroscopic redshifts for the 83 systems, enabling reliable photometric membership; applied to Abell 4038 this recovers new members and about a dozen substructures (including A4038B and A4049), while color–luminosity segregation weakens for low-concentration galaxies so that low-luminosity systems are blue largely independent of concentration, challenging a simple morphology–color dichotomy.

What carries the argument

Reliable Photometric Membership (RPM): a support-vector-machine classifier trained on spectroscopic members of the SCALE sample (excluding A4038) that uses S-PLUS colors, magnitudes, photo-zs, surface brightness and projected distance to assign membership probabilities, recovering faint members missed by spectroscopy.

Load-bearing premise

The catalog and A4038 analysis rest on dynamical M200 and R200 from iterative shifting-gapper membership plus a velocity-dispersion–mass scaling that the paper itself reports can have tens-of-percent to factor-of-two uncertainties, especially for poorly sampled low-mass systems.

What would settle it

Obtain substantially more spectroscopic redshifts for the RPM-selected A4038 candidates (especially the 124 new photometric members within 5 R200) and re-run the substructure and color–concentration tests; if many supposed members are interlopers or the concentration-dependent color slopes disappear, the membership and evolutionary claims fail.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. The paper introduces SCALE and delivers a catalog of 83 known groups/clusters (0.008 ≤ z ≤ 0.1) in S-PLUS DR5 with iteratively derived σ_cl, R200, and M200 from literature spectroscopy via the shifting-gapper technique, plus a large membership table. It demonstrates that S-PLUS photo-zs match literature spec-zs well (small peak offsets s, σ_NMAD ≲ 1–3% by magnitude), applies the RPM algorithm to recover photometric members of Abell 4038, maps ~a dozen substructures (including A4038B and A4049) with 2D/3D methods, and reports a color–luminosity trend that is weaker for low-concentration (C ≤ 2.5) galaxies, with faint systems blue largely independent of C.

Significance. A homogeneous southern reference sample with public membership catalogs, photo-z validation, and multi-method substructure maps is useful for environmental studies and for planning spectroscopy (e.g. 4MOST/CHANCES). Strengths include deliberate exclusion of A4038 from RPM training, explicit photo-z vs. spec-z offset corrections, and an independent eROSITA mass check (median offset −0.03 dex, σ_MAD = 0.20 dex). The evolutionary claim that concentration modulates the color–magnitude relation and challenges a simple morphology–color dichotomy is interesting but rests on a single complex system; if confirmed on the full SCALE sample it would be a solid contribution to environmental quenching studies.

major comments (2)
  1. [Abstract; §4.3–4.6; Fig. 4, 6] The abstract and §4.5–4.6/Fig. 6 present the weaker color–luminosity slope for C ≤ 2.5 and the faint-end convergence as evidence for mass-dependent pathways that challenge a simple morphology–color dichotomy. That interpretation is drawn only from A4038 (420 RPM members inside 5 R200). Section 4.3 and Fig. 4 show three kinematically distinct systems (A4038, A4038B at |ΔV|/σ ~ 1.5–2, A4049 at R/R200 ~ 1.25). Photometric members assigned to “A4038” can therefore mix galaxies from different halos and dynamical states. The paper should either re-run the C-split analysis after excluding or separately tagging A4038B/A4049 members, or clearly reframe the result as a pilot finding for one multi-halo field rather than a general evolutionary claim.
  2. [§2; Appendix B; §4.4–4.5] All radial normalizations and the 5 R200 membership cut for A4038 use R200 from the iterative shifting-gapper + Ferragamo/Munari σ–M pipeline. Section 2 and Appendix B report median ΔM200/M200 ≃ 38% (and 70–140% for N200 < 10). For A4038 itself (N200 = 119) the mass is better constrained, but the absolute length scale remains uncertain. A short sensitivity test (re-binning colors/radii at R200 ± 20–30%, or quoting physical Mpc alongside R/R200) would show whether the C-split slopes and faint-end convergence are robust to that scale error.
minor comments (5)
  1. [§4.4] No k-corrections are applied to g−r (§4.4). The stated ~0.02 mag shift at z = 0.028 is small, but a one-sentence note that relative quintile ordering is unchanged (or a quick check with Chilingarian-style k-corrections) would close the point for absolute color comparisons.
  2. [§4.5] The C = 2.5 split is justified for dwarfs, but the text should state whether C is measured on S-PLUS or Legacy imaging and whether a seeing/PSF floor was applied beyond the Petrosian-radius argument for Q5.
  3. [Table 1; §3.2] Table 1 lists s for many systems but leaves blanks for others; a short note on when s could not be measured (too few members, multi-peaked distributions) would help users of the catalog.
  4. [Fig. 3] Figure 3 color coding is helpful; adding a brief legend or panel labels that map colors to the named substructures (A4038B, A4049, eastern group, etc.) would make the 2D/3D comparison easier to follow without the text.
  5. [§2; Table 1] For systems with M200 ≲ 10^13 M⊙ the paper already cautions that masses are highly uncertain; consider flagging those rows more visibly in Table 1 (e.g. a quality column) so the catalog is not over-interpreted.

