COALAS III: The ATCA CO(1-0) look at the growth and death of H$\alpha$ emitters in the Spiderweb protocluster at z=2.16

A. Naufal; A. P. Thomson; B. H. C. Emonts; B. Indermuehle; B. Ziegler; C. De Breuck; C. D'Eugenio; C. M. Casey; G. Drouart; G. Miley

REVIEW 4 major objections 5 minor 1 cited by

COALAS III: The ATCA CO(1-0) look at the growth and death of H$\alpha$ emitters in the Spiderweb protocluster at z=2.16

T0 review · 4 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The Spiderweb protocluster's H-alpha emitters split sharply by gas fraction near $\log M_*/M_\odot\approx10.5$, and this paper argues that AGN feedback plus gas overconsumption, not slow starvation, drives their quenching.

desk verdict Valuable new CO(1-0) data for a z>2 protocluster, but the headline two-regime gas fraction is partly built on biased upper limits and needs a censored-data reanalysis before the steep transition is taken at face value. read the letter →

arxiv 2411.12138 v1 pith:6JQLXCAX submitted 2024-11-19 astro-ph.GA

J. M. Pérez-Martínez , H. Dannerbauer , B. H. C. Emonts , J.R. Allison , J. B. Champagne , B. Indermuehle , R. P. Norris , P. Serra

show 21 more authors

N. Seymour A. P. Thomson C. M. Casey Z. Chen K. Daikuhara C. De Breuck C. D'Eugenio G. Drouart N. Hatch S. Jin T. Kodama Y. Koyama M. D. Lehnert P. Macgregor G. Miley A. Naufal H. Röttgering M. Sánchez-Portal R. Shimakawa Y. Zhang B. Ziegler

This is my paper · ORCID

classification astro-ph.GA

keywords moleculargasCO(1-0)protoclustergalaxyquenchingAGNfeedbackfractionH-alphaemittersSpiderweb

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

Using ATCA CO(1-0) imaging of 43 spectroscopically confirmed H-$\alpha$ emitters in the Spiderweb protocluster at $z=2.16$, this paper measures or limits the cold molecular gas masses of a forming cluster's typical star-forming galaxies. It finds that the sample splits into two gas regimes around $\log M_*/M_\odot\approx10.5$: lower-mass galaxies have gas fractions at or near unity, while more massive galaxies often drop below $f_{\rm gas}\approx0.4$ and are frequently AGN (12 of 20). The authors argue that these massive galaxies will exhaust their fuel and become passive by $1

What carries the argument

The load-bearing measurement is the molecular gas fraction $f_{\rm gas}=M_{\rm mol}/(M_*+M_{\rm mol})$, derived from CO(1-0) fluxes using a fixed conversion factor $\alpha_{\rm CO}=4.36\,M_\odot\,({\rm K\,km\,s^{-1}\,pc^2})^{-1}$. Ten sources have detections from the COALAS catalog; for the other 33, upper limits are obtained by integrating only positive flux channels within $\pm500$ km/s of each H-$\alpha$ redshift and taking the brightest spaxel in a $3\times3$ grid around the source. Stacking the spectra in three bins (low mass, massive non-AGN, massive AGN) gives average gas fractions of $0.86\pm0.04$, $0.55\pm0.04$, and $0.38\pm0.05$, and a logistic function in the $f_{\rm gas}$--$M_*$ plane places the transition at $\log M_*/M_\odot=10.93\pm0.05$. The phase-space parameter $\eta=(R/R_{200})(|\Delta v|/\sigma)$ then ties gas content to position within the forming cluster.

What would settle it

Re-observe the 33 non-detected H-$\alpha$ emitters with higher sensitivity, for example with ALMA Band 1, and re-derive their CO(1-0) fluxes using a full Bayesian upper-limit treatment that includes negative noise channels; if the true gas fractions of the $\log M_*/M_\odot<10.5$ galaxies fall substantially below 0.8, the reported steep transition at $\log M_*/M_\odot\approx10.5$ would not be as sharp as claimed.

