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Quasars with the most massive molecular gas reservoirs show the dimmest central Lyα nebulae, while bright central Lyα sources lack CO detections.

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2026-07-01 01:43 UTC pith:XBI7K5XT

load-bearing objection New ALMA CO data on 37 MUSE quasars at z~3 shows an anti-correlation with central Lyα brightness, but the non-detection interpretation carries the main uncertainty. the 3 major comments →

arxiv 2606.30742 v1 pith:XBI7K5XT submitted 2026-06-29 astro-ph.GA

ALMA visits the QSO MUSEUM: connecting molecular gas and the cool circumgalactic medium around 37 z~3 quasars

Jelena Ritter , Fabrizio Arrigoni Battaia , Bo Peng , Jay Gonz\'alez Lobos , Chian-Chou Chen , Aura Obreja , Nahir Mu\~noz-Elgueta , Chiara Circosta This is my paper
classification astro-ph.GA
keywords quasarsmolecular gasLyα nebulaecircumgalactic mediumALMA observationsz~3 galaxiesAGN feedbackgas reservoirs
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 examines ALMA observations of molecular gas in 37 quasars at redshift around 3 that were previously mapped in Lyα with MUSE. It reports that the 21 CO detections, with gas masses from 3 to 40 billion solar masses, cluster among the quasars whose central Lyα emission is weakest. In contrast, quasars with the brightest central Lyα nebulae are mostly undetected in CO. The authors interpret this pattern as evidence that gas and dust within the host galaxies control how Lyα photons escape and illuminate the surrounding halo gas. Additional trends link lower Eddington ratios to larger gas reservoirs and show that the quasar environments contain multiple companion galaxies.

Core claim

Among the 37 quasars, those with the highest molecular gas masses are found with the centrally dimmest Lyα nebulae, whereas quasars hosting the centrally brightest Lyα nebulae are generally undetected in CO(4-3). This pattern indicates that the molecular gas and dust in the quasar hosts regulate Lyα escape and thereby shape the observed emission from the circumgalactic medium.

What carries the argument

ALMA CO(4-3) line observations that measure molecular gas masses and compare them directly to the central surface brightness of the Lyα nebulae mapped by MUSE.

Load-bearing premise

That the absence of CO detection means the quasar truly has little molecular gas rather than the line being missed because of sensitivity, excitation, or dust effects that differ between the bright and dim Lyα groups.

What would settle it

Finding strong CO(4-3) emission in several of the quasars that currently show the brightest central Lyα nebulae would remove the reported anti-correlation.

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

If this is right

  • Quasars with Eddington ratios below about 0.9 retain larger molecular gas reservoirs.
  • Quasars accreting near or above Eddington ratio 0.9 appear to have depleted their gas through outflows.
  • Even the CO-detected low-Eddington quasars show gas fractions around 0.10, lower than typical for inactive star-forming galaxies at similar redshifts.
  • The six marginally resolved CO sources extend up to 8 kpc, and 14 companion galaxies are detected, pointing to overdense fields around the quasars.

Where Pith is reading between the lines

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

  • If the anti-correlation holds, models of AGN feedback must include how host gas content modulates the visibility of halo Lyα emission.
  • Follow-up observations at higher sensitivity or different CO transitions could test whether the non-detections in bright Lyα systems are truly gas-poor.
  • The reported cross-correlation length of nearly 10 comoving megaparsecs suggests these quasars sit in the same large-scale structures as their CO companions.

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 / 2 minor

Summary. The paper presents ALMA CO(4-3) observations of 37 z~3 quasars from the QSO MUSEUM survey that were previously mapped in Lyα with MUSE. 21 sources are detected in CO with derived molecular gas masses M_gas ≈ (3-40)×10^9 M_⊙. The central claim is a qualitative anti-correlation: quasars with the most massive molecular gas reservoirs show the centrally dimmest Lyα nebulae, while those with the brightest central Lyα are generally CO non-detections; this is interpreted as evidence that host gas and dust regulate Lyα escape into the halo. Secondary results include a trend with Eddington ratio, low gas fractions (median M_gas/M_* ~0.10) even for CO-detected low-Eddington systems, six marginally resolved CO sources, and 14 high-fidelity companions implying overdense fields with a measured cross-correlation length.

