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arxiv: 2605.21592 · v1 · pith:2EGURZCNnew · submitted 2026-05-20 · 🌌 astro-ph.GA · astro-ph.CO

Molecular gas properties of star-forming brightest group galaxies at z sim 0.3

Greta Toni , Gianluca Castignani , Fran\c{c}oise Combes , Philippe Salom\'e , Angel Bongiovanni , Lauro Moscardini , Matteo Maturi This is my paper

Pith reviewed 2026-05-22 09:11 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords brightest group galaxiesmolecular gasCO observationsstar formationgalaxy groupsgas depletionenvironmental effectsgalaxy evolution
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The pith

Brightest group galaxies at z~0.3 show molecular gas depletion timescales of 0.5-1.5 Gyr, suggesting group environments exhaust cold gas before full quenching.

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

The paper reports targeted CO(1-0) observations of three brightest group galaxies at redshift around 0.3 that display disturbed morphologies and active star formation. One system yields a detected molecular hydrogen mass near 3 times 10 to the 10 solar masses, while the other two remain undetected and produce upper limits below 10 to the 10 solar masses. When these gas constraints are divided by infrared-derived star formation rates, the resulting depletion timescales fall between roughly 0.5 and 1.5 billion years. The authors interpret the short timescales as evidence that environmental processes inside groups can limit gas supply or drive rapid exhaustion even while star formation continues. This positions the observed BGGs as possible transitional objects between gas-rich cluster centrals and passively evolving systems.

Core claim

Targeted CO(1→0) observations detect substantial molecular gas (M_H2 ~ 3 × 10^10 M_⊙) in one BGG while placing stringent upper limits (M_H2 ≲ 10^10 M_⊙) on the other two; combined with fiducial SFRs from total infrared luminosity, these measurements imply gas depletion timescales ≲ 0.5–1.5 Gyr, indicating that environmental regulation in groups can deplete cold gas reservoirs and precede star-formation quenching in central galaxies.

What carries the argument

CO(1→0) line emission observed with the IRAM 30 m telescope, used to derive molecular gas masses that are then ratioed against infrared-based star formation rates to obtain depletion timescales.

If this is right

  • Some actively star-forming BGGs already sit in a rapid gas-exhaustion phase driven by group-scale processes.
  • Gas depletion can occur before star formation is fully quenched, creating a bridge between gas-rich and passive central galaxies.
  • Interaction signatures and extended blue substructures may trace the same environmental mechanisms that suppress gas replenishment.
  • Group environments may regulate cold gas availability more efficiently than previously assumed for central galaxies at intermediate redshift.

Where Pith is reading between the lines

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

  • If confirmed in larger samples, these short depletion times would imply that group preprocessing accelerates the transition of centrals toward the red sequence at z<0.5.
  • Direct comparison with hydrodynamic simulations of group mergers could test whether the observed interaction signatures quantitatively match the inferred gas exhaustion rates.
  • Extending the same CO strategy to BGGs at both lower and higher redshifts would map whether the 0.5–1.5 Gyr depletion window is a characteristic feature of the group environment across cosmic time.

Load-bearing premise

Non-detections give tight upper limits on molecular gas mass and infrared emission accurately traces current star formation without significant AGN or dust-heating contamination.

What would settle it

A survey of additional BGGs at z~0.3 that finds molecular gas masses well above 10^10 M_⊙ or depletion timescales exceeding several Gyr in systems with similar morphologies and SFRs.

Figures

Figures reproduced from arXiv: 2605.21592 by Angel Bongiovanni, Fran\c{c}oise Combes, Gianluca Castignani, Greta Toni, Lauro Moscardini, Matteo Maturi, Philippe Salom\'e.

Figure 1
Figure 1. Figure 1: From left to right: Target BGG 0957+0204, BGG 1000+0207 and BGG 0958+0223. Top panels: Colour composite 30′′×30′′ images of the three targets in HSC g, r, i bands; bottom panels: 30′′×30′′ UltraVISTA Ks image (for BGG 0957+0204) and HST￾ACS I mosaic (for BGG 1000+0207 and BGG 0958+0223). For reference, at the bottom of each panel we report the physical size corresponding to 5′′. Our targets are unresolved … view at source ↗
Figure 2
Figure 2. Figure 2: Location of our three targets (white crosses: 1. BGG [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: SEDs and respective LePhare best fitting modelling for [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Baseline-subtracted CO(1→0) spectrum of BGG 1000+0207. The solid line shows the Gaussian best fit. The flux (y-axis) in units of mJy is plotted against the relative velocity with respect to the BGG redshift. The IRAM 30m half-power beam width (HPBW) is ∼ 16 arcsec λobs 2 mm (Kramer et al. 2013), where λobs is the observer frame wavelength. This translates into a beam diameter for our three targets falling … view at source ↗
Figure 5
Figure 5. Figure 5: Molecular gas properties of BCGs (diamonds) and cluster galaxies (grey points) detected in CO from the literature, compared [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
read the original abstract