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Extended reading notes

Core claim

This paper reports the cold molecular gas content, traced by CO(1-0), for 43 spectroscopically confirmed H-$\alpha$ emitters in the Spiderweb protocluster at $z=2.16$, using 10 detections and 33 upper limits. It finds that the total gas fraction $f_{\rm gas}=M_{\rm mol}/(M_*+M_{\rm mol})$ drops sharply from values near unity at $\log M_*/M_\odot<10.5$ to values often below 0.4 above that mass. At the massive end, 12 of 20 sources show AGN signatures, and stacking gives $f_{\rm gas}\approx0.55$ for massive galaxies without AGN and $f_{\rm gas}\approx0.38$ for AGN candidates. The paper argues that this sharp transition, combined with depletion times of 1-3 Gyr, means these galaxies will become passive by $1<z<1.6$, and that the quenching mechanism is rapid cold-gas depletion driven by AGN feedback plus overconsumption rather than starvation alone.

Load-bearing premise

The sharp transition depends on treating 33 CO(1-0) upper limits as gas measurements, but those limits were made by summing only positive noise fluctuations within a velocity window and taking the brightest of nine spatial pixels, a procedure the paper itself notes can overestimate fluxes.

Editorial extensions

If this is right

If the gas-fraction break is real, the low-mass H-alpha emitters are still being replenished by cold inflows from the cosmic web, since their gas fractions approach unity even as they sit on the main sequence.
With typical depletion times of 1-3 Gyr and no further inflows, the Spiderweb HAEs would become passive by $1<z<1.6$, matching the epoch when massive clusters build their red sequences.
The stacked gas fractions ($F_{\rm gas}\approx0.55$ without AGN, $F_{\rm gas}\approx0.38$ for AGN candidates) imply that nuclear activity removes or heats a substantial fraction of the cold gas on top of ordinary star formation at $M_*\gtrsim10^{10.5}\,M_\odot$.
Because star formation stays on the main sequence while gas fractions decline toward the core, environmental effects act through reducing the fuel supply rather than by directly boosting or suppressing star formation.

Reading between the lines

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

If the threshold is universal, deep CO(1-0) surveys in other $z\approx2$ protoclusters and in the field should reproduce the same logistic break, and tracing how that break moves with redshift would separate a mass-driven quenching clock from an environment-driven one.
A direct test of the proposed mechanism would compare black-hole-to-stellar-mass ratios among the massive HAEs: the model predicts that the most gas-poor objects host the most massive black holes even when their current AGN activity is faint.
Combining the phase-space gas-fraction gradient with the detection of a nascent intracluster medium could yield a first empirical map of where cold streams stop penetrating a forming cluster, turning the proposed starvation cutoff into a measurable radius.
If a metallicity-dependent CO conversion factor is applied, the low-mass gas fractions would shift; the steep threshold could move in mass rather than disappear, so the claim should be re-tested with $\alpha_{\rm CO}$ variations.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Punchline: this is a genuinely useful dataset – the largest CO(1-0) census of Hα emitters in a z>2 protocluster – and the environmental trends are worth having. But the central two-regime gas-fraction claim leans on an upper-limit method that overestimates fluxes, so the sharp transition at log M* ≈ 10.5 is not as secure as the paper suggests.

What's new: 43 spectroscopically confirmed HAEs with CO(1-0) measurements or upper limits, 10 detections, a stacking analysis in three bins, and environmental trends (µ_gas, SFE vs η) that haven't been published for this sample. The authors are transparent about many caveats, which is a real positive. The comparison with literature samples and the Tacconi et al. (2018) scaling relations is fair and useful. This is a solid observational contribution.

Soft spots: the upper limits for 33 of 43 sources are computed by integrating only positive flux channels within ±500 km/s and taking the maximum over a 3×3 spaxel grid. The authors themselves note this can overestimate flux, yet those limits are then plotted as fgas points and included — together with the 10 detections — in the logistic fit that defines the steep transition. The stacked low-mass Fgas = 0.86 uses the same positive-only integration, so it is not an independent check of the individual upper limits. A censored-data treatment (e.g., Bayesian upper limits) could shift both the transition mass and the inferred gas-richness of the low-mass population. The qualitative trend likely survives, but the quantitative sharpness is not proven. Minor: the logistic fit is done on the combined PKS1138 + CLJ1001 sample, with only 10 detections; the result depends on treating limits as measurements.

Who it's for: observers working on high-z protoclusters, cold gas, and quenching. It deserves a serious referee. The data are valuable and the analysis is mostly careful, but the upper-limit method needs revision before the central claim can be accepted. Recommendation: send to peer review with a request for a censored-data analysis or an explicit demonstration that the bias does not change the conclusion.

