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REVIEW 5 major objections 6 minor 103 references

Galaxies at the edges: a complete census of MACS J0416.1-2403 cluster

T0 review · 5 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read A spectroscopic census of the outskirts of cluster MACS J0416 confirms 81 galaxies inside photometrically identified overdensities and filaments, arguing that galaxies are quenched in groups before joining the cluster.

desk verdict A useful new spectroscopic catalog of the MACS J0416 outskirts, with environmental claims that currently rest on inherited photometry and need a sturdier analysis. read the letter →

arxiv 2506.11216 v1 pith:JIRZPC6F submitted 2025-06-12 astro-ph.GA

Rossella Ragusa , Maurizio D'Addona , Amata Mercurio , Marcella Longhetti , Marisa Girardi , Marianna Annunziatella , Nicolas Estrada , Claudio Grillo
show 15 more authors
Angela Iovino Giula Rodighiero Piero Rosati Benedetta Vulcani Giuseppe Angora Hans Bohringer Massimo Brescia Gabriel Bartosch Caminha Gayoung Chon Fedor Getman Aniello Grado Marco Gullieuszik Luca Limatola Alessia Moretti Luisa Pecoraro
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyclustersclusteroutskirtspre-processinginfallfilamentsspectroscopicredshiftsMACSJ0416environmentalquenching
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports a spectroscopic census of the outskirts of the massive galaxy cluster MACS J0416.1-2403 at $z=0.397$, extending to $5.5R_{200}$, roughly 10 Mpc from the center. The authors measured redshifts for 1236 objects with the AAOmega spectrograph and identify 148 new cluster members, of which 81 fall inside overdensity regions and filaments that a prior photometric study had flagged as candidate infalling groups. The paper argues this is spectroscopic evidence that those structures are real group-scale systems feeding the cluster, and that the outskirts show an environmental sequence: galaxies in higher-density regions are redder, more massive, and more passive than galaxies in lower-density regions. The result matters because it extends the pre-processing scenario, in which galaxies are transformed in group environments before they enter the cluster, to intermediate redshift and to the poorly explored cluster periphery.

What carries the argument

The carrying object is the local density field $\delta$ inherited from the prior photometric catalog, divided into three bins, $\delta\leq 0$ for underdense regions, $0<\delta\leq 1$ for filamentary regions, and $\delta>1$ for overdensities, and overlaid with the new spectroscopic members. The new measurements come from AAOmega multi-object spectroscopy, with redshifts obtained by three independent methods, namely Redrock, EZ, and the new Redmost tool, a member selection window $z=[0.382,0.412]$, and rest-frame stacked spectra that make the color, mass, and density trends visible. Kolmogorov-Smirnov tests comparing the average spectra support the claim that the spectral differences between density populations are not driven by their K-band magnitude distributions.

What would settle it

Re-derive the local density field using only the new spectroscopic members and measure the line-of-sight velocity dispersions of the galaxies assigned to each overdensity: if the 81 galaxies do not cluster in A/B/C and the filaments, or if their dispersions are comparable to the field rather than well below the cluster's global roughly 800-1000 km/s, the pre-infall interpretation would fail.

Watch

Extended reading notes

Core claim

The paper's central claim is that the photometric overdensities and filaments in the outskirts of MACS J0416 correspond to genuine galaxies or galaxy groups currently undergoing infall, and that the environment has already begun reshaping their galaxy populations before they reach the cluster. This rests on the spectroscopic confirmation of 81 of the 148 new members inside the three overdensity regions A, B, and C plus the filamentary structures, and on stacked spectra that show a density-dependent trend: as local density rises from underdense through filamentary to overdense, galaxies become progressively redder in $(g-r)_{\rm Kron}$, brighter in the K band, and more passive, while the small population of blue galaxies in high-density regions stays spectrally similar to blue galaxies elsewhere, suggesting recent infall.

Load-bearing premise

The density bins and the A/B/C overdensity and filament labels are taken from a photometric catalog based on SED fitting and photometric redshifts, and the paper does not re-derive the density field from the new spectroscopic data, so if those photometric structures are projections or contaminated by field galaxies, the 81-galaxy confirmation and the density-property trends would rest on a flawed assignment.

