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In void galaxies, the resolved molecular gas main sequence is the tightest and most time-stable of the three star-formation scaling relations, implying the environment sets which relation is fundamental.

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2026-08-01 07:21 UTC pith:IOSBCGOQ

load-bearing objection First resolved-CO void-galaxy scaling relations; the tight-rMGMS claim is plausible but needs a common-noise test before the environmental interpretation is secure. the 3 major comments →

arxiv 2607.21464 v1 pith:IOSBCGOQ submitted 2026-07-23 astro-ph.GA

ALMA CO-CAVITY II. Resolved Scaling Relations in Void Galaxies

S. B. De Daniloff , D. Espada , S. Duarte Puertas , Y. K. Gonz\'alez-Koda , G. Torres-R\'ios , S. F. S\'anchez , R. Garc\'ia-Benito , S. Verley
show 17 more authors
I. P\'erez M. Argudo-Fern\'andez A. Bongiovanni M. S\'anchez-Portal U. Lisenfeld M. I. Rodr\'iguez A. Conrado A. Jim\'enez B. Bidaran L. S\'anchez-Menguiano T. Ruiz-Lara A. Zurita P. V\'asquez-Bustos M. Alc\'azar-Laynez P. Villalba-Gonz\'alez E. Florido R. E. Miura
This is my paper
classification astro-ph.GA
keywords void galaxiesresolved scaling relationsmolecular gas main sequenceSchmidt-Kennicutt relationstar-forming main sequenceCO(1-0) interferometryintegral field spectroscopygalaxy environment
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.

The paper tries to establish that the large-scale environment changes which resolved galaxy scaling relation is the most fundamental. In 41 void galaxies observed with kiloparsec-resolution CO and optical IFU data, the resolved molecular gas main sequence (rMGMS) is the tightest relation, with 0.16 dex scatter, ahead of the resolved Schmidt-Kennicutt relation at 0.21 dex and the resolved star-forming main sequence at 0.24 dex — the opposite of what previous samples spanning all environments find. Galaxy-to-galaxy variations are the main source of scatter, yet the rMGMS is least affected, and removing deviant galaxies leaves its scatter unchanged. If right, this means void isolation suppresses the rapid star-formation variations that inflate the other two relations, so the rMGMS — interpreted as tracing the gravitational potential set by stellar and dark matter content — is the most stable relation over time. A sympathetic reader would care because it identifies a clean benchmark relation for undisturbed galaxies and shows that environment, not only internal physics, sets which law is primary.

Core claim

On kiloparsec-resolution CO(1-0) and optical IFU maps of 41 void galaxies, the authors fit three resolved scaling relations across 7,937 pixels and find that the resolved molecular gas main sequence (rMGMS) — molecular gas surface density vs. stellar mass surface density — is the tightest, at 0.16 dex scatter, versus 0.21 dex for the resolved Schmidt-Kennicutt relation and 0.24 dex for the resolved star-forming main sequence. This ordering reverses earlier resolved surveys spanning all environments, where the rSK is tightest. Galaxy-to-galaxy variations dominate the scatter, but the rMGMS is least affected; removing deviant galaxies leaves its scatter at 0.16 dex while the other two drop. Th

What carries the argument

The central object is the rMGMS, the resolved correlation between molecular gas surface density (Σ_H2) and stellar mass surface density (Σ⋆). The argument runs through two quantitative tools: ODR fits that assign each relation a 1σ scatter, and running-median offset analysis that measures how far each galaxy sits from the full-sample trend. The rMGMS carries the load by being both the tightest (0.16 dex) and the least variable galaxy-to-galaxy (σ_med = 0.14 dex vs 0.21 and 0.22), which the paper ties to its proposed physical origin: molecular gas concentrated in the gravitational potential set by the stellar and dark matter content.

Load-bearing premise

The load-bearing premise is that the scatter ordering (rMGMS < rSK < rSFMS) reflects the physics of void galaxies rather than the different dynamic ranges, sensitivities, and noise levels of the three surface-density maps; if the rMGMS only looks tightest because Σ⋆ and Σ_H2 maps are smoother and lower-noise than Σ_SFR, the environmental interpretation fails.