Referee Report

4 major / 5 minor

Summary. This paper presents ATCA CO(1-0) observations of 43 spectroscopically confirmed H-alpha emitters in the Spiderweb protocluster at z=2.16, of which 10 are detected in CO(1-0) and the rest are assigned upper limits. The central claim is that the molecular gas fraction, fgas = M_mol/(M_mol + M_star), shows two distinct regimes with a steep transition near log M_star/M_sun ~ 10.5: low-mass galaxies are gas-rich (fgas near unity) while massive galaxies, especially AGN candidates, have fgas below about 0.4. The authors interpret this as evidence for rapid cold-gas depletion via AGN feedback and overconsumption, with environmental gas removal playing a secondary role. They also present stacking results, depletion times, and environmental trends in phase space and local density.

Significance. If the two-regime fgas pattern is robust, this is one of the most complete molecular-gas censuses of a protocluster at cosmic noon, providing an important observational benchmark for galaxy formation models. The paper also gives a clear, falsifiable picture: low-mass protocluster galaxies are replenished by cosmic-web inflows, while massive galaxies quench through gas depletion aided by AGN. The comparison with coeval field and protocluster samples and the explicit discussion of accretion-regime changes are strengths. However, the central result rests on an upper-limit method that the authors themselves note can overestimate fluxes; because those upper limits are treated as measurements in the fgas analysis, the claimed steep transition is not yet demonstrated to the standard required for such a strong physical conclusion.

major comments (4)

[Sect. 3.1 and Fig. 6] The upper limits for the 33 non-detections are computed by integrating only positive flux channels within ±500 km/s and by taking the maximum over a 3x3 spaxel grid. This is a deliberately conservative upper limit, but it is also a positively biased estimator: noise fluctuations push the derived flux upward. The text acknowledges this ('can result in a flux overestimation'). These biased upper limits are then plotted as fgas points and included in the logistic fit of Eq. 5 that defines the steep transition. Because low-mass sources are mostly non-detections, this systematically raises their fgas and can create or exaggerate a gas-rich low-mass regime. The paper needs a quantitative robustness check: for example, fitting Eq. 5 using only the 10 detections, or treating upper limits with a censored-data/survival-analysis approach, and reporting how A, B, and the transition location change.
[Sect. 4.2, Table 2] The stacked low-mass Fgas = 0.86 ± 0.04 is presented as supporting the individual upper-limit trend. However, the stacking analysis uses the same positive-only, maximum-spaxel prescription of Sect. 3.1. A positive-only stack of mostly undetected sources will produce a positive flux even if the true signal is zero, so this stacking result is not an independent confirmation. The authors should either demonstrate that a symmetric integration (or one that subtracts a negative-noise control) yields the same result, or explicitly state that the stacked value inherits the same bias.
[Sect. 4.1 and Sect. 5.1] The interpretation that low-mass HAEs have gas fractions 'close to unity' and are 'replenished by inflows' is a direct consequence of the positive-biased upper limits in §3.1. The same applies to the conclusion that massive galaxies deplete their gas rapidly above log M* = 10.5. The paper should either recalibrate the upper-limit method through simulations or a control sample (e.g., using negative-flux maps to estimate the bias), or soften these physical conclusions to what is actually supported by the detections alone.
[Sect. 4.1, Eq. 5] The logistic fit is performed simultaneously on this sample and the CLJ1001 sample of Wang et al. (2018), and the text states that removing Wang et al. changes A and B by 1 sigma and 0.5 sigma, respectively. This means the steepness parameter B is not strongly constrained. The claim of a 'steep' transition should be quantified with a confidence interval on B and the location of the transition, and the fit should be repeated excluding the upper limits to show that the transition is not an artifact of the limit distribution.

minor comments (5)

[Conclusions, item 1] The text states 'we have obtained 26 CO(1-0) upper flux limits for the rest of our sample,' while Sect. 4 and Table A.1 list 33 upper limits (including the four cases with S/N>4 that are still treated as upper limits). This inconsistency should be corrected.
[Sect. 3.1] The description of the upper-limit extraction does not specify how the local noise rms is measured for each spaxel, which is needed to reproduce the quoted median S/N of about 2.3. A precise definition (e.g., the rms in line-free channels of that spaxel) should be added.
[Sect. 4.2] There is a typo in the text: 'Fgas = 0.86 ± 0.0.04' should read '0.86 ± 0.04'.
[Fig. 6 caption] The caption says the red solid line is the fit 'to the PKS1138 and CLJ1001 protocluster samples,' but it does not mention that Eq. 5 with A = 10.93 and B = -2.15 is used. Adding the parameters to the caption would make the figure self-explanatory.
[Sect. 4.1] There is a typo 'Sect.,3.1' in the first paragraph; it should be 'Sect. 3.1'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the fgas and depletion-time results are measured directly from CO(1-0) and Halpha data, and the logistic fit is a fit rather than a prediction.