Circularity Check

0 steps flagged

No load-bearing circularity: catalog masses, photo-z validation, RPM membership (trained excluding A4038), and A4038 trends are data-driven against external benchmarks; only routine method self-citations.

full rationale

The derivation chain is observational and non-circular. Spectroscopic members for the 83 systems are selected via the shifting-gapper technique on literature redshifts (Lima 2025 compilation), then M200/R200/sigma are obtained iteratively from the Ferragamo/Munari sigma-M scaling (external calibrations) and compared independently to eROSITA X-ray masses (Appendix B: median offset -0.03 dex, sigma_MAD=0.20 dex). Photo-z performance is quantified against the same external spec-zs (sigma_NMAD, bias, PIT, HPDCI in Fig. 1; peak offsets s measured and listed in Table 1, then applied). RPM photometric membership for A4038 is trained on the other SCALE systems while deliberately excluding A4038 galaxies, then validated for completeness/purity against held-out spectroscopic members. Substructure detection (DS+/mclust/CALSAGOS) and the color-luminosity-concentration trends (Figs. 5-6) are direct analyses of the resulting member catalogs; they do not redefine inputs as outputs. Overlapping-author citations (Lopes & Ribeiro 2020 for RPM; prior Lopes shifting-gapper papers) supply reusable tools, not uniqueness theorems or fitted parameters that force the central claims. Residual score of 1 reflects only that methodological scaffolding is partly self-cited, which is normal and non-load-bearing. No self-definitional loop, fitted-input-as-prediction, or ansatz smuggling is present.

Axiom & Free-Parameter Ledger

6 free parameters · 6 axioms · 2 invented entities

The work rests on standard cosmology and published scaling relations plus several analysis choices (membership velocity window, concentration cut, RPM probability threshold, substructure multiplicity cuts). No new physical entities are postulated; free parameters are algorithmic thresholds and literature-calibrated scatter terms that affect membership and mass precision.

