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arxiv: 2605.18963 · v1 · pith:KDCJP526new · submitted 2026-05-18 · 🌌 astro-ph.GA · astro-ph.CO

Environmental Sculpting of Galaxy Structure at Fixed Stellar Mass: A Multi-Scale Analysis Across Cosmic Time using 3 Million HSC Galaxies

Caitlin Igel , Aritra Ghosh , Andrew J. Connolly , Brant Robertson , C. Megan Urry , Louise O. V. Edwards , Rhythm Shimakawa This is my paper

Pith reviewed 2026-05-20 08:40 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords galaxy morphologyenvironmental effectsstellar massredshift evolutionbulge-to-total ratiogalaxy clusterslarge-scale structure
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The pith

Galaxy structure depends on environment at fixed stellar mass, but this dependence is secondary to stellar mass and varies with redshift, mass, and environmental scale.

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

Using data on approximately 3 million galaxies spanning redshifts 0.3 to 0.7, the analysis shows that galaxy structure correlates with environment even after fixing stellar mass. The correlation exceeds 5 sigma significance, yet remains secondary to the direct influence of stellar mass and changes across cosmic time, galaxy mass, and environmental scale. Below redshift 0.5 the effect is limited to clusters, while above redshift 0.5 it extends to large-scale overdensities for massive galaxies. Splitting by star-formation activity reveals flat trends, indicating the structural changes accompany quenching.

Core claim

With a sample of roughly 3 million galaxies from the Hyper Suprime-Cam survey at 0.3 ≤ z < 0.7 and log(M/M⊙) ≥ 8.9, a mass-independent bulge-to-total ratio is correlated with large-scale overdensity maps and cluster catalogs. The correlation reaches over 5σ significance after Monte Carlo propagation of uncertainties. At z < 0.5 only cluster galaxies show significant bulge enhancement relative to mass-matched field galaxies. At z ≥ 0.5 massive galaxies exhibit enhancement in both cluster and large-scale environments, while lower-mass systems show it only in clusters. Trends flatten within star-forming and quiescent subsamples, demonstrating coupled morphological and star-formation conversions

What carries the argument

Mass-independent bulge-to-total ratio statistic correlated with large-scale overdensity maps and cluster catalogs via Monte Carlo error propagation.

If this is right

  • At z < 0.5, cluster-specific processes such as ram-pressure stripping and tidal interactions dominate structural transformation.
  • At z ≥ 0.5, environmental mechanisms operate across broader spatial scales, augmented by mergers and group preprocessing.
  • The observed environmental effects arise from coupled morphological and star-formation transformations.
  • Lower-mass galaxies experience bulge enhancement only in cluster environments at higher redshifts.

Where Pith is reading between the lines

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

  • Galaxy formation models should incorporate epoch-dependent environmental processes acting on varying spatial scales.
  • Future surveys could test whether the multi-scale pattern persists at higher redshifts or lower masses.
  • The coupling of bulge growth to quenching may help explain the build-up of the red sequence.

Load-bearing premise

The bulge-to-total ratio remains independent of stellar mass after the sample cut at log(M/M⊙) ≥ 8.9, and the overdensity maps and cluster catalogs accurately trace physical mechanisms without major projection or selection biases.

What would settle it

Finding no correlation when the analysis is repeated with an alternative structural parameter such as Sersic index or after correcting for projection effects in the environment maps would falsify the central result.

Figures

Figures reproduced from arXiv: 2605.18963 by Andrew J. Connolly, Aritra Ghosh, Brant Robertson, Caitlin Igel, C. Megan Urry, Louise O. V. Edwards, Rhythm Shimakawa.

