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SYMPHANY- SYnergy of Molecular PHase And Neutral hYdrogen in galaxies in A2626

T0 review · 4 major / 8 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read In the A2626 cluster, the molecular gas is depleted even though the atomic gas survives, suggesting the cluster's calm core shapes how gas is removed.

desk verdict First CO map of A2626 is a useful data release, but the claimed H2-vs-HI deficiency contrast rests on a biased, error-bar-free sample. read the letter →

arxiv 2505.15060 v1 pith:P5V3WI2S submitted 2025-05-21 astro-ph.GA

Tirna Deb , Garrett K. Keating , Nikki Zabel , Alessia Moretti , Cecilia Bacchini , Timothy A Davis , Bianca M. Poggianti , Marco Gullieuszik
show 4 more authors
Benedetta Vulcani Yara Jeffé Neven Tomicic Toby Brown
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyclustersmoleculargasatomichydrogenrampressurestrippingCO(2-1)observationsstarformationefficiencycool-coreclusterA2626
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 uses matched CO(2-1) and HI observations of ten galaxies in the A2626 cluster to test which cold-gas phase is removed first in a dense environment. It argues that in A2626, a relaxed cool-core cluster, the atomic gas is more extended and shows stripping signatures, yet the galaxies are only mildly HI-deficient; instead they are comparatively more H2-deficient, with higher gas fractions and shorter depletion timescales (0.3-3 Gyr) than Virgo galaxies. The implied picture is that cluster dynamical state matters: A2626's calm intracluster medium weakens ram-pressure stripping of atomic gas, while local interactions or early infall still erode the molecular phase. If correct, the paper shows that molecular gas depletion is not reserved for violent clusters and that the standard 'HI is stripped first' sequence is environment-dependent.

What carries the argument

The argument is carried by a joint morphological and kinematic comparison of the two gas phases, using CO(2-1) cubes from ALMA and SMA and HI cubes from MeerKAT, overlaid on optical images. Gas content is quantified with the deficiency definition $\mathrm{def}_i = \log M_{i,\mathrm{exp}} - \log M_{i,\mathrm{obs}}$ from Zabel et al. (2022), where expected masses come from stellar-mass-matched field samples, and the paper compares these deficiencies, total gas fractions, and depletion times ($M_{\mathrm{HI}}+M_{\mathrm{H2}}$ over SFR) against Virgo and GASP samples while placing the galaxies on a projected phase-space diagram ($R/R_{200}$ versus $\Delta v/\sigma_{\mathrm{cl}}$). The mechanism that carries the interpretation is the contrast between A2626's relaxed cool-core intracluster medium and Virgo's unrelaxed non-cool-core state.

What would settle it

Deep CO(2-1) observations of the ALMA and SMA targets that were not detected would settle the point: if most of those galaxies turn out to have very low H2 masses, the apparent 'HI-normal but H2-poor' pattern may be an artifact of excluding faint CO emitters. A second test would compare A2626 with a matched-mass non-cool-core cluster using the same deficiency definition; if H2 deficiencies turn out similar, the cool-core explanation rather than sample selection would need revision.

Watch

Extended reading notes

Core claim

On the paper's own terms, the central discovery is that environment can deplete molecular gas while leaving atomic gas relatively intact. In the ten detected A2626 galaxies, HI is morphologically extended and often asymmetric or truncated, while CO is centrally concentrated; nevertheless, the sample shows low HI deficiencies but elevated H2 deficiencies relative to expected masses from field scaling relations, and several galaxies have lopsided CO distributions or disturbed velocity fields. The authors interpret this as the signature of a cool-core cluster: weaker ram-pressure stripping allows galaxies to keep their HI, while earlier infall or local galaxy-galaxy interactions act on the molecular reservoir. A2626 galaxies also sit at higher gas fractions and shorter depletion timescales than Virgo galaxies, implying moderately enhanced star formation efficiency, and the paper finds no correlation between H2 deficiency and cluster-centric radius or velocity, which it reads as evidence that current cluster location is not the main driver of molecular gas loss.