free parameters (6)
  • Initial membership velocity window Δz=±0.01667 (±5000 km/s)
    Hand-chosen large window used to preselect galaxies before shifting-gapper cleaning; affects interloper pool.
  • RPM membership probability threshold >70%
    Conservative cut that sets reported purity/completeness and the photometric member sample used for color analysis.
  • Concentration split C=2.5
    Adopted threshold separating low- and high-concentration populations; directly shapes the claimed weaker color-luminosity slope for extended galaxies.
  • Substructure Nmin (5 inside 5R200, 10 outside) and DS+ 90% confidence
    Multiplicity and significance cuts that determine which of the ~dozen substructures are retained.
  • Intrinsic σ–M scatter floor (~12% in σ from Munari et al.)
    Literature scatter term propagated into M200 uncertainties; sets a precision floor independent of Ngal.
  • NFW concentration c=4.5 for M500 o M200 conversion
    Fixed concentration assumed when comparing dynamical masses to eROSITA M500 values.
axioms (6)
  • domain assumption Flat ΛCDM with ΩM=0.3, ΩΛ=0.7, H0=100h km/s/Mpc and h=0.7
    Stated cosmology used for distances, absolute magnitudes, and R200/M200.
  • domain assumption Velocity dispersion–mass scaling of Munari et al. (2013) with Ferragamo et al. (2020) corrections yields usable M200
    Core of the dynamical mass pipeline in Section 2; paper notes large errors at low N200.
  • domain assumption Shifting-gapper spectroscopic membership defines the truth sample for training/validation
    Used both for catalog members and as RPM training labels (excluding A4038).
  • domain assumption S-PLUS 12-band ML photo-zs are sufficiently accurate for membership after small per-cluster offsets
    Supported by metrics in Fig. 1 and histogram matches in Fig. 2; still an assumption at faint magnitudes and large radii.
  • domain assumption Gaussian mixture / density-based clustering components with chosen cuts correspond to physical substructures
    Underpins the ~dozen substructures reported around A4038.
  • ad hoc to paper Standard statistical tests (KS, ANOVA, Fisher z) on photometric samples are adequate without full k-corrections at z~0.028
    Authors argue k-correction ~0.02 mag is small relative to color range; absolute color comparisons deferred.
invented entities (2)
  • SCALE project / 83-system reference catalog independent evidence
    purpose: Homogeneous nearby cluster/group sample with derived dynamical properties and member lists for future S-PLUS environment studies
    Organizational product of the paper; not a new physical object, but the main delivered entity.
  • Abell 4038B (kinematically distinct central subsystem) no independent evidence
    purpose: Label a background-like component near A4038 with large line-of-sight velocity offset
    Identified via mclust/pdfCluster on the core; needs independent confirmation as a separate halo.

pith-pipeline@v1.1.0-grok45 · 35578 in / 3843 out tokens · 31328 ms · 2026-07-12T07:35:50.043724+00:00 · methodology

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read the original abstract

Within the framework of the Southern Photometric Local Universe Survey (S-PLUS), we introduce ${\bf S}$-PLUS ${\bf C}$lusters ${\bf A}$nd ${\bf L}$arge-scale ${\bf E}$nvironments (SCALE), a project dedicated to the study of galaxy clusters, groups, and their environments using 12-band photometry of S-PLUS combined with spectroscopic and photometric data from the literature. In this first paper, we present a catalog of 83 previously known systems in the redshift range $0.008 \leq z_{\rm spec} \leq 0.1$, for which we derive $R_{200}$, $M_{200}$, and velocity dispersions. Spectroscopic members are selected and matched with S-PLUS photometric redshifts (photo-$z$s). We find very good agreement between literature spectroscopic redshifts (spec-$z$s) and S-PLUS photometric redshifts (photo-$z$s), demonstrating the potential of the latter for cluster and group membership determination. As a proof of concept, we obtain photometric memberships for Abell 4038 using the Reliable Photometric Membership technique. A two- and three-dimensional analysis of the region within $10 h^{-1}$ Mpc ($10\times R_{200}$) from the center of Abell 4038 reveals about a dozen substructures including two additional clusters within $1.3\times R_{200}$ (Abell 4038B and Abell 4049). A color-luminosity segregation analysis shows that more luminous (less luminous) galaxies are redder (bluer), as expected. Low-concentration galaxies ($C \leq 2.5$) exhibit a weaker color-luminosity dependence, compared to higher-concentration ones, indicating mass-dependent evolutionary pathways that challenge a simple morphology-color dichotomy, with low-luminosity galaxies presenting bluer colors largely independent of concentration. The SCALE catalog provides a valuable basis for future studies of large-scale structures and their connection to galaxy evolution.