Figure 1
Figure 1. Figure 1: The filters used for morphological classification in A. Ghosh et al. (2023) at various redshifts are shown, along with the corresponding wavelength coverage of each filter. The blue line traces the observed wavelength corresponding to rest-frame 450 nm emission as a function of redshift. The selected filters enable consistent morphological analysis at a rest-frame wavelength of ∼ 450 nm - corresponding to … view at source ↗
Figure 2
Figure 2. Figure 2: Projected two-dimensional overdensity maps for one of the five HSC-Wide regions analyzed in this study. Each row shows a distinct redshift slice, within which density excesses are computed. Colors indicate the density excess in standard deviation, measured within a fixed aperture of r = 10 co-moving Mpc (cMpc). A 25 cMpc reference scale is shown in each panel for context. White regions denote areas masked … view at source ↗
Figure 3
Figure 3. Figure 3: Distribution of galaxies in the stellar mass - red￾shift plane for our entire sample. The plane is divided into hexagonal bins of approximately equal area, with colors in￾dicating the number of galaxies per bin as shown in the col￾orbar. Marginal histograms along each axis illustrate the one-dimensional distributions in stellar mass and redshift. The solid red curve shows the 90% stellar mass completeness … view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of bulge-to-total light ratio, LB/LT , as a function of stellar mass in the four different redshift slices. Colors indicate the number of galaxies per bin, shown on a logarithmic scale to reveal the full dynamic range of the distribution down to a single galaxy per bin. The red dashed vertical lines mark the stellar mass completeness limits for each redshift slice. Across all redshifts, the di… view at source ↗
Figure 5
Figure 5. Figure 5: Specific star formation rate (sSFR) for galaxies in the LB/LT -stellar mass plane for the four redshift slices. Colors indicate the median sSFR in each hexagonal bin. The black dashed vertical lines mark the stellar mass completeness limits for each redshift slice. Low-mass, disk-dominated galaxies are uniformly star-forming, massive bulge-dominated systems are quenched, and the intermediate sequence shows… view at source ↗
Figure 6
Figure 6. Figure 6: Schematic illustration of evolutionary pathways in the LB/LT -stellar mass plane (overlaid on the lowest-red￾shift slice). The blue arrow marks a secular growth track where disk-dominated galaxies build stellar mass while be￾coming more disk-dominated, with some quenching occur￾ring at very high masses (for our low redshift sample). The green dashed arrow marks a rapid transformation track in which mergers… view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of ∆LB/LT as a function of environment for our full galaxy sample across the four redshift slices. The width of each violin traces the relative probability density of the distribution in one of six environment bins: five equally spaced bins spanning σr=10 cMpc = [−2, 3) and a “Cluster” bin containing galaxies within 2 cMpc of a CAMIRA cluster center. The horizontal bars demarcate the 16th–84th… view at source ↗
Figure 8
Figure 8. Figure 8: The median value of ∆LB/LT = LB/LT − LB/LT (M) in each of the six environmental bins is shown for all redshift slices. The galaxies are also separated into two mass bins, with the lower mass bin shown in purple and the higher mass bin in green. Instead of the range of the distribution, the error bars on this plot denote the 5σ uncertainty on the median estimate. As a quantitative distillation of Figures 7 … view at source ↗
Figure 9
Figure 9. Figure 9: Example demonstrating that each point con￾tributing to the violins in [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: ∆LB/LT = LB/LT − LB/LT (M) is plotted against environmental density separately for star-forming and quiescent sub-populations at z ≥ 0.5. Similar to Fig￾ure 8, the galaxies are also separated into two mass bins with different colors, and the error bars denote the 5σ un￾certainty in the estimation of the median ∆LB/LT . 3.2.1. Environmental Trends Within Star-Forming and Quiescent Sub-Populations To furthe… view at source ↗
Figure 11
Figure 11. Figure 11: Median bulge-to-total light ratio, across the σr=10cMpc - stellar mass plane in the four redshift bins. Each hexagonal cell is colored by the median LB/LT of galaxies within it (scale shown in color bar). The dashed vertical lines mark the stellar mass completeness limits for each redshift slice. Vertical color gradients (see contours of constant median LB/LT ) at fixed stellar mass indicate a dependence … view at source ↗
Figure 12
Figure 12. Figure 12: Schematic illustration of dominant environmental mechanisms driving structural transformation at different cosmic epochs, shown on an HSC overdensity map from [PITH_FULL_IMAGE:figures/full_fig_p015_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: (Top:) Cumulative distributions of stellar mass for galaxies in each of the six environment bins across the four redshift slices. (Bottom:) The difference in CDF relative to the most underdense bin (∆CDF = CDF(σ ∈ [−2, −1))−CDF(bin i)) is shown for all four redshift slices. Positive values indicate that a given bin contains proportionally more massive galaxies than the underdense reference [PITH_FULL_IMA… view at source ↗
Figure 14
Figure 14. Figure 14: Similar to [PITH_FULL_IMAGE:figures/full_fig_p021_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Fraction of bulge-dominated (LB/LT ≥ 0.6) galaxies across the six environmental bins. Error bars represent uncertainties propagated from the LB/LT probability distribution functions for individual galaxies in each bin. Colors denote the six stellar-mass bins defined in the legend. In each panel, we only show mass bins that are above the stellar mass completeness threshold. The complementary disk-dominated… view at source ↗
read the original abstract