Load-bearing premise

The comparison of HI and H2 deficiencies assumes that the ten galaxies detected in CO are representative of A2626's galaxy population; the eight observed but non-detected galaxies are left out of the deficiency, gas-fraction, and star-formation-efficiency analyses, and if those galaxies are preferentially H2-poor the claimed pattern would be biased.

Editorial extensions

If this is right

  • A2626 galaxies show low HI deficiencies but elevated H2 deficiencies, opposite to the usual expectation that atomic gas is depleted first.
  • Several galaxies have asymmetric or truncated CO discs and disturbed velocity fields, so molecular gas is not fully shielded in dense environments.
  • Depletion times of 0.3-3 Gyr imply moderately enhanced star formation efficiency relative to Virgo galaxies.
  • The absence of a correlation between H2 deficiency and cluster-centric radius or velocity favors early infall or local interactions over current cluster position as the driver.
  • Cluster dynamical state (relaxed cool-core versus unrelaxed non-cool-core) is a plausible control on how environmental gas removal proceeds.

Reading between the lines

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

  • If this pattern holds, cluster dynamical state should become a standard axis in environmental-quenching models, not just cluster mass and radius.
  • A direct extension would be to measure the same HI and H2 deficiency pair in a sample of cool-core versus non-cool-core clusters matched in mass and redshift; the paper's logic predicts a systematic offset in the HI-versus-H2 deficiency plane.
  • The short depletion times suggest that pre-processing or tidal compression may convert or consume molecular gas before ram-pressure stripping removes atomic gas; this could be tested by checking whether the H2-deficient galaxies have enhanced central stellar surface densities or compact bulges.
  • Upper limits on CO for the non-detected galaxies would let the deficiency statistics be recomputed with a survival analysis, testing whether the reported pattern survives selection effects.
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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

4 major / 8 minor

Summary. The paper presents ALMA and SMA CO(2-1) observations of 10 galaxies in the A2626 cluster, combined with MeerKAT H I data, to study environmental effects on atomic and molecular gas. The authors compare H I and CO morphology and kinematics, compute H I and H2 deficiencies relative to xGASS/xCOLDGASS scaling relations, and compare gas fractions and depletion times with Virgo and GASP samples. They conclude that H I is more extended and more easily stripped, but CO also shows asymmetries and H2 deficiencies; A2626 galaxies have lower H I deficiencies but higher H2 deficiencies than Virgo, higher gas fractions, and shorter depletion times (0.3-3 Gyr), implying enhanced star formation efficiency, with no correlation between H2 deficiency and cluster-centric distance or velocity.

Significance. If the quantitative conclusions survive scrutiny, the paper would provide a notable counterpoint to the usual picture that H I is affected before H2: in the relaxed cool-core cluster A2626, the molecular phase may be relatively more depleted than the atomic phase. The dataset is valuable—spatially resolved CO and H I for 10 galaxies, with a careful ALMA/SMA consistency check confirming that ALMA does not resolve out significant flux. The morphological/kinematic evidence (Figures 6 and 7) is credible and supports the qualitative claim that H I is more extended and that some CO discs are asymmetric. However, the current analysis does not establish the quantitative claims because the CO-detected sample is a biased subset, and the deficiency and depletion-time comparisons lack error bars and significance tests.