Editorial extensions

If this is right

  • The A, B, and C overdensities plus the filamentary bridge between B and C are real physical structures that contribute to the cluster's mass assembly.
  • Galaxy properties in the outskirts are already differentiated before infall, supporting pre-processing in group environments at $z\sim0.4$.
  • The new catalog extends spectroscopic coverage of MACS0416 from roughly $2R_{200}$ to $5.5R_{200}$ and includes galaxies down to the dwarf regime, providing a resource for outskirts studies.
  • The secondary redshift peaks near $z\sim0.384$ and $z\sim0.405$ correspond to infalling structures, now visible in the combined MUSE, VIMOS, and AAOmega redshift distribution.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A direct dynamical test is available: if the 81 galaxies in regions A, B, and C and the filaments are bound infalling groups, their line-of-sight velocity dispersions should be well below the cluster's roughly 800-1000 km/s, whereas unbound projections would show field-like dispersions.
  • The same photometric-to-spectroscopic follow-up strategy could be used to locate pre-processing sites in other $z\sim0.4$ clusters, where X-ray detection of the group gas is difficult.
  • The paper's mass-versus-environment separation is only qualitative; a quantitative analysis at fixed stellar mass, combining MUSE, VIMOS, and AAOmega data, would test whether the density trends persist when mass is held constant.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

5 major / 6 minor

Summary. This paper presents 2dF+AAOmega spectroscopy of the outskirts of the galaxy cluster MACS J0416.1-2403 out to about 5.5 R200, measuring redshifts for 1236 objects with a 98.7% success rate and identifying 148 new spectroscopic cluster members in a narrow redshift window around z=0.397. The members are matched to the photometric density map of Estrada et al. (2023), and the paper reports that 81 of the 148 members lie in the A/B/C overdensity and filamentary regions, which it interprets as spectroscopic confirmation of infalling groups and thus support for the pre-processing scenario. The paper also presents stacked spectra split by g-r color, K-band magnitude, and local density, arguing that higher-density environments contain redder, more massive, and more passive galaxies. The redshift catalog and its quality control appear robust, but the environmental analysis is largely qualitative and relies entirely on the inherited photometric density field without controlling for target selection or providing statistical tests.

Significance. If the 81/148 confirmation and the density-property trends are correct, this would be one of the first spectroscopic confirmations of photometric infall structures around a z~0.4 cluster and would support the pre-processing scenario in cluster outskirts. The deliverable catalog is a clear strength: the AAOmega redshifts extend spectroscopic coverage of MACS0416 by a factor of about 2.5 in radius, reach dwarf galaxies, and are supported by careful quality flags following Balestra et al. (2016), cross-checks with three independent redshift codes (Redrock, EZ, and the newly released Redmost), and a public data release. These strengths make the dataset a useful community resource. However, the scientific claims about the reality and nature of the overdense regions are not yet supported at the same standard, because the key counts and trends are not tested against the selection function or a null expectation, and the statistical procedures used for the spectral comparisons are not valid as presented.