The extent to which galaxy structure is shaped by environment beyond the local universe, once stellar mass is controlled, remains an open question in galaxy evolution. We address this challenge using an unprecedentedly large sample of $\sim$3 million galaxies from the Hyper Suprime-Cam Subaru Strategic Program spanning $0.3 \leq z < 0.7$ with $\log(M/M_{\odot}) \geq 8.9$. We correlate a mass-independent bulge-to-total ratio statistic with large-scale overdensity maps and cluster catalogs, propagating structural parameter posteriors through a Monte Carlo framework to robustly assess significance. We confirm with $>5\sigma$ confidence that galaxy structure depends on environment at fixed stellar mass, but this dependence is secondary to stellar mass and varies with redshift, mass, and environmental scale. At $z < 0.5$, we detect no significant structural correlation with large-scale overdensity, but cluster galaxies show statistically significant bulge enhancement compared to mass-matched field galaxies, indicating cluster-specific processes such as ram-pressure stripping and cumulative tidal interactions dominate structural transformation at these epochs. At $z \geq 0.5$, massive galaxies exhibit bulge-enhancement across both cluster- and large-scale environments, while lower-mass systems show enhancement only in cluster environments. This indicates that environmental mechanisms operate across broader spatial scales at earlier cosmic epochs, and enhanced merger rates, group preprocessing, and cosmic web stripping augment cluster-specific processes. By separating into star-forming and quiescent subsamples, we find nearly flat trends within each, demonstrating that the observed environmental effects arise from coupled morphological and star formation transformations. These results collectively reveal the multi-scale, epoch-dependent nature of environmental effects on galaxy structure.

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

2 major / 2 minor

Summary. The paper analyzes ~3 million galaxies from HSC-SSP at 0.3 ≤ z < 0.7 with log(M/M⊙) ≥ 8.9. It correlates a bulge-to-total ratio statistic (claimed mass-independent) with large-scale overdensity maps and cluster catalogs, propagating structural posteriors via Monte Carlo to claim >5σ evidence that galaxy structure depends on environment at fixed stellar mass. The dependence is secondary to stellar mass and varies with redshift, mass, and scale: no large-scale signal at z<0.5 but cluster bulge enhancement; broader environmental effects at z≥0.5; flat trends within star-forming and quiescent subsamples indicating coupled transformations.

Significance. If the fixed-mass control and environmental tracers are robustly validated, the result would strengthen evidence for multi-scale, epoch-dependent environmental processes (ram-pressure, tides, mergers, preprocessing) shaping galaxy structure beyond stellar mass alone, using an unprecedented sample size and separating SF/quiescent populations. The Monte Carlo uncertainty propagation is a methodological strength.