major comments (4)
  1. [Section 3.4, Table 5, Fig. 8] The quantitative comparison of H2 deficiency with Virgo rests on the 10 CO-detected galaxies, while 8 of 17 ALMA targets and 2 of 6 SMA targets were not detected and are silently excluded from the deficiency, gas-fraction, and depletion-time analyses. If the non-detections are preferentially H2-poor, the median H2 deficiency of A2626 would shift toward the Virgo values and could erase the claimed contrast. The text notes 'sensitivity limitations' as a possible cause, but no CO(2-1) upper limits are given. Please add flux or mass upper limits for the non-detections (using the RMS and an assumed line width) and recompute the deficiency distributions including these limits, or explicitly justify their exclusion.
  2. [Eq. (2), Table 5, Fig. 8] The central quantitative result—that H2 deficiency exceeds H I deficiency in A2626—is presented without uncertainties on the deficiency values. From Table 5, the H2 mass errors range from ~0.05 to ~1.0 dex, and the xCOLDGASS expected-mass relation has intrinsic scatter of ~0.2–0.5 dex, comparable to or larger than the median offset between H2 and H I deficiency (~0.14 dex). Without propagating these errors and performing a significance test (e.g., bootstrap or a paired test), the headline offset is not established. Please report deficiency uncertainties and a statistical assessment of the offset.
  3. [Section 3.1, Figs. 2–4] Section 3.1 refers to 'Figure 2' as presenting the CO(2-1) moment 0 and moment 1 maps and global spectra for the ALMA-detected galaxies, but Figures 2–4 in the manuscript are captioned as H I moment maps and profiles. The CO maps are not displayed anywhere, so the reader cannot verify the individual morphological and kinematic descriptions (e.g., 'elongated and asymmetric' for H I ID 15, 'clumpy and extended' for H I ID 107). Please either include the CO maps as a figure or renumber the reference so the evidence is available.
  4. [Section 3.6, Fig. 11] The claim that A2626 galaxies have shorter depletion times (median ~1.2 Gyr) than VERTICO galaxies (~3–5 Gyr) is made without uncertainties on the depletion times or SFRs, and it inherits the selection bias of the CO-detected sample. The WISE 12-um SFRs have quoted errors of ~0.3–1.5 M_sun/yr (Table 3), which propagate into the depletion time. Please provide error bars or a sensitivity test, and state how the CO non-detections would affect the median.
minor comments (8)
  1. [Abstract] The phrase 'moderately enhanced star formation efficiency A2626 galaxies' is missing a preposition ('in').
  2. [Section 3.1, H I ID 170] The caveat that the SMA detection may have captured only part of the CO reservoir should be reflected in the H2 mass uncertainty for H I ID 170 in Table 5, which is reported with an uncertainty of 0.352 dex.
  3. [Table 3, column (11)] The H I class column uses Arabic numbers (0, 1, 2) while the text refers to classes I–V; please clarify the mapping so the absence of class III and IV is unambiguous.
  4. [Eq. (1)] The equation normalizes r21 by 0.7, but the text adopts r21 = 0.79; please state explicitly that the scaling uses the adopted value relative to 0.7, or update the normalization to 0.79 to avoid confusion.
  5. [Figure 7] The caption states that 'all but one' CO profiles are from ALMA, but the text excludes H I ID 8 from Figure 7; please clarify the exact number of profiles shown and which galaxies are included.
  6. [Section 2] The sample selection is described as requiring the expected CO disc to span at least three beams; this criterion favors galaxies with larger optical radii and should be listed among the selection effects affecting the deficiency comparison.
  7. [References] Healy et al. (2021a,b) are cited as arXiv e-prints; please provide the published versions if available.
  8. [Acknowledgments] 'My acknowledgments:' appears to be a leftover template phrase; please remove.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: molecular gas masses, deficiencies, and gas fractions are derived from literature conversion factors and external field scaling relations, with no fitted parameter recycled as a prediction.

