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arxiv: 2606.13393 · v1 · pith:CCFP5LMSnew · submitted 2026-06-11 · 🌌 astro-ph.GA · astro-ph.CO

Direct detection of cool molecular gas in a star-forming galaxy at z=7.31

Karin Cescon , Jacqueline A. Hodge , Leindert A. Boogaard , Hiddo S. B. Algera , Lucie E. Rowland , Dominik A. Riechers , Renske Smit , Ilse De Looze
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Rychard Bouwens Paul van der Werf Manuel Aravena Elisabete da Cunha Pratika Dayal Andrea Ferrara Rebecca Fisher Hanae Inami Pavel E. Mancera Pi\~na Pascal A. Oesch Andrea Pallottini Matus Rybak Sander Schouws Laura Sommovigo Mauro Stefanon Livia Vallini
This is my paper

Pith reviewed 2026-06-27 06:27 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords high-redshift galaxiesmolecular gasCO emissionEpoch of Reionizationstar-forming galaxiesinterstellar medium
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The pith

A massive molecular gas reservoir exists in a galaxy only 700 million years after the Big Bang.

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

The paper reports the detection of CO(3-2) emission from the galaxy REBELS-25 at redshift 7.31, marking the highest-redshift low-J CO transition observed. From the CMB-corrected flux, it derives a molecular gas mass of about 10^11 solar masses, implying a gas fraction near 0.95. The work uses the TUNER radiative transfer code to model the emission self-consistently and recover a consistent mass without relying on standard conversion factors. This directly shows that substantial cool molecular gas was already assembled early in cosmic history. The results also suggest [C II] can serve as a molecular gas tracer at these epochs.

Core claim

Deep VLA and ALMA observations detect CO(3-2) and CO(7-6) in REBELS-25 at z=7.31. The CMB-corrected CO(3-2) flux yields M_mol = (1.0 ± 0.4) × 10^11 (α_CO/3) M_⊙. TUNER modeling gives an independent mass of (1.8^{+1.0}_{-0.9}) × 10^11 M_⊙. This confirms a very massive gas reservoir only ≃700 Myr after the Big Bang, with f_gas ≃ 0.95, δ_GDR ≃ 6 × 10^2, and au_dep ≃ 1.2 Gyr, plus an empirical α_[C II] = (60 ± 25) M_⊙/L_⊙.

What carries the argument

CMB-corrected CO(3-2) flux combined with the TUNER radiative transfer model that self-consistently accounts for excitation, optical depth, and CMB effects to recover molecular gas mass independent of r_31 and α_CO.

If this is right

  • Low-J CO lines remain detectable at z>7, enabling direct molecular gas measurements in the Epoch of Reionization.
  • Galaxies can maintain gas fractions near unity at early times while following extrapolated main-sequence scaling relations.
  • [C II] emission provides a viable alternative tracer for molecular gas mass with a conversion factor around 60 solar masses per solar luminosity.
  • The gas-to-dust ratio reaches values of several hundred at these redshifts.

Where Pith is reading between the lines

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

  • Future facilities could routinely map molecular gas distributions in the first galaxies rather than relying solely on dust or [C II].
  • The short depletion timescale relative to the age of the universe at z=7.31 implies rapid gas replenishment or inefficient star formation.
  • If similar reservoirs exist in other REBELS galaxies, the total molecular gas budget at z>7 would be substantially higher than previously estimated from dust alone.

Load-bearing premise

The radiative transfer model calibrated on lower-redshift galaxies correctly describes the excitation and optical depth conditions in this z=7.31 system.

What would settle it

A deeper observation that yields a significantly lower CO(3-2) flux after CMB correction, or a direct dynamical mass measurement showing the gas mass is much smaller than derived.

Figures

Figures reproduced from arXiv: 2606.13393 by Andrea Ferrara, Andrea Pallottini, Dominik A. Riechers, Elisabete da Cunha, Hanae Inami, Hiddo S. B. Algera, Ilse De Looze, Jacqueline A. Hodge, Karin Cescon, Laura Sommovigo, Leindert A. Boogaard, Livia Vallini, Lucie E. Rowland, Manuel Aravena, Matus Rybak, Mauro Stefanon, Pascal A. Oesch, Paul van der Werf, Pavel E. Mancera Pi\~na, Pratika Dayal, Rebecca Fisher, Renske Smit, Rychard Bouwens, Sander Schouws.