What would settle it

Refit the three relations under a matched control: restrict pixels to the dynamic range common to all three maps, or include the two-axis and upper-limit pixels with a survival-analysis fit (the paper's own appendices show the rSFMS slope drops to 1.005 and the rSK slope to 0.72 under those choices). If the rMGMS scatter then ceases to be the smallest — in particular if the rSK scatter falls to or below 0.16 dex — the claim that void isolation makes the rMGMS the tightest relation is falsified.

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

If this is right

  • If the rMGMS is the tightest in void galaxies, then environment, not just galaxy physics, determines which resolved scaling relation is primary; in sparse regions the gas-to-stellar-mass relation is the anchor.
  • The rMGMS can serve as a stable, low-scatter tracer of the gravitational potential in isolated galaxies: deviations from it should reflect slowly changing potential rather than rapid star-formation bursts.
  • The scatter of the rSK and rSFMS is largely set by galaxy-to-galaxy variations, and the extra rSK scatter relative to the rMGMS nearly disappears when deviant galaxies are removed — so short-timescale star-formation changes are mostly a galaxy-scale phenomenon.
  • The parametric form of the three relations in voids matches that found for galaxies in denser environments, so the relations themselves are universal while their scatter ordering is not.
  • Correlations between per-galaxy offsets in the three relations are reproduced by a mock sample with Gaussian noise and arise from projecting a three-dimensional Σ⋆-Σ_H2-Σ_SFR relation onto two-dimensional planes, not from secondary physical relations.

Where Pith is reading between the lines

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

  • Editorial inference: a direct test would sort galaxies by environment density and measure the scatter ordering continuously; the prediction is that the rSK-to-rMGMS scatter ratio grows with the fraction of interacting galaxies.
  • Editorial inference: the appendices show the fitted slopes are sensitive to pixel selection — including two-axis detections changes the rSFMS slope from 1.249 to 1.005 and adds 147.8% more pixels, and including upper limits changes the rSK slope from 1.282 to 0.72 — so the tightness ordering should be re-checked on a matched dynamic range and sensitivity before the environmental interpretation is
  • Editorial inference: if the ordering holds, void galaxies become a clean laboratory for calibrating CO-based gravitational-potential tracers and for testing simulations of galaxy evolution without interaction-driven outliers.

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

3 major / 4 minor

Summary. This paper presents the resolved Schmidt-Kennicutt relation (rSK), resolved molecular gas main sequence (rMGMS), and resolved star-forming main sequence (rSFMS) for 41 void galaxies from the ALMA CO-CAVITY survey, combining ALMA CO(1-0) maps with CAVITY/MaNGA IFU data at 2.5 arcsec resolution. From 7,937 pixels detected in all three axes, the authors derive ODR fits with slopes 1.282, 0.955, and 1.249 and scatters 0.21, 0.16, and 0.24 dex for rSK, rMGMS, and rSFMS, respectively, concluding that the rMGMS is the tightest resolved relation in void galaxies. Individual-galaxy fits, running-median offset analyses, a truncated sample of 15 galaxies, and mock projection tests are used to argue that galaxy-to-galaxy variations dominate the scatter and that the rMGMS is least affected, leading to the hypothesis that the rMGMS traces the gravitational potential on longer timescales and is the most stable relation in voids. Appendices test local alpha_CO values, pixels detected in two axes, and survival analysis with upper limits.

Significance. If the central claim holds, this is the first resolved scaling-relation comparison in void galaxies and would challenge the usual rSK-tightest ordering found in denser environments, with direct implications for environmental dependence and the timescale interpretation of resolved scaling relations. The paper has substantial strengths: it presents a unique, kpc-resolution CO+IFU sample of void galaxies; the 10,000 bootstrap resamples quantify the statistical significance of the scatter differences; the survival analysis in Appendix D is a serious attempt to include upper limits; the local-alpha_CO test in Appendix A checks an important systematic; and a pipeline is released. These strengths make the empirical result credible as a description of the selected pixels. However, the environmental/timescale interpretation is not yet secured because the headline scatter ordering is compared across maps with different noise levels and dynamic ranges, and the truncated-sample analysis is partly circular. The result is potentially important enough to warrant major revision rather than rejection.