full rationale

The paper is an observational study whose derived quantities, fgas = Mmol/(M* + Mmol) and tau_dep = Mmol/SFR, are direct ratios of measured CO(1-0) fluxes (or upper limits) and Halpha-based SFRs (Eqs. 1 and 2). The logistic transition (Eq. 5) is explicitly presented as a fit to the protocluster and comparison samples, with A and B as fitted parameters, not as a prediction generated from the model; the comparison against Tacconi et al. (2018) is an external benchmark. The stacking analysis in Sect. 4.2 uses the same CO(1-0) data and the same positive-channel integration method as the individual upper limits, so it does not independently confirm those limits, but this is a methodological limitation rather than circular reasoning. Prior work by the same team (e.g., Perez-Martinez et al. 2023) is used as data provenance for SFRs, metallicities, and AGN diagnostics, and no load-bearing argument reduces to an unverified self-citation or an imported uniqueness theorem. The positive-only flux integration and maximum-spaxel selection may bias upper limits upward, but that would be a measurement-systematic concern, not equivalence of the derivation to its inputs. Accordingly, no circular step is present.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central claim rests primarily on the conversion from CO luminosity to gas mass, the custom upper-limit method, and the adopted protocluster dynamical parameters. No new physical entities are introduced. The logistic fit parameters A and B are the only genuinely fitted quantities in the analysis.

free parameters (2)

logistic fit A = 10.93 +/- 0.05
Center of the fgas-M* transition fitted to the combined sample (this work + Wang et al. 2018) using Eq. 5.
logistic fit B = -2.15 +/- 0.33
Slope of the fgas-M* transition fitted simultaneously with A; controls the steepness of the claimed transition.

assumptions (5)

domain assumption A single conversion factor alpha_CO(1-0)=4.36 M_sun/(K km/s pc^2) applies to all sources in the sample.
Used to convert CO(1-0) luminosity to molecular gas mass (Eq. 1). The paper derives metallicity-dependent corrections up to fcorr=3.3 for low-mass sources but chooses a constant value for the main analysis.
domain assumption The H-alpha emission is predominantly powered by star formation, not AGN or shocks, for all galaxies in the sample.
Sect. 3.2: the paper computes SFR from H-alpha fluxes and states it cannot quantify AGN contamination in the narrow-line component.
domain assumption The protocluster core is virialized with R200=0.53 Mpc and sigma=683 km/s, and the Spiderweb galaxy marks the center.
Used to define the phase-space parameter eta (Sect. 3.4). These values come from Shimakawa et al. (2014) and are uncertain.
ad hoc to paper The custom upper-limit extraction (positive-flux integration, max over 3x3 spaxels) yields fluxes that can be treated as upper limits on the true CO(1-0) flux.
Sect. 3.1: this method is introduced in this paper and is acknowledged to overestimate fluxes; all fgas upper limits and the low-mass gas-rich interpretation depend on it.
domain assumption The H-alpha selected sample is representative of the star-forming protocluster population at z=2.16.
Selection via NB2071 filter and spectroscopic follow-up may miss heavily obscured star-forming galaxies; the paper discusses this but assumes representativeness for environmental comparisons.