major comments (5)
  1. [Sec. 5.3 (Fig. 6)] The central claim that 81 of 148 new members lie in the A/B/C overdensity and filamentary regions of Estrada et al. (2023) is made without a control for the area fraction of those regions or for the spectroscopic target-selection function. Because the AAOmega targets were selected from the same photometric catalog used to define the overdensities (Sec. 3), an overdensity in the target distribution could be partly induced by the input catalog. The paper should (i) report the sky-area fraction covered by the A/B/C+filament footprint; (ii) compute the expected number of members in that footprint under a null distribution with the same selection function; and (iii) give the counts in A, B, C, and filaments separately, since region A is explicitly admitted to lack a well-defined spectroscopic counterpart. Without these, the 81/148 number cannot be evaluated as a confirmation.
  2. [Sec. 5.3 (Fig. 4b)] The secondary redshift peaks at z~0.385 and z~0.405 are presented as evidence that regions B and C are real infalling systems, with the text stating that 'These findings support the hypothesis that such structures may correspond to real physical systems currently experiencing infall,' but no statistical significance is given. The peaks appear in the AAOmega and combined redshift distributions, yet no mixture-model fit, bootstrap test, or velocity-dispersion estimate is provided. Given that the membership window itself is ±3000 km/s, the peaks need to be distinguished from the main cluster velocity distribution before they can be used to support the physical interpretation.
  3. [Sec. 5.3 (Fig. 8)] The Kolmogorov–Smirnov tests are applied to smoothed stacked spectra ('We performed a KS test on each pair of average spectra, obtaining p-values much smaller than 0.05'), which is not a valid test of whether the underlying galaxy populations differ. The effective sample size is not the number of galaxies, and the Gaussian smoothing further modifies the distributions being compared. The subsequent KS tests on K-band magnitude distributions are more appropriate, but they should be reported with sample sizes and test statistics. The spectral comparison should instead use standard two-sample tests on the individual galaxies (e.g., on emission-line strengths or colors) or, at minimum, bootstrap confidence envelopes on the stacked spectra.
  4. [Sec. 3] The paper states that only ~1290 of ~2000 expected targets were observed due to weather, i.e., roughly 30% of the photometric catalog with Vlim<21.5, and that this 'prevented us from fully spectroscopically covering all the photometric overdensities' and 'partially limited the statistical significance.' The spatial selection function is not quantified. If the missing fibers are not randomly distributed on the sky, which is likely for weather-affected multi-object spectroscopy, both the 81/148 count and the density-property trends could be biased. Please provide a completeness map relative to the parent photometric catalog and test the robustness of the key results to the selection function, for example by re-weighting or by comparing against random subsamples.
  5. [Secs. 5.1-5.3 (Figs. 5, 7, 8)] All stacked spectra are presented without uncertainties. The qualitative claims, for example that red galaxies in overdense regions are more passive than their lower-density counterparts and that blue galaxies show minimal variation with density, cannot be assessed without error estimates. Adding bootstrap or jackknife confidence envelopes and stating the number of galaxies in each stack would convert these from visual impressions into testable statements. This is particularly relevant because the KS-test justification in Fig. 8 is not statistically valid, as noted above.
minor comments (6)
  1. [Sec. 4.1] The heading contains a typo: 'distibution' should be 'distribution'.
  2. [Throughout] The text contains many instances of split ligatures, such as 'e ffects', 'di fferent', and 'e fficiencies'; please ensure the final typeset version renders these correctly.
  3. [Fig. 6] In the left panel caption, white circles are used for all AAOmega redshifts and light blue circles for members; in grayscale these may be difficult to distinguish, so different symbols or labeled contours would improve readability.
  4. [Sec. 5.1] The color cut (g-r)~1.20 is adopted from Estrada et al. (2023), but the paper does not state whether the photometric catalog version is the same as that used for target selection; a brief explicit statement would avoid ambiguity.
  5. [Sec. 5.3] The text explains that region A lacks a spectroscopic counterpart because the photometric candidates did not meet the magnitude limit, but it does not state the actual limiting magnitude of the AAOmega sample; adding this value would help quantify the selection effect.
  6. [Sec. 4.1] The connection between the quoted cluster redshift z=0.397±0.001 and the adopted membership window z=[0.382-0.412] is described, but a brief sentence explicitly relating the ±3000 km/s velocity range to the Δz=0.015 window would improve clarity.

Circularity Check

1 steps flagged · score 4.0 of 10

The 81/148 confirmation and the environmental trends are measured against the Estrada et al. (2023) photometric density field inherited from the same team and the same parent catalog as the AAOmega targets, so the pre-processing conclusion is partly a self-consistency check rather than an independent test.

  1. self citation load bearing [Sec. 5.3, Fig. 6 and surrounding text]
    "following the environmental density definition by Estrada et al. (2023) ... we superimpose the whole AAOmega dataset on the density field of objects dentified as cluster members through photometric SED fitting Estrada et al. (2023). ... In total, we spectroscopically confirm 81 galaxies in the three A, B and C overdensities plus filamentary regions."