full rationale

The paper's quantitative derivation chain is self-contained in the relevant sense. H2 masses are computed from CO(2-1) fluxes via Eq. (1) with fixed literature values alpha10 = 4.3 (Bolatto et al. 2013) and r21 = 0.79 (Moretti et al. 2018, 2020a,b), neither fitted to A2626 data. Deficiencies use the Zabel et al. (2022) definition, Eq. (2), with expected masses from external xGASS/xCOLDGASS samples; observed masses are independent ALMA/SMA/MeerKAT measurements. The comparison samples (VERTICO, GASP, xCOLDGASS) are external benchmarks, not outputs of this paper. Prior A2626 HI data from Deb et al. (2023) and Healy et al. (2021a) are used as input catalogs, which is normal data provenance rather than circular derivation. The only notable limitation is that CO non-detections are excluded from deficiency and gas-fraction analyses without published upper limits (Sec. 3.4), which is a possible selection-bias and robustness concern, not a circularity: the detections are not defined in terms of the deficiencies they are used to compute, and the expected-mass relations come from outside the paper. No fitted parameter is renamed as a prediction, no uniqueness theorem is imported from the authors, and no ansatz is smuggled in via citation. Therefore the circularity score is 0.

Assumptions & free parameters 2 free parameters · 3 assumptions · 0 invented entities

The central results depend on standard literature calibrations for CO-to-H2 conversion and CO(2-1)/CO(1-0) ratio, plus external field scaling relations for expected gas masses and private WISE-based masses and SFRs. No new entities are invented, and no parameters are fitted to the A2626 data in this paper beyond the adopted calibrations.

free parameters (2)
  • CO-to-H2 conversion factor alpha10 = 4.3 M_sun pc^-2 (K km/s)^-1
    Adopted from Bolatto et al. (2013) to convert CO(2-1) flux to H2 mass (Equation 1). Central to all molecular gas masses and deficiencies; if the true value in cluster environments differs, absolute masses shift linearly.
  • CO(2-1)/CO(1-0) line ratio r21 = 0.79
    Adopted from Moretti et al. (2018, 2020b) for consistency with previous studies. Converts observed CO(2-1) to CO(1-0) equivalent flux; directly scales H2 masses.
assumptions (3)
  • domain assumption The CO-to-H2 conversion factor alpha10 = 4.3 and line ratio r21 = 0.79 are applicable to these galaxies.
    Adopted from Bolatto et al. (2013) and Moretti et al. (2018, 2020b) to convert CO(2-1) flux to molecular gas mass (Equation 1). If the conversion factor differs in cluster environments, absolute H2 masses and deficiencies shift.
  • domain assumption The expected HI and H2 masses for deficiency calculations are well described by xGASS/xCOLDGASS scaling relations.
    Deficiencies are computed as log(expected) minus log(observed) using stellar-mass-binned medians from xGASS/xCOLDGASS (Section 3.4). These field scaling relations are used as the zero-deficiency baseline.
  • domain assumption WISE-based stellar masses and SFRs (private communication, Jarrett) are reliable and consistently calibrated.
    Stellar mass and SFR are used to normalize deficiencies and to compute depletion times; their calibration is not described in this paper.

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Cite this review

Pith. "Pith review of SYMPHANY- SYnergy of Molecular PHase And Neutral hYdrogen in galaxies in A2626." pith.science (2026). https://pith.science/paper/P5V3WI2S

@misc{pith2026250515060,
  author       = {Pith},
  title        = {Pith review of: SYMPHANY- SYnergy of Molecular PHase And Neutral hYdrogen in galaxies in A2626},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/P5V3WI2S}},
  note         = {Machine review of arXiv:2505.15060}
}
read the original abstract

We present an analysis of the molecular and atomic gas properties of 10 spatially resolved galaxies in the A2626 cluster (z = 0.055), observed as part of the SYMPHANY project. Using CO(2-1) observations from ALMA and SMA, together with HI data from MeerKAT, we examine the interplay between gas phases and environmental influences. A joint morphological and kinematic analysis reveals that while the kinematic behavior of HI and CO are often similar, morphologically the atomic gas is more extended compared to centrally concentrated CO distributions, making it more susceptible to environmental stripping. However, we also find evidence for molecular gas asymmetries, disturbed velocity fields, and H2 deficiencies in some galaxies, indicating that H2 reservoirs can also be disrupted in dense environments. Compared to Virgo-a dynamically unrelaxed, non-cool-core cluster-A2626's relaxed, cool-core structure likely results in less intense ram-pressure stripping. This may allow galaxies to retain more atomic gas, while local interactions or pre-processing may still affect the molecular phase, causing relatively low HI deficiencies but high H2 deficiencies in A2626 galaxies. This is also reflected in the higher gas fractions, slightly elevated SFRs, along with shorter depletion timescales (0.3-3 Gyr), implying moderately enhanced star formation efficiency A2626 galaxies. Moreover, the lack of correlation between H2 deficiency and cluster-centric distance or velocity suggests that molecular gas evolution in A2626 may be shaped more by early infall or local interactions than by current cluster location.