major comments (3)
  1. [Section 3, Table 1; Section 5.1] The headline scatter ordering is interpreted physically, but no common-noise control is performed. The paper states that the median uncertainties are 0.05 dex for Sigma_H2 and Sigma_* and 0.09 dex for Sigma_SFR (Sect. 5.1). Unweighted ODR scatter is inflated by a noisier axis, so the observed ordering (rMGMS 0.16, rSK 0.21, rSFMS 0.24 dex) is qualitatively what would be expected if the intrinsic relations had similar scatter and the extra Sigma_SFR noise was responsible for the difference. The 10,000 bootstrap resamples only resample the observed pixels and therefore cannot separate noise-driven scatter from intrinsic scatter. Please add a quantitative test, e.g., degrading Sigma_H2 and Sigma_* to the noise level of Sigma_SFR, fitting with measurement-error weights, or otherwise demonstrating that the ordering survives a common-noise treatment.
  2. [Appendix C; Appendix D; Section 3] The statement that including two-axis pixels and upper limits 'does not significantly alter the relations' is not fully supported by the appendices. Appendix C shows that the rSFMS slope changes from 1.249 to 1.005 when 19,668 two-axis pixels are used (+147.8% pixels), with a plateau at low Sigma_*; Appendix D shows that the rSK slope changes from 1.282 to 0.72 when upper limits are included, and all fitted slopes become sub-linear. These changes show that the main sample's pixel selection and dynamic range affect the fitted relations. The appendices are useful, but they do not prove that the scatter ordering survives a homogeneous selection or a common dynamic-range treatment; the rMGMS-tightest conclusion needs a single consistent analysis applied to all three relations with the same pixel selection and noise treatment.
  3. [Section 5; Section 4.4] The truncated-sample analysis is partly circular. The 15 galaxies in the truncated sample are selected as following the full-sample trend for all three resolved SRs (Sect. 4.4), and this same subsample is then used to conclude that the rMGMS scatter is unchanged and remains the tightest. Removing galaxies classified as deviant in rSK and rSFMS, but not in rMGMS, would be informative; removing galaxies selected on all three relations, including rMGMS, cannot by itself demonstrate that the rMGMS is less affected by galaxy-to-galaxy variations. Please either select the truncated sample using only rSK/rSFMS deviations, or present this analysis as a consistency check rather than as independent evidence for the environmental claim.
minor comments (4)
  1. [Section 5, Fig. 6 caption] The text says 'distributions of medians of Delta_rSK, Delta_rSFMS and Delta_rSFMS'; the last should presumably read Delta_rMGMS.
  2. [Appendix D] The LEO-Py scatter is a vertical OLS scatter while the ODR scatter is orthogonal; comparing the ordering of these two metrics directly is not apples-to-apples. Please state explicitly that the ordering under survival analysis is based on a different scatter definition.
  3. [Section 3, Fig. 1 caption] The phrase 'contours show levels of inclusion of pixels of 5, 10, 20, 50 and 80%' could be clarified: are these percentages of the total pixel sample enclosed, or kernel-density levels?
  4. [Section 5.1] The mock sample is generated from the fitted relations and Gaussian noise with widths 0.1, 0.1, 0.2 dex. This is a useful projection test, but it assumes the noise model; the conclusion that the correlations are not physical should be phrased as conditional on that model.

Circularity Check

0 steps flagged

No circular derivation: the resolved scatter ordering is a direct empirical fit, not a fitted parameter recycled as a prediction.

full rationale

The central result of the paper is an empirical measurement: ODR fits to 7,937 detected pixels (Sect. 3, Table 1) yield σ_rMGMS=0.16 dex, σ_rSK=0.21 dex, σ_rSFMS=0.24 dex, with 10,000 bootstrap resamples confirming the ordering. This ordering is not obtained by construction from any assumed model; the fit parameters are not recycled as predictions. The mock sample in Sect. 5.1 is generated from the fitted relations but is used as a null distribution for offset correlations, which is an appropriate statistical test rather than a circular prediction. Paper I self-citations supply data products (CO masks, αCO) and global relations, but the resolved pixel-level fits are performed independently here and are benchmarked against external surveys (ALMaQUEST XI, EDGE-CALIFA). The truncated-sample analysis in Sect. 5 is a supplementary confirmation that selects galaxies visually classified as following the full-sample trend; because the main scatter ordering is already established from the full sample before truncation, this step is not load-bearing and does not make the central claim circular. Appendices C and D demonstrate sensitivity to pixel selection and upper limits, which is a robustness/measurement concern rather than circularity. No step in the derivation chain reduces to the claim being derived.