    The overdensity regions A/B/C and the delta bins are not re-derived from the new spectroscopic sample; they are taken from Estrada et al. (2023), whose photometric SED-fitting member catalog is also the parent catalog from which the AAOmega targets were drawn (Sec. 3: targets are '30% of the total number of objects in the photometric catalog'). The headline '81/148 in overdensities plus filaments' is therefore a count of how many spectroscopically confirmed members fall inside regions defined by the same photometric catalog that supplied the targets; it does not independently establish that those regions are real bound infalling groups. That reality, the pre-processing interpretation, is the load-bearing input inherited from the same team's prior paper.

full rationale

The paper's new spectroscopic redshifts are genuinely independent measurements of cluster membership: 148 members are selected by AAOmega redshifts in z=[0.382-0.412], not derived from Estrada et al. (2023) fitting. However, the central '81 in overdensities' result and the environmental trends are computed by overlaying these new redshifts on Estrada's photometric density field, and the AAOmega targets were drawn from that same photometric catalog. The paper never re-derives the density field or delta bins from the new spectroscopy, and it explicitly admits that region A lacks a well-defined spectroscopic counterpart while still including it in the 81 count. The redshift peaks near z~0.385 and z~0.405 provide some independent support for regions B and the B-C filament, so the central claim is not forced by construction. The result is therefore partially circular in that the pre-processing conclusion is a self-consistency check of the inherited photometric map, but it retains independent spectroscopic content.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The central environmental claims rest on a small set of free binning choices (density thresholds, K-band magnitude bins, redshift window) and on the inherited photometric density field from Estrada et al. (2023). No new physical entities are introduced. The K-band mass proxy and g-r color classification are standard domain assumptions but are load-bearing for the qualitative spectral comparisons.

free parameters (4)
  • Local density bins for environment classification
    The sample is split into low (delta <= 0), medium (0 < delta <= 1), and high (delta > 1) density regions, a hand-chosen binning of the Estrada et al. (2023) density field. This binning directly determines the environmental trends in Section 5.3.
  • K Kron magnitude bins for mass stratification
    The cluster members are divided into three bins (KKron < 17.9, 17.9 to 18.9, and >= 18.9 mag), chosen to create roughly equal subsample sizes for the stacked spectra in Section 5.2. The exact boundaries are ad hoc.
  • Redshift membership window = z = [0.382, 0.412]
    Cluster membership is assigned through a fixed redshift window corresponding to +-3000 km/s around the cluster redshift, following Balestra et al. (2016) and Rosati et al. (2014). This window is not derived from a dynamical analysis and is acknowledged to include possible infalling and backsplash galaxies.
  • g-r color cut = (g-r)Kron = 1.20 mag
    The red/blue split uses the color cut from Estrada et al. (2023), adopted without modification. The cut is a free threshold from prior work, not derived in this paper.
assumptions (4)
  • domain assumption K-band luminosity is a reliable proxy for stellar mass.
    Stated in Section 5.2, relying on a tight mass-to-light ratio in the near-infrared. This is a standard approximation but not model-independent, and the paper uses it to interpret stacked spectra as functions of mass.
  • domain assumption The photometric density field and overdensity regions A/B/C from Estrada et al. (2023) correspond to real physical structures.
    The interpretation that 81 spectroscopically confirmed members trace infalling groups depends on the photometric map being physically correct. The paper does not independently re-derive the density field from the new redshifts.
  • domain assumption g-r color bimodality separates star-forming from passive galaxies.
    The paper classifies galaxies as red or blue solely by the (g-r)Kron color cut, then interprets stacked spectra accordingly in Section 5.1. This is a standard approximation, but it ignores dust reddening and AGN contamination.
  • standard math Lambda-CDM cosmology with Omega_m=0.3, Omega_Lambda=0.7, and H0=70 km/s/Mpc.
    Adopted at the end of Section 1 for converting angular scales to physical scales. This is a standard background assumption.