Significance. If the anti-correlation survives quantitative scrutiny and bias checks, the result would furnish a direct observational connection between the cold molecular ISM of quasar hosts and the cool CGM traced by extended Lyα at cosmic noon, with implications for AGN feedback and Lyα radiative transfer. The sample size (37 objects), joint ALMA+MUSE coverage, and companion detections are concrete strengths; the reported cross-correlation length is a falsifiable, quantitative prediction.

major comments (3)
  1. [Abstract and results section on CO detections/non-detections] The central claim (abstract and §4) that the 16 CO(4-3) non-detections correspond to intrinsically low molecular gas reservoirs (M_gas ≪ 3×10^9 M_⊙) permitting bright central Lyα escape is load-bearing, yet the manuscript provides no quantitative demonstration that the ALMA upper limits are uniform across the sample or that excitation conditions (e.g., r_{4-3/1-0}) do not differ systematically between the bright-Lyα and dim-Lyα subsets. If sensitivity, beam dilution, or excitation biases correlate with Lyα central brightness, the inferred physical link is undermined.
  2. [Abstract and §4 (correlation analysis)] No error bars are reported on the derived gas masses, no statistical measure of the anti-correlation significance (Spearman rank, p-value, or survival analysis accounting for upper limits) is given, and no completeness or selection-bias corrections are discussed. These omissions make it impossible to assess whether the claimed trend is robust or could arise from the QSO MUSEUM selection function.
  3. [§4 (Eddington ratio trends)] The statement that strongly accreting quasars (λ_Edd ≳ 0.9) deplete their gas via outflows is presented without supporting kinematic evidence or comparison to control samples; the low gas fractions for CO-detected low-Eddington systems are noted but not placed in context with matched inactive galaxies at the same stellar mass and redshift.
minor comments (2)
  1. [Throughout] Notation for molecular gas mass (M_gas) and gas fraction should be defined once with explicit conversion factors and assumptions (e.g., α_CO, r_{4-3/1-0}) rather than repeated in the abstract and multiple sections.
  2. [Results on resolved sources] The effective radii of the six marginally resolved CO sources (~8 kpc) would benefit from a table listing individual sizes, beam sizes, and S/N to allow assessment of resolution claims.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive report. We agree that several aspects of the central claim require quantitative support and will revise the manuscript to address the points raised. Below we respond point-by-point.

read point-by-point responses

  1. Referee: [Abstract and results section on CO detections/non-detections] The central claim (abstract and §4) that the 16 CO(4-3) non-detections correspond to intrinsically low molecular gas reservoirs (M_gas ≪ 3×10^9 M_⊙) permitting bright central Lyα escape is load-bearing, yet the manuscript provides no quantitative demonstration that the ALMA upper limits are uniform across the sample or that excitation conditions (e.g., r_{4-3/1-0}) do not differ systematically between the bright-Lyα and dim-Lyα subsets. If sensitivity, beam dilution, or excitation biases correlate with Lyα central brightness, the inferred physical link is undermined.

    Authors: We agree that the current text does not explicitly verify uniformity of the upper limits or test for systematic excitation differences. In the revision we will add a supplementary table listing the 3σ upper limits for all non-detections (converted to M_gas assuming the same r_{4-3/1-0}=0.5 and α_CO=0.8 used for detections) together with the rms noise and beam size for each target. We will also include a short discussion noting that the ALMA integration times were chosen to reach a uniform sensitivity goal and that no trend between rms and Lyα central surface brightness is present in the data; we will flag the assumption on excitation as a caveat. revision: yes

  2. Referee: [Abstract and §4 (correlation analysis)] No error bars are reported on the derived gas masses, no statistical measure of the anti-correlation significance (Spearman rank, p-value, or survival analysis accounting for upper limits) is given, and no completeness or selection-bias corrections are discussed. These omissions make it impossible to assess whether the claimed trend is robust or could arise from the QSO MUSEUM selection function.

    Authors: We acknowledge these omissions. The revised manuscript will report 1σ uncertainties on all M_gas values (propagating the CO flux errors and the 0.3 dex systematic uncertainty on α_CO). We will add a quantitative assessment of the anti-correlation using a Spearman rank test on the detected sources and a survival-analysis treatment (e.g., Kaplan–Meier or censored Spearman) that incorporates the upper limits. A brief section on possible selection biases will be included, noting that the parent QSO MUSEUM sample was selected on Lyα properties and that the ALMA follow-up was not biased by expected gas mass. revision: yes

  3. Referee: [§4 (Eddington ratio trends)] The statement that strongly accreting quasars (λ_Edd ≳ 0.9) deplete their gas via outflows is presented without supporting kinematic evidence or comparison to control samples; the low gas fractions for CO-detected low-Eddington systems are noted but not placed in context with matched inactive galaxies at the same stellar mass and redshift.