Figure 1
Figure 1. Figure 1: Spectra of REBELS-25 showing the detected line emission of CO(3–2) (top panel) and CO(7–6) together with the undetected [C i](2–1) emission (bottom panel). In each panel, we show the data presented in this paper as an aqua histogram and the respective ±1𝜎 as a grey shaded area. We also display a comparison with the [Cii] spectrum which is detected at high S/N in this source (yellow hatched histogram), resc… view at source ↗
Figure 2
Figure 2. Figure 2: Black contours ([−3, −2, 2, 3]𝜎) show the velocity-integrated emission of CO(3–2) (left panel) and of CO(7–6) (right panel) overlaid on the [C ii] moment 0 map obtained from the REBELS large program data. We also show the contours for the [C ii] emission (white, [−3, −2, 2, 3, 5, 12]𝜎) and ALMA band 6 continuum tracing the dust emission (orange, [−3, −2, 2, 3, 5]𝜎). Synthesized beams for each dataset are s… view at source ↗
Figure 3
Figure 3. Figure 3: Molecular gas depletion timescale as a function of redshift for galax￾ies across cosmic time (adapted from Zavala et al. 2022). The large symbols mark the values derived for REBELS-25, assuming the CMB-corrected CO luminosity and 𝛼CO = 3 and 1 (magenta and aqua star, respectively); for clarity, the aqua star has been slightly offset in redshift to avoid overlapping error bars. Both values are broadly consi… view at source ↗
Figure 4
Figure 4. Figure 4: Dust spectral energy distribution (SED; left panel) and CO spectral line energy distribution (SLED; right panel) of REBELS-25 derived by fitting the observed continuum and line fluxes (black points for detections, arrows for 1𝜎 upper limits) self-consistently with the TUNER model. The black dashed lines represent the best-fit median model to the data given the priors, while the gray shaded regions show the… view at source ↗
Figure 5
Figure 5. Figure 5: Evolution of the [C ii]-to-H2 conversion factor (𝛼[C ii] ) as a function of redshift. We include measurements drawn from the literature for main￾sequence galaxies (MS), starburst galaxies (SB) and Lymann break analogues (LBA) (Stacey et al. 1991; Ferkinhoff et al. 2014; Huynh et al. 2014; Magdis et al. 2014; Capak et al. 2015; Cormier et al. 2015; Gullberg et al. 2015; Schaerer et al. 2015; Madden et al. 2… view at source ↗
Figure 6
Figure 6. Figure 6: Resolved analysis of the [Cii]–𝑀gas relation in REBELS-25 following the prescription of Vallini et al. (2025) based on simulated galaxies (see text for details). Maps of: [C ii] surface brightness (Σ[C ii] , in L⊙ kpc−2 ) derived from the high–S/N, high–resolution (∼ 0.14′′/700 pc) ALMA data (left panel); resolved [C ii]-to-H2 conversion factor (𝑊[C ii] , in (M⊙ kpc−2 )/(L⊙ kpc−2 )) computed using Eq. 11 i… view at source ↗
read the original abstract

We investigate the molecular gas content and interstellar medium (ISM) conditions of REBELS-25, a massive, star-forming galaxy at $z=7.31$. Deep VLA Q-band and ALMA Band 3 observations reveal CO(3-2) and CO(7-6) emission (both at $\sim3.5\sigma$), and provide an upper limit on [C I](2-1). From the CMB-corrected CO(3-2) flux-representing the highest-redshift detection of a low-$J$ CO transition to date-we derive a molecular gas mass of $M_{\rm mol}=(1.0\pm0.4)\times10^{11}\,(\alpha_{\rm CO}/(3\,$M$_{\odot}$(K$\,$\kms$\,$pc$^2)^{-1}))\,$M$_{\odot}$, directly confirming the presence of a very massive gas reservoir only $\simeq700\,$Myr after the Big Bang. This implies an extreme gas fraction of $f_{\rm gas}\simeq0.95$, a gas-to-dust ratio of $\delta_{\rm GDR}\simeq6\times10^2$, and a depletion timescale of $\tau_{\rm dep}\simeq1.2\,$Gyr, broadly consistent with extrapolated scaling relations for main-sequence galaxies at lower redshift. Using the radiative transfer code TUNER, we self-consistently model CO and dust continuum emission in the context of the significant CMB background, constraining ISM properties and recovering $M_{\rm mol}= (1.8^{+1.0}_{-0.9})\times10^{11}\,$M$_{\odot}$, independent of assumptions about $r_{31}$ and $\alpha_{\rm CO}$. We further discuss the use of alternative molecular gas tracers at early epochs. Combining CO and [C II] measurements, we infer an empirical [C II]-to-H$_2$ conversion factor of $\alpha_{\rm [C II]}=(60\pm25)\,$M$_{\odot}$/L$_{\odot}$, suggesting [C II] remains a viable molecular gas tracer in the Epoch of Reionization. These results demonstrate the detectability of low-$J$ CO emission even at $z>7$, paving the way for next-generation facilities, and provide critical insights into the rapid mass assembly of galaxies during the first billion years of cosmic history.

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 / 1 minor

Summary. The paper reports ~3.5σ detections of CO(3-2) and CO(7-6) in the z=7.31 galaxy REBELS-25 from VLA Q-band and ALMA Band 3 data, derives M_mol=(1.0±0.4)×10^11 (α_CO/3) M_⊙ from the CMB-corrected CO(3-2) flux, and uses the TUNER radiative transfer code to obtain M_mol=(1.8^{+1.0}_{-0.9})×10^{11} M_⊙ independent of r_31 and α_CO while also discussing an empirical α_[C II] conversion factor.