Axiom & Free-Parameter Ledger

2 free parameters · 7 axioms · 0 invented entities

The paper introduces no new particles, forces, or conserved quantities. Its central numerical result rests on standard extragalactic calibrations (αCO, Hα SFR, stellar-population synthesis), a specific pixel-selection choice, and a cited gravitational-potential interpretation of the rMGMS. The free parameters are data-analysis choices inherited from prior work or selected by hand; the appendices test the two most important ones (αCO and pixel selection).

free parameters (2)
  • Global metallicity-dependent CO-to-H2 conversion factor αCO (per galaxy) = mean 4.56 ± 1.66 M⊙ (K km s−1 pc2)−1; non-detected galaxies 5.82–8.17
    Adopted from Paper I / Rodríguez et al. 2024; sets the Σ_H2 zero-point and affects rSK and rMGMS intercepts and scatter. Appendix A shows local αCO does not change the ordering, so this parameter does not drive the central result but is a genuine free input.
  • Detection threshold parameters (3σ, ΔV_cloud=40 km s−1) = 3σ; 40 km/s
    Chosen by hand to define detected pixels and upper limits; affects how many pixels enter the fits and the survival-analysis slopes (App. D).
axioms (7)
  • domain assumption ΛCDM cosmology with H0=70 km/s/Mpc, Ωm=0.3, T_CMB=2.725 K; Chabrier IMF
    Adopted in the introduction; converts distances and masses. Standard but not derived here.
  • domain assumption CO(1-0) luminosity traces molecular gas mass through αCO
    §2.1: Σ_H2 is computed from masked CO(1-0) moment-0 maps with a global metallicity-dependent αCO.
  • domain assumption Hα emission traces SFR via the Kennicutt & Evans calibration and Case B ratio 2.86
    §2.2: SFR maps are computed from extinction-corrected Hα using Hβ/Hα=2.86; this underpins the rSK and rSFMS axes.
  • domain assumption pyPipe3D stellar population fits and dezonification recover Σ⋆ maps
    §2.2: Σ⋆ comes from spectral fitting with the MaStar_sLOG library; Voronoi-binned zones are dezonified to recover spatial information.
  • domain assumption Smoothing ALMA maps to 2.5″ and regridding to optical templates preserves the relative scatter of the relations
    §2.3 and App. B: homogenisation may affect dynamic range and scatter; this is not independently validated.
  • domain assumption The d25 elliptical mask and 3σ detections select an unbiased pixel population for comparing scatters
    §2.4: the 7,937-pixel sample is defined by these criteria; Apps. C/D show the fitted slopes are sensitive to this selection.
  • domain assumption The rMGMS reflects molecular gas concentration in the gravitational potential of stars and dark matter (Lin et al. 2019; Baker et al. 2022)
    §6: this cited interpretation underpins the timescale hypothesis but is not derived or tested in this paper.

pith-pipeline@v1.3.0-alltime-deepseek · 33466 in / 12790 out tokens · 125097 ms · 2026-08-01T07:21:16.599886+00:00 · methodology