Figures

Figures reproduced from arXiv: 2607.02704 by A. Kanaan, A. Krabbe, A. L. B. Ribeiro, A. P. Costa, A. R. Lopes, A. V. Smith Castelli, C. Lima-Dias, C. Lobo, C. Mendes de Oliveira, D. E. Olave-Rojas, E. R. Carrasco, E. S. Cypriano, E. V. R. Lima, F. Almeida-Fernandes, F. R. Herpich, G. Oliveira Schwarz, G. P. Montaguth, L. Doubrawa, L. Nakazono, L. Sodr\'e Jr., M. Fonseca-Faria, M. S. Carvalho, N. M. Cardoso, P. A. A. Lopes, R. Cid Fernandes, R. Demarco, S. Torres-Flores, T. Ribeiro, W. Schoenell.

Figure 1
Figure 1. Figure 1: Performance of the photo-z model. Panels (a) and (b) show the scatter and bias of the SPE metrics as a function of magnitude, and panels (e) and (f) as a function of spectroscopic redshift. Panels (c), (d), and (g) display the odds, PIT, and HPDCI metrics, respectively. Shaded regions represent 1σ uncertainties from bootstrap resampling. brightness (mu max g), and projected distance to the cluster center (… view at source ↗
Figure 2
Figure 2. Figure 2: Comparative redshift distributions for 10 clusters with 0.02 < z < 0.1. Blue histograms show spectroscopic members from Lima (2025). For each cluster, the left panel compares spectroscopic redshift (blue) and photo-z (orange), while the right panel shows the corrected photo-z distribution (pink) after applying the small shift s (listed in the last column of [PITH_FULL_IMAGE:figures/full_fig_p010_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Identification of galaxy substructures in the direction of A4038. The blue solid and dashed circles correspond to R200 and 5R200 of the cluster, respectively. Left panel: 3D phase-space substructures identified for A4038 using the spectroscopic sample and a combination of DS+ and mclust methods, as described in Section 4.1. Middle panel: 2D substructures recovered using CALSAGOS on the spectroscopic sample… view at source ↗
Figure 4
Figure 4. Figure 4: Upper panel: Density contours in projected phase space around A4038 showing the 2D density distribution of all galaxies. Colored points and labels mark the three cluster centers identified by mclust (+BCGs) and pdfCluster. The overdensity located at |∆V |/σ = 2.2 and R/R200 = 1.7 is most probably a substructure around A4038B. Lower panel: Spatial distribution in Equatorial coordinates, with density contour… view at source ↗
Figure 5
Figure 5. Figure 5: Cumulative distribution functions (CDFs) of the g − r color (left panel) and the normalized projected radial distance, R/R200 (right panel), for galaxies grouped into five absolute magnitude quintiles: Q1 (brightest; red), Q2 (orange), Q3 (green), Q4 (blue), and Q5 (faintest; purple). The left panel illustrates segregation in (g-r) color (in units of mag) in bins of magnitude, while the right panel investi… view at source ↗
Figure 6
Figure 6. Figure 6: Upper panel: Behavior of g − r color (in units of magnitude) as a function of absolute r-band magnitude (Mr) for two galaxy populations divided by their concentration index (C). Galaxies with C ≤ 2.5 (blue line) are compared to those with C > 2.5 (red line). Lower panel: Density distributions of C within each bin of absolute r magnitude. The colors are the same as in [PITH_FULL_IMAGE:figures/full_fig_p015… view at source ↗
Figure 7
Figure 7. Figure 7: Logarithmic mass ratio between dynamical mass estimates from the SCALE sample and eROSITA re-scaled masses (i.e., eROSITA M500 were converted to M200, to allow a comparison - see text for details). The ratio shows a small median offset of ∼ 0.03 dex, and σMAD = 0.20 dex. Better agreement is observed if considered only structures with N200 > 50. As previously discussed, the small median offset and moderate … view at source ↗

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