Significance. If the detections and TUNER modeling hold, the result would provide direct evidence for a massive molecular gas reservoir at z>7 and demonstrate the viability of low-J CO at early epochs; the model-independent mass estimate is a notable technical strength when the code is shown to be robust.

major comments (2)
  1. [Abstract, modeling paragraph] Abstract and modeling paragraph: the headline claim that TUNER recovers M_mol independent of r_31 and α_CO rests on the model's ability to correctly solve for excitation, optical depth, and CMB effects at z=7.31; the code is calibrated on lower-redshift systems, yet no test or external benchmark for the high-z regime is provided, making this assumption load-bearing for the reported (1.8^{+1.0}_{-0.9})×10^{11} M_⊙ value.
  2. [Abstract] Abstract: both lines are detected at only ~3.5σ; without explicit details on baseline subtraction, error budgets, or the precise significance calculation in the observations section, it is difficult to assess whether the fluxes are robust enough to support the derived gas mass and f_gas≃0.95.
minor comments (1)
  1. [Abstract] The abstract states an upper limit on [C I](2-1) but does not specify the corresponding luminosity or how it constrains the ISM parameters in the TUNER fit.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We address each major comment below in a point-by-point manner and have revised the manuscript accordingly where the concerns can be directly addressed through additional text or clarifications.

read point-by-point responses

  1. Referee: [Abstract, modeling paragraph] Abstract and modeling paragraph: the headline claim that TUNER recovers M_mol independent of r_31 and α_CO rests on the model's ability to correctly solve for excitation, optical depth, and CMB effects at z=7.31; the code is calibrated on lower-redshift systems, yet no test or external benchmark for the high-z regime is provided, making this assumption load-bearing for the reported (1.8^{+1.0}_{-0.9})×10^{11} M_⊙ value.

    Authors: We appreciate the referee highlighting the importance of validating TUNER's applicability at z=7.31. TUNER solves the radiative transfer equations self-consistently for level populations, optical depths, and excitation, with the elevated CMB temperature at high redshift explicitly included as an input; r_31 and α_CO are therefore derived outputs rather than assumed inputs. The underlying atomic and molecular physics governing CO excitation remains unchanged with redshift, and the dominant high-z modification (CMB) is modeled directly. In the revised manuscript we have added a dedicated paragraph in the modeling section that acknowledges the low-z calibration basis of TUNER, explains why the physical framework still applies, and notes the consistency between the TUNER-derived mass and the independent CO(3-2) luminosity-based estimate. We agree that an external high-z benchmark would be valuable but lies outside the scope of the present work. revision: partial

  2. Referee: [Abstract] Abstract: both lines are detected at only ~3.5σ; without explicit details on baseline subtraction, error budgets, or the precise significance calculation in the observations section, it is difficult to assess whether the fluxes are robust enough to support the derived gas mass and f_gas≃0.95.

    Authors: We agree that the marginal significance of the detections requires fuller documentation. In the revised manuscript we have substantially expanded the 'Observations and Data Reduction' section to provide: (i) the precise baseline-subtraction procedure applied to both the VLA and ALMA spectra, (ii) a complete error budget that includes thermal noise, flux-calibration uncertainties, and any residual baseline or pointing errors, and (iii) the exact significance calculation (integrated line flux divided by the rms measured in line-free channels, scaled by the number of channels in the integration window). These additions allow readers to evaluate the robustness of the reported fluxes and the resulting gas-mass and gas-fraction estimates. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper reports direct CO(3-2) and CO(7-6) detections, applies a CMB correction to the observed flux, and converts to M_mol using a conventional alpha_CO factor. Separately, it applies the external TUNER radiative-transfer code to jointly fit the line and continuum data while solving for excitation and optical depth, yielding an alternative M_mol value. No equation or modeling step is shown to be defined in terms of the output mass, no fitted parameter is relabeled as a prediction, and no load-bearing uniqueness theorem or ansatz is imported via self-citation. The lower-redshift calibration of TUNER is an applicability assumption, not a definitional reduction. The chain therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the applicability of standard CO-to-H2 conversion factors and the TUNER radiative-transfer code at z>7; both are extrapolated from lower-redshift calibrations without new independent verification in this work.

free parameters (1)
  • alpha_CO
    Conversion factor scaled to a Milky-Way value of 3; used to translate CO flux into molecular mass in the primary derivation.
axioms (2)
  • domain assumption CO(3-2) emission traces the total molecular hydrogen reservoir after CMB correction
    Invoked when converting observed flux to M_mol in the abstract.
  • domain assumption TUNER radiative transfer accurately recovers ISM conditions under strong CMB background at z=7.31
    Used to obtain an alpha_CO-independent mass estimate.

pith-pipeline@v0.9.1-grok · 6111 in / 1580 out tokens · 28956 ms · 2026-06-27T06:27:46.096255+00:00 · methodology

discussion (0)

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