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read the original abstract

Scaling relations involving star formation rates (SFRs), molecular gas mass, and stellar mass are key to understand galaxy evolution, and have previously been explored at resolved scales. However, they have not been examined with particular emphasis on the large-scale environments (LSEs). In this work, we study the resolved Schmidt-Kennicutt relation (rSK), molecular gas main sequence (rMGMS) and star-forming main sequence (rSFMS) from a sample of 41 void galaxies (VGs) residing in the least dense regions of the Universe. Using high-resolution interferometric CO(1-0) data and optical IFU data from the ALMA CO-CAVITY and CAVITY surveys at scales of 2.5" (0.8-2.1 kpc), we study these relations for the full sample as well as for individual galaxies in voids. We fit the relations, finding a similar parametrisation as that used for galaxies from all LSEs. However, the rMGMS is the tightest of the three relations ($\sigma_{rMGMS}=0.16$ dex, $\sigma_{rSK}=0.21$ dex, and $\sigma_{rSFMS}=0.24$ dex), unlike in other samples. We find that a large source of deviations in the relations comes from galaxy-to-galaxy variations. However, the rMGMS is less affected by these variations. It has been suggested that the rMGMS arises from the concentration of molecular gas within the gravitational potential set by the stellar content and dark matter. We hypothesise that deviations from the rMGMS trace changes in the gravitational potential occurring on longer time-scales, whereas deviations in the rSK and the rSFMS are driven by more rapid variations in the SFR. This distinction is particularly relevant for our sample of VGs because the 41 ALMA CO-CAVITY VGs are more isolated than galaxies in other LSEs, and therefore are less affected by events that can significantly alter the gas distribution or trigger SF on short time-scales. In this sense, the rMGMS is likely the most stable of these relations over time.

Figures

Figures reproduced from arXiv: 2607.21464 by A. Bongiovanni, A. Conrado, A. Jim\'enez, A. Zurita, B. Bidaran, D. Espada, E. Florido, G. Torres-R\'ios, I. P\'erez, L. S\'anchez-Menguiano, M. Alc\'azar-Laynez, M. Argudo-Fern\'andez, M. I. Rodr\'iguez, M. S\'anchez-Portal, P. V\'asquez-Bustos, P. Villalba-Gonz\'alez, R. E. Miura, R. Garc\'ia-Benito, S. B. De Daniloff, S. Duarte Puertas, S. F. S\'anchez, S. Verley, T. Ruiz-Lara, U. Lisenfeld, Y. K. Gonz\'alez-Koda.

Figure 1
Figure 1. Figure 1: Resolved SRs for the 41 ALMA CO-CAVITY galaxies. We show the distribution of 7 937 detected pixels with the filled contours: (left) in red for the rSK, (mid) in purple for the rMGMS, and (right) in blue for the rSFMS. In each panel, we show in the lower-left corner the median of the error bars. The orthogonal distance regression (ODR) fit results are shown in the upper-left legend of each panel and are rep… view at source ↗
Figure 3
Figure 3. Figure 3: Resolved molecular gas main sequence for all ALMA CO-CAVITY VGs. The symbols and colours are equivalent to those of [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Resolved star-forming main sequence for all ALMA CO-CAVITY VGs. The symbols and colours are equivalent to those of Figs. 2 and 3. log10(sSFR/yr−1 ) ∼ [−10.0, −9.4] (the standard deviation for the full sample is 0.36 dex). As the sSFR is the SFR per unit of M⋆, it seems logical to observe similar trends on the relations involv￾ing ΣSFR and Σ⋆ for these galaxies. − rSK and rSFMS normal, rMGMS above: 27657 an… view at source ↗
Figure 5
Figure 5. Figure 5: Running medians of resolved SRs for the rSK (left panel), rMGMS (mid panel) and rSFMS (right panel), for the 35 detected galaxies. In each panel, we show the individual detected pixels with grey data points, the running medians calculated for each galaxy individually with the coloured curves, and the one calculated for the full-sample distribution with the black curve. We apply a linear fit to the full-sam… view at source ↗
Figure 6
Figure 6. Figure 6: Median deviations of individual galaxies in the resolved SRs with respect to the running median of the full-sample dis￾tribution of pixels. In the top panel we show the distributions of medians of ∆rSK, ∆rSFMS and ∆rSFMS for the complete sam￾ple of 35 detected galaxies. In the bottom panel we show the same distributions for the truncated sample of 15 galaxies (see text for explanation). In each panel, we s… view at source ↗
Figure 7
Figure 7. Figure 7: Galaxy-by-galaxy offsets from the full-sample trends of the resolved SRs compared between each relation. In each panel the data points are the the median offsets, with the rSFMS − rMGMS diagram in the left panel, the rSFMS − rSK diagram in the mid panel, and the rSK − rMGMS diagram in the right panel. The error bars are the median absolute deviation of each value. In red we highlight the 15 galaxies of the… view at source ↗

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Reference graph

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