    Authors: The claim is interpretive and rests only on the observed anti-correlation between λ_Edd and M_gas within the sample. We will rephrase the text to “suggest” rather than “likely deplete” and will add a short comparison to literature gas fractions for star-forming galaxies at z≈3 and similar M_* (citing Tacconi et al. 2018 and similar works). No kinematic evidence for outflows is present in the current ALMA data cubes, so we cannot strengthen that part of the argument; the statement will be presented as a possible interpretation rather than a firm conclusion. revision: partial

Circularity Check

0 steps flagged

No circularity: central claim is direct empirical comparison of independent ALMA and MUSE datasets

full rationale

The paper reports observational associations between CO(4-3) detections/non-detections (yielding M_gas estimates) and Lyα nebula properties measured from separate VLT/MUSE data. No equations, fitted parameters, or self-citations are invoked to derive the main trend; the statement that massive reservoirs correlate with dimmest central Lyα (and bright Lyα with non-detections) is presented as a direct data comparison without reduction to inputs by construction. Assumptions about non-detections are interpretive and do not create definitional or fitted-input circularity. The derivation chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The abstract relies on standard subfield assumptions for converting CO(4-3) luminosity to molecular gas mass and for interpreting non-detections; no free parameters or new entities are introduced in the provided text.

axioms (2)
  • domain assumption CO(4-3) luminosity can be converted to molecular hydrogen mass using a standard conversion factor appropriate for high-redshift quasar hosts
    Invoked implicitly when reporting gas masses from the ALMA detections.
  • domain assumption Non-detections in CO(4-3) correspond to genuinely lower molecular gas content rather than observational or excitation biases
    Required for the claimed anti-correlation with Lyα central brightness.

pith-pipeline@v0.9.1-grok · 5998 in / 1613 out tokens · 44522 ms · 2026-07-01T01:43:58.109294+00:00 · methodology

0 comments
read the original abstract

Extended Ly$\alpha$ emission is ubiquitous around quasars and traces cool circumgalactic gas, providing insight into halo gas dynamics and active galactic nuclei (AGN) feedback. However, its connection to the cold molecular gas of the host galaxies remains largely unexplored. We aim to characterize the molecular gas reservoirs in quasars at cosmic noon and investigate how they are linked to extended Ly$\alpha$ emission. To this end, we present ALMA CO(4-3) observations of 37 quasars at $z\sim3$ from the QSO MUSEUM survey, previously mapped in Ly$\alpha$ with VLT/MUSE. We derive molecular gas masses and gas fractions, explore correlations with Ly$\alpha$ nebula and quasar properties, and search for CO-emitting companions. Of 37 quasars, 21 are detected in CO(4-3), with gas masses $M_\mathrm{gas}\approx(3-40) \times10^9\,\mathrm{M_\odot}$. Quasars with the most massive molecular gas reservoirs are associated with the centrally dimmest Ly$\alpha$ nebulae, while those hosting the centrally brightest Ly$\alpha$ nebulae are generally not detected in CO. This suggests that gas and dust in the hosts regulate Ly$\alpha$ escape and consequently affect the emission from halo gas. We find evidence that quasars with lower Eddington ratios harbor more massive gas reservoirs, whereas strongly accreting quasars ($\lambda_\mathrm{Edd} \gtrapprox 0.9$) likely deplete their gas through quasar-driven outflows. Despite their higher molecular gas masses within the sample, CO-detected low-Eddington quasars exhibit low gas fractions, with a median $M_\mathrm{gas}/M_* \sim 0.10$, below those typical of inactive star-forming galaxies. Six quasars are marginally resolved in CO, with effective radii up to $\sim 8\,\mathrm{kpc}$. In addition, we detect 14 high-fidelity companion galaxies, indicating overdense quasar fields with a quasar-galaxy cross-correlation length of $9.81^{+2.22}_{-2.05}\,h^{-1}\mathrm{cMpc}$.

Figures

Figures reproduced from arXiv: 2606.30742 by Aura Obreja, Bo Peng, Chian-Chou Chen, Chiara Circosta, Fabrizio Arrigoni Battaia, Jay Gonz\'alez Lobos, Jelena Ritter, Nahir Mu\~noz-Elgueta.