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Cite this review

Pith. "Pith review of Galaxies at the edges: a complete census of MACS J0416.1-2403 cluster." pith.science (2026). https://pith.science/paper/JIRZPC6F

@misc{pith2026250611216,
  author       = {Pith},
  title        = {Pith review of: Galaxies at the edges: a complete census of MACS J0416.1-2403 cluster},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JIRZPC6F}},
  note         = {Machine review of arXiv:2506.11216}
}
read the original abstract

Numerous studies have established that the environment influences the physical properties of a galaxy. While gas inflows supply the fuel for SF, high density and temperature conditions suppress SF activity through various quenching processes. Investigations into large scale structures, such as filaments and overdense regions in the cluster outskirts, have focused on the low z. To move to intermediate z and explore galaxy pathways combined with environmental effects, it is crucial to join wide field spectroscopy and deep photometry. Our primary objective is to spectroscopically analyze the photometric overdensities observed by Estrada et al.(2023) in the outskirts of massive cluster MACS J0416.1-2403 (z=0.397), interpreted as evidence of ongoing group infall, i.e. the pre processing scenario, and to investigate the behavior of galaxies in the outskirts about their g-r color, Mstar, and local density, emphasizing the influence of the environment on galaxy evolution. We conducted a spectroscopic analysis out to 5.5R200, using the AAOmega spectrograph. The large FoV and depth allowed us to explore galaxies up to the cluster periphery and across a wide Mstar range, reaching down to the limit of dwarf galaxies. Redshifts were obtained through independent but comparable methods: Redrock, EZ, and Redmost. We identified 148 new spectroscopic cluster members from a sample of 1236 objects. We found 81 galaxies located in filamentary and overdense regions, supporting the role of filamentary infall in the cluster mass assembly history. Our analysis revealed that galaxies in high density regions are more massive, redder, and more passive, compared to galaxies in low density regions that appear to be bluer, less massive, and more SF. These findings underscore the significance of environmental effects and the role of pre processing in shaping galaxy properties before cluster infall.

Figures

Figures reproduced from arXiv: 2506.11216 by the authors.

Figure 1
Figure 1. Imaging and redshifts spatial distribution for MACS0416. On the top left, the VST i-band image is shown, covering the 30x30 arcmin2 cluster region showing MUSE (red) and VIMOS (blue) redshifts, over the range z=[0.02-6.2]. The bottom left image shows the Hubble Frontier Fields (HFF) color image (2.8’ across), where MUSE integral field spectroscopy yields additional redshifts in the cluster core. The right color comp… view at source ↗
Figure 2
Figure 2. Top Panel: AAOmega spectrum of a galaxy in our sample (ID: MACS_64052446, z∼0.40), with the z estimated by using Redrock. Key emission and absorption lines are marked with dashed lines, following the color scheme in the legend. Bottom Panel: Variance of the spectrum. the lack of comprehensive observational campaigns targeting the cluster outskirts beyond 2-3 virial radii leaves a significant gap in our understanding… view at source ↗
Figure 3
Figure 3. VST i-band image covering 1 deg2 (∼ 20×20 Mpc2 ), over￾lapped with the 1236 AAOmega measured redshifts (turquoise points). The light blue circles with black edges represent the new 148 mem￾bers of MACS0416 from AAOmega catalog, in the redshift range z=[0.382 − 0.412]. The region where VIMOS or MUSE redshifts are available over z=[0.02 − 6.2] range is represented as a blue rectangle. The black circle corresponds to t… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Top left panel: redshift distribution of the 1233 sources extracted from the AAOmega spectra. Three objects with redshift ≥1 were excluded from the plot for a better visualization of the distribution; Bottom left panel: Zoom into the redshift range of the members selec…
Figure 5
Figure 5. Figure 5: Average spectral properties of our sample as a function of color and KKron as a proxy of the stellar mass. Left panel: Using a (g − r)Kron color cut, the sample was divided into red (72) and blue (76) galaxies, with their stacked spectra displayed in red and blue, resp…
Figure 6
Figure 6. Figure 6: Left Panel: Photometric density map of MACS0416 from Estrada et al. (2023), with all the new redshifts of objects with QF≥2 (1236) obtained with AAOmega overlaid (white circles), highlighting the new spectroscopic cluster members (148) (light blue circles). Right Panel…
Figure 7
Figure 7. Figure 7: Average spectral properties of our sample as a function of the local environment. Top panel: The stacked spectrum of the AAOmega members (148) is shown in black. The stacked spectra of galaxies located in overdense regions are shown in red, those in filamentary re￾gion…
Figure 8
Figure 8. Figure 8: Average spectral properties of our sample of red and blue galaxies as a function of the local environment. Left panel: the stacked spectrum of the population of red members (72) of MACS0416, is shown in dark red, at the top of the image. The entire sample was then divi…

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