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Cite this review

Pith. "Pith review of COALAS III: The ATCA CO(1-0) look at the growth and death of H$\alpha$ emitters in the Spiderweb protocluster at z=2.16." pith.science (2026). https://pith.science/paper/6JQLXCAX

@misc{pith2026241112138,
  author       = {Pith},
  title        = {Pith review of: COALAS III: The ATCA CO(1-0) look at the growth and death of H$\alpha$ emitters in the Spiderweb protocluster at z=2.16},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6JQLXCAX}},
  note         = {Machine review of arXiv:2411.12138}
}

abstract

We obtain CO(1-0) molecular gas measurements with ATCA on a sample of 43 spectroscopically confirmed H$\alpha$ emitters in the Spiderweb protocluster at $z=2.16$ and investigate the relation between their star formation and cold gas reservoirs as a function of environment. We achieve a CO(1-0) detection rate of $\sim23\pm12\%$ with 10 dual CO(1-0) and H$\alpha$ detections at $10<\log M_{*}/M_\odot<11.5$. In addition, we obtain upper limits for the remaining sources. In terms of total gas fractions ($F_{gas}$), our sample is divided into two different regimes with a steep transition at $\log M_{*}/M_\odot\approx10.5$. Galaxies below that threshold have gas fractions that in some cases are close to unity, indicating that their gas reservoir has been replenished by inflows from the cosmic web. However, objects at $\log M_{*}/M_\odot>10.5$ display significantly lower gas fractions and are dominated by AGN (12 out of 20). Stacking results yield $F_{gas}\approx0.55$ for massive emitters excluding AGN, and $F_{gas}\approx0.35$ when examining only AGN candidates. Furthermore, depletion times show that most H$\alpha$ emitters may become passive by $1<z<1.6$, concurrently with the surge and dominance of the red sequence in the most massive clusters. Our analyses suggest that galaxies in the outskirts of the protocluster have larger molecular-to-stellar mass ratios and lower star formation efficiencies than in the core. However, star formation across the protocluster remains consistent with the main sequence, indicating that evolution is primarily driven by the depletion of the gas reservoir towards the inner regions. We discuss the relative importance of in-/outflow processes in regulating star formation during the early phases of cluster assembly and conclude that a combination of feedback and overconsumption may be responsible for the rapid cold gas depletion these objects endure.

Figures

Figures reproduced from arXiv: 2411.12138 by the authors.

**Figure 1.** Spiderweb protocluster field at z ≈ 2.16. Blue circles display the full sample of candidate HAEs from Koyama et al. (2013) and Shimakawa et al. (2018b). Red circles show those HAEs with measured spectroscopic redshift (Shimakawa et al. 2018b and Pérez-Martínez et al. 2023). Orange crosses and contours respectively show the CO(1-0) emitters reported by Jin et al. (2021) and the limits of the COALAS ATCA footprint. Em… view at source ↗

**Figure 2.** Redshift distribution of sources. The complete sample [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗

**Figure 4.** Comparison of the L ′ CO(1−0) obtained by applying our methodology and the source detection codes outlined in Jin et al. (2021) for HAEs with CO(1-0) detection at S/N > 4. Article number, page 6 of 25 [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗

Figures from the paper (8 more)

**Figure 5.** Figure 5: Star forming main sequence diagram. The black solid [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]

**Figure 6.** Figure 6: Left: Total gas fraction versus stellar mass diagram. The solid green line and shaded region represent the field scaling relations [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]

**Figure 7.** Figure 7: Stacked spectra around the CO(1-0) emission line for the three bins defined in Sect. 4.2: Low-mass galaxies [PITH_FULL_IMAGE:figures/full_fig_p011_7.png]

**Figure 8.** Figure 8: Molecular gas mass versus star formation rate diagram. [PITH_FULL_IMAGE:figures/full_fig_p011_8.png]

**Figure 9.** Figure 9: Left: Phase space diagram. Objects are color-coded by their molecular to stellar mass ratio [PITH_FULL_IMAGE:figures/full_fig_p013_9.png]

**Figure 10.** Figure 10: Left: Star formation rate offsets from the Main Sequence of Tacconi et al. (2018) as a function of the environmental parameter η. Right: Star formation efficiency offsets with respect to the scaling relation of Tacconi et al. (2018) as a function of η. The symbols and…

**Figure 11.** Figure 11: Gas fraction as a function of local density defined by the area enclosing two, five, and 10 neighboring galaxies ( [PITH_FULL_IMAGE:figures/full_fig_p014_11.png]

**Figure 12.** Figure 12: Accretion regime diagram. Colored stars display the [PITH_FULL_IMAGE:figures/full_fig_p014_12.png]

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

In the Spiderweb protocluster, passive fraction rises with local density to ~60% while passive mass–size intercepts sit between field and cluster values, indicating advanced quenching but ongoing size growth.

Reference graph

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, " * write output.state after.block = add.period write newline

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sent...
[252]

write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 gl...

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.

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