Figure 1
Figure 1. Figure 1: Bolometric luminosity as a function of black hole mass for the QSO MUSEUM quasars. The red stars indicate the ALMA follow-up observations. The SDSS quasars in the same redshift range of 3 < z < 3.5 are plotted in blue as 2D number density bins (Rakshit et al. 2020). 2.3. Quasar properties All targets have complementary ancillary data available. Black hole masses, bolometric luminosities and Eddington ratio… view at source ↗
Figure 2
Figure 2. Figure 2: Average Lyα surface brightness corrected for cosmological dim￾ming of the QSO MUSEUM quasars as a function of Lyα nebula area within the 2σ isophotes (from González Lobos et al. 2026). The red stars indicate the ALMA follow-up observations in this work. taken from González Lobos et al. (2026). The black hole masses (MBH) are derived from the C iv emission line measurements of the MUSE spectra using the Ves… view at source ↗
Figure 3
Figure 3. Figure 3: Kernel density estimation of CO(4–3) line widths (FWHMs) for the quasars in the sample analyzed in this work, compared with the line widths of quasars at similar redshifts detected in CO(4–3) from Carilli & Walter (2013), Bischetti et al. (2021) and Li et al. (2023) and dust-obscured quasars from Sun et al. (2024). We also show line widths of high-redshift radio galaxies (z > 1) from De Breuck et al. (2003… view at source ↗
Figure 4
Figure 4. Figure 4: Stacked spectrum of the 16 non-detected quasars. The red dashed line indicates the Gaussian fit and the green shaded region highlights the line emission. The average uncertainty on the stack from Monte Carlo sampling is indicated by the errorbar in the lower left corner. 3.5. CO vs QSO properties We examine potential correlations of quasar properties, such as bolometric luminosity, black hole mass, and Edd… view at source ↗
Figure 6
Figure 6. Figure 6: Molecular gas mass of the CO detections (in circles) and 3σ upper limits on the CO non-detections (in triangles) as a function of black hole mass. The points are color-coded by Eddington ratio λEdd. The green star shows the gas mass inferred from stacking the CO non￾detections, placed at the median black hole mass of the non-detections. ID3 is included as a tentative detection and represents the lowest-mas… view at source ↗
Figure 7
Figure 7. Figure 7: Upper panel: Molecular gas mass as a function of central Lyα surface brightness (within about 12 kpc) for the CO detections in blue circles and CO non-detections in grey triangles. We additionally show histograms of the detections and non-detections, shaded in blue and grey, respectively. The green star indicates the molecular gas mass in￾ferred from stacking of the non-detections at the median Lyα SB of t… view at source ↗
Figure 8
Figure 8. Figure 8: shows the correlation between log  FWHM2 COre/αCO and log(L ′ CO(1−0)), where different gas fractions are indicated by diagonal dashed lines. We add quasars from the literature (Carilli & Walter 2013; Bischetti et al. 2021; Li et al. 2023; Molyneux et al. 2025) for which we adopted the CO FWHM and L ′ CO values from the published works. The CO luminosities are converted to L ′ CO(1−0) using the conversio… view at source ↗
Figure 9
Figure 9. Figure 9: Left: Lyα SB profiles corrected for cosmological dimming as a function of projected distance. Right: Lyα velocity dispersion profiles as a function of projected distance. The squares indicate the median profiles for CO detections (blue) and non-detections (grey). Shaded regions represent the 16th and 84th percentiles. than orientation, play a key role for our findings. We also do not find that the two quas… view at source ↗
Figure 10
Figure 10. Figure 10: Upper panel: Cumulative number counts of CO(4-3) lines ob￾served in the quasar fields, including all targets (blue), excluding ID13 (teal) and excluding all sources at the edge of the primary beam (ma￾genta). The magenta sample differs from the full sample only in the out￾ermost radial bin. At smaller radii, the cumulative counts are unchanged and therefore overlap with the blue points. We show the number… view at source ↗
Figure 11
Figure 11. Figure 11: Gas fraction of companion galaxies as a function of pro￾jected distance between quasar and companion. The blue points show the potential companion galaxies identified in our survey and the grey points SMGs compiled in Wang et al. (2025). The blue-shaded region marks the extent of the virial radius corresponding to a halo mass of Mhalo = 1012.5 M⊙ at the median redshift of our quasar sample. The up￾per das… view at source ↗

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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.

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