Recent efforts to characterise the molecular gas content of brightest cluster galaxies (BCGs) at intermediate redshift have revealed a sub-population of gas-rich systems, whose star formation activity is likely influenced by environmental processing. In this study, we aim to investigate the molecular gas reservoirs and star formation fuelling of central galaxies in groups, also known as brightest group galaxies (BGGs), at intermediate redshifts. We present targeted carbon monoxide (CO) line observations of three BGGs in the COSMOS field at $z \sim 0.3$, obtained with the IRAM 30m telescope. The galaxies exhibit disturbed morphologies, extended blue substructures, and interaction signatures. Furthermore, they exhibit significant star formation rates derived from multiwavelength diagnostics. We detect CO(1$\rightarrow$0) emission in one system, revealing a substantial molecular gas mass of $M_{H_2} \sim 3 \times 10^{10}$ M$_\odot$, while for the other two BGGs, CO emission lines remain undetected, yielding stringent upper limits of $M_{H_2} \lesssim 10^{10}$ M$_\odot$. By combining molecular gas constraints with fiducial star formation rates derived from total infrared emission, we infer gas depletion timescales in the range of $\lesssim 0.5-1.5$ Gyr. These results may indicate that, despite their active star formation and interaction signatures, some BGGs could already experience efficient gas exhaustion or suppressed gas replenishment, suggesting that gas depletion precedes star formation quenching. Our findings hint that environmental processes in galaxy groups could strongly regulate the availability of cold gas and drive rapid evolutionary phases in central galaxies, possibly bridging the gap between gas-rich BCGs and passively evolving systems.

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 manuscript reports targeted CO(1→0) observations with the IRAM 30m telescope of three star-forming brightest group galaxies (BGGs) at z ∼ 0.3 in the COSMOS field. These galaxies exhibit disturbed morphologies and interaction signatures. One system shows a CO detection corresponding to M_H2 ∼ 3 × 10^10 M_⊙, while the other two yield upper limits of M_H2 ≲ 10^10 M_⊙. Combining these molecular gas constraints with star formation rates derived from total infrared emission produces gas depletion timescales of ≲ 0.5–1.5 Gyr. The authors interpret the short timescales as evidence that environmental processes in galaxy groups may regulate cold gas availability, drive rapid evolutionary phases in central galaxies, and bridge the gap between gas-rich BCGs and passively evolving systems.

Significance. If the results hold after addressing the assumptions below, the work supplies new direct constraints on molecular gas reservoirs in BGGs at intermediate redshift, a population less studied than BCGs. The mix of one detection and two upper limits, together with the inferred short depletion times, offers a suggestive observational link between active and quenched central galaxies. The small sample size, however, prevents any statistical control against field BGGs or larger BCG samples at comparable redshift, so the environmental-regulation interpretation remains tentative rather than conclusive.

major comments (2)
  1. [Abstract] Abstract: The upper limits M_H2 ≲ 10^10 M_⊙ for the two non-detections are presented as stringent, yet the manuscript provides no explicit values for the assumed CO line width, velocity resolution, or baseline uncertainties entering the limit calculation. If the disturbed morphologies imply broader lines than assumed, the limits weaken and the short depletion timescales (≲ 0.5–1.5 Gyr) that anchor the evolutionary claim become less secure.
  2. [Abstract] Abstract and Results: Depletion timescales are derived from fiducial SFRs based on total infrared luminosity, but the text contains no quantitative test for AGN or dust-heating contributions to the 8–1000 µm emission. Because the central interpretation—that gas exhaustion precedes quenching—rests directly on these short timescales, an explicit assessment of possible SFR overestimation is required.
minor comments (2)
  1. [Abstract] Abstract: The choice and justification of the CO-to-H2 conversion factor should be stated explicitly, as it is a free parameter that scales all reported gas masses and depletion times.
  2. [Abstract] Abstract: The phrase 'stringent upper limits' would be clearer if accompanied by the 3σ noise level or assumed line width used to obtain M_H2 ≲ 10^10 M_⊙.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and valuable comments, which have helped improve the clarity and robustness of our manuscript. We have revised the paper to address the two major comments regarding the calculation of upper limits and the potential contributions to the infrared luminosity. Our point-by-point responses are as follows.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The upper limits M_H2 ≲ 10^10 M_⊙ for the two non-detections are presented as stringent, yet the manuscript provides no explicit values for the assumed CO line width, velocity resolution, or baseline uncertainties entering the limit calculation. If the disturbed morphologies imply broader lines than assumed, the limits weaken and the short depletion timescales (≲ 0.5–1.5 Gyr) that anchor the evolutionary claim become less secure.