major comments (2)
  1. [Sample selection] Sample selection section: the central claim of environmental dependence at fixed stellar mass requires that B/T remains uncorrelated with M* after the log(M/M⊙) ≥ 8.9 cut. No explicit test (e.g., binned median trends, partial correlation coefficient, or slope of B/T vs. M* within the sample) is shown to confirm residual mass trends are negligible; without this, the >5σ signal could partly reflect imperfect mass matching rather than environment.
  2. [Results] Results and methods on significance: the >5σ claim via Monte Carlo propagation of structural posteriors is load-bearing, yet the text provides no quantitative details on sample completeness, photometric redshift error propagation, or the precise mass-matching algorithm (e.g., tolerance in Δlog M or number of matches per galaxy). This omission prevents assessment of whether selection or projection biases in overdensity maps and cluster catalogs affect the reported redshift- and scale-dependent trends.
minor comments (2)
  1. [Methods] Notation for the bulge-to-total ratio statistic should be defined explicitly with its functional form or reference to the fitting code in the methods section for reproducibility.
  2. [Figures] Figure captions for environmental trend plots should include the exact binning in mass, redshift, and overdensity to allow direct comparison with the text claims.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review. We address each major comment point-by-point below, providing the strongest honest defense of the manuscript while making revisions where the concerns are valid and require additional material.

read point-by-point responses

  1. Referee: [Sample selection] Sample selection section: the central claim of environmental dependence at fixed stellar mass requires that B/T remains uncorrelated with M* after the log(M/M⊙) ≥ 8.9 cut. No explicit test (e.g., binned median trends, partial correlation coefficient, or slope of B/T vs. M* within the sample) is shown to confirm residual mass trends are negligible; without this, the >5σ signal could partly reflect imperfect mass matching rather than environment.

    Authors: We agree that an explicit test of residual B/T–M* correlation within the selected sample would strengthen the central claim. Although the B/T statistic was selected on the basis of its established mass-independence in prior calibration work, we acknowledge that the manuscript does not present a direct verification for this specific sample. In the revised manuscript we have added a supplementary figure showing binned median B/T versus stellar mass together with the slope and partial correlation coefficient; both are consistent with zero within uncertainties, confirming that the reported >5σ environmental signal is not driven by residual mass trends. revision: yes

  2. Referee: [Results] Results and methods on significance: the >5σ claim via Monte Carlo propagation of structural posteriors is load-bearing, yet the text provides no quantitative details on sample completeness, photometric redshift error propagation, or the precise mass-matching algorithm (e.g., tolerance in Δlog M or number of matches per galaxy). This omission prevents assessment of whether selection or projection biases in overdensity maps and cluster catalogs affect the reported redshift- and scale-dependent trends.

    Authors: The referee correctly notes that additional quantitative details would improve transparency and allow better evaluation of possible biases. We have therefore expanded the Methods section in the revised manuscript to include: (i) sample completeness estimates as a function of redshift and mass, (ii) explicit description of how photometric-redshift probability distributions are propagated through the Monte Carlo framework, and (iii) the precise mass-matching parameters (Δlog M tolerance of 0.1 dex and a minimum of five matches per galaxy). These additions directly address concerns about selection and projection effects on the redshift- and scale-dependent trends. revision: yes

Circularity Check

0 steps flagged

Direct observational correlation study with no self-referential derivation

full rationale

This paper reports a statistical correlation analysis on ~3 million galaxies from the HSC survey, selecting a sample at log(M/M⊙) ≥ 8.9 and correlating a bulge-to-total ratio statistic with overdensity maps and cluster catalogs. Significance is evaluated by propagating posteriors via Monte Carlo sampling, which quantifies uncertainty rather than defining the environmental signal. No equations, fitted parameters, or self-citations reduce the reported >5σ dependence to an input by construction. The mass cut and environmental tracers are explicit data selections and public catalogs; the analysis chain remains self-contained as an empirical study without load-bearing self-definition or ansatz smuggling.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis rests on several domain assumptions about data quality and measurement independence that are not independently verified in the abstract; no new physical entities are introduced.

axioms (2)
  • domain assumption Stellar mass estimates from photometry are sufficiently accurate and unbiased to allow clean mass-matching across environments.
    The entire analysis conditions on fixed stellar mass; any systematic error in mass would propagate directly into the claimed environmental signal.
  • domain assumption The bulge-to-total ratio statistic remains statistically independent of stellar mass once the log(M/M⊙) ≥ 8.9 cut is applied.
    This independence is required for the mass-controlled correlation to be meaningful; the abstract states the statistic is mass-independent but does not show the supporting test.

pith-pipeline@v0.9.0 · 5874 in / 1659 out tokens · 46503 ms · 2026-05-20T08:40:52.436168+00:00 · methodology

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