Figures

Figures reproduced from arXiv: 2505.15060 by the authors.

Figure 1
Figure 1. Sky distribution of galaxies in A2626. Star and diamond markers denote non-substructure and substructure galaxies respec￾tively, targeted by ALMA and/or SMA within A2626. Small grey points represent other cluster galaxies with optical redshifts, while the dotted circle indicates the cluster’s R200 radius. Observations of atomic hydrogen (H I) in galaxies reveal that H I reservoirs are significantly affected by clust… view at source ↗
Figure 2
Figure 2. Overview of H I kinematic and global profile properties (1/3). Each panel shows the moment zero map, velocity field, and global H I profile for a different galaxy [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Overview of H I kinematic and global profile properties (2/3) [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Overview of H I kinematic and global profile properties (3/3) [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]
Figure 5
Figure 5. Figure 5: Comparison of ALMA and SMA global profiles for galaxies in A2626. Both profiles have been matched to the same spatial and spectral resolution by smoothing the ALMA cube to the SMA resolution. After this adjustment, the profiles appear similar, demonstrating consistency…
Figure 6
Figure 6. Figure 6: SYMPHANY galaxies in the A2626 galaxy cluster, with CO (red) and H I (white) contours overlaid on DECaLS RGB color images. CO and H I observations are from ALMA and MeerKAT observations respectively (except H I ID 170 is observed by SMA). A 15′′ scale bar in the bottom…
Figure 7
Figure 7. Figure 7: Global CO (black) and H I (blue) profiles for A2626 galaxies. All but one (SMA observations of H I ID 170) CO profiles are based on ALMA observations. The x-axis represents the velocity in km/s, while the y-axis normalized flux density for galaxies. the H I and CO comp…
Figure 8
Figure 8. Figure 8: Correlation between H I and H2 deficiencies of SYMPHANY galaxies compared to Virgo (Zabel et al. 2022) and three other cluster samples (Moretti et al. 2023). The ALMA-observed galaxies are color-coded based on classifications derived from optical and H I morphologies (…
Figure 9
Figure 9. Figure 9: The distribution of SYMPHANY galaxies in the pro￾jected phase-space of A2626. The x-axis shows the projected clus￾tercentric distance normalized by R200, and the y-axis shows the line-of-sight velocity relative to the cluster mean, normalized by the cluster velocity di…
Figure 10
Figure 10. Figure 10: Total gas (H I +H2) fraction as a function of stellar mass for A2626 galaxies (large blue markers), Virgo galaxies (turquoise markers), and GASP galaxies (pink markers). In A2626, star mark￾ers represent non-substructure galaxies, while diamond markers de￾note substru…
Figure 11
Figure 11. Figure 11: Relation between total gas mass (MHI+ MH2) and SFR for galaxies in A2626 and Virgo clusters. Blue stars represent A2626 galaxies, while orange circles represent Virgo (VERTICO) galaxies. Dotted diagonal lines denote constant gas depletion times, defined as total gas m…

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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

  1. HI Depletion Begins Well Beyond the Virial Radius: A FAST Stacking Study of 36 Galaxy Clusters to 5R200

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    Stacked FAST spectra show cluster galaxies have less neutral hydrogen than field galaxies out to 5R200, including blue star-forming members.

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