    Authors: We acknowledge that explicit values for the assumed CO line width, velocity resolution, and baseline uncertainties were not provided in the abstract or main text. We will revise the manuscript to include these details in both the abstract and the observations section. Specifically, we will state the assumed line width used for the non-detections and discuss the implications of potentially broader lines due to the interaction signatures. This will allow readers to better evaluate the stringency of the upper limits and the robustness of the inferred depletion timescales. revision: yes

  2. Referee: [Abstract] Abstract and Results: Depletion timescales are derived from fiducial SFRs based on total infrared luminosity, but the text contains no quantitative test for AGN or dust-heating contributions to the 8–1000 µm emission. Because the central interpretation—that gas exhaustion precedes quenching—rests directly on these short timescales, an explicit assessment of possible SFR overestimation is required.

    Authors: We concur that the manuscript would benefit from an explicit assessment of possible AGN or dust-heating contributions to the total infrared emission used to derive the star formation rates. In the revised version, we will add a quantitative discussion based on the multi-wavelength data available for these COSMOS sources. This includes checking for X-ray detections or radio excesses that could indicate AGN activity, as well as comparing the IR SFRs to independent estimates from UV and SED modeling. While we do not expect significant overestimation given the star-forming nature of these BGGs, we will explicitly address this to strengthen the interpretation of the short depletion timescales. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results from new observations

full rationale

The paper reports targeted IRAM 30m CO(1-0) observations of three BGGs at z~0.3, with a direct detection yielding M_H2 ~ 3e10 Msun in one object and upper limits M_H2 ≲ 1e10 Msun in the other two. These gas masses are obtained from the observed line intensities via standard conversion factors. Fiducial SFRs are taken from total infrared luminosities using established multiwavelength diagnostics. Depletion times are then formed as the direct ratio M_H2/SFR, producing the reported range ≲0.5-1.5 Gyr. No equation reduces a reported quantity to a prior fitted parameter by construction, no self-citation supplies a load-bearing uniqueness theorem or ansatz, and the central inference about environmental regulation of cold gas follows from the new data rather than from any internal redefinition or renaming of known results. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard assumptions for converting CO luminosity to molecular gas mass and for deriving star formation rates from infrared luminosity; no new entities are postulated.

free parameters (1)
  • CO-to-H2 conversion factor
    Standard value assumed to convert observed CO(1-0) luminosity to H2 mass; choice directly affects the reported gas masses and depletion times.
axioms (2)
  • domain assumption The three selected BGGs are representative of star-forming central galaxies in groups at z~0.3
    Sample chosen based on multiwavelength star formation diagnostics and disturbed morphologies.
  • domain assumption Infrared emission provides a reliable tracer of current star formation rate without major contamination
    Used to compute depletion timescales from gas masses.

pith-pipeline@v0.9.0 · 5889 in / 1464 out tokens · 35523 ms · 2026-05-22T09:11:17.326361+00:00 · methodology

discussion (0)

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Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    We detect CO(1→0) emission in one system, revealing a substantial molecular gas mass of M_H2 ∼ 3×10^10 M_⊙, while for the other two BGGs, CO emission lines remain undetected, yielding stringent upper limits of M_H2 ≲ 10^10 M_⊙. By combining molecular gas constraints with fiducial star formation rates derived from total infrared emission, we infer gas depletion timescales in the range of ≲0.5−1.5 Gyr.

  • IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    Our findings hint that environmental processes in galaxy groups could strongly regulate the availability of cold gas and drive rapid evolutionary phases in central galaxies

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

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