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Evidence for universal gas depletion in a sample of 41 luminous Type 1 quasars at z $\sim$ 2

T0 review · 2 major / 6 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read Luminous unobscured quasars at z~2 are gas-poor: gas fractions of 0.02-0.32 lie below inactive galaxies and obscured quasars, marking an evolutionary shift from gas-rich obscured to gas-poor unobscured hosts.

desk verdict Useful new CO sample, honest sensitivity analysis, but 'universal depletion' leans on a single geometric assumption only three sources justify. read the letter →

arxiv 2505.03884 v1 pith:GROTC75V submitted 2025-05-06 astro-ph.GA

S. J. Molyneux , M. Banerji , M. J. Temple , M. Aravena , R. J. Assef , P. Hewett , G. C. Jones , A. Puglisi
show 4 more authors
A. L. Rankine C. Ricci M. Stepney S. Tang
This is my paper · ORCID
classification astro-ph.GA
keywords quasarsmoleculargasfractionsCOemissionAGNfeedbackgalaxyevolutioncosmicnoonType1
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 tries to establish that the brightest unobscured quasars at redshift $\sim 2$ — the epoch of peak star formation, 'cosmic noon' — are systematically gas-depleted: they hold far less molecular gas per unit stellar mass than typical star-forming galaxies or than obscured quasars of similar luminosity. Using 41 quasars with carbon-monoxide (CO) observations from a millimetre interferometer, it derives gas masses and dynamical masses and finds gas fractions in the range $0.02$–$0.32$, with a median near $0.06$. If this is right, it matters because it places luminous AGN activity at the end of a gas-clearing sequence: a galaxy fuelling a bright quasar first appears dusty, gas-rich and obscured, then sheds its molecular reservoir and emerges as a blue, unobscured, gas-poor quasar. The paper also reports a tentative connection between higher gas fractions and stronger broad-line-region winds traced by C IV blueshifts.

What carries the argument

The load-bearing machinery is the chain from CO line measurements to gas fractions. A CO(3–2) luminosity is converted to CO(1–0) using fixed line ratios ($r_{31}=0.97$, $r_{41}=0.87$, $r_{71}=0.20$) and then to molecular gas mass with $\alpha_{\rm CO}=0.8\ M_\odot\,({\rm K\,km\,s^{-1}\,pc^2})^{-1}$; dynamical masses come from the CO line width through a rotating-disk model, $M_{\rm dyn} = 1.16\times 10^5 \times 0.75 \times \mathrm{FWHM_{CO}} \times \sin(i)^2 \times r_{\rm kpc}$, with inclination $i=30^\circ$ and radius $r=5\ {\rm kpc}$ assumed for every target; stellar masses are the remainder $M_\star = M_{\rm dyn} - M_{\rm BH} - M_{\rm gas}$, so the gas fraction is $M_{\rm gas}/M_\star$. Because only three targets are spatially resolved, the single assumed radius is what carries the depletion contrast.

What would settle it

Resolve the CO emission in a representative subset of about a dozen of these quasars at sub-kiloparsec resolution and measure the actual radii and orientations; if the median radius is close to $2\,\mathrm{kpc}$ rather than $5\,\mathrm{kpc}$, the dynamical-mass equation raises the median $\log_{10} f_{\rm gas}$ from $-1.22$ to $-0.76$, largely erasing the claimed depletion relative to the star-forming main sequence. Alternatively, measure stellar masses independently from rest-frame optical or near-infrared SED fitting and recompute the gas fractions directly.

Watch

Extended reading notes

Core claim

The central claim is that luminous, unobscured (Type 1) quasars at $z\sim 2$ have depleted molecular gas reservoirs. In the 20 of 41 targets with CO detections the median gas mass is $8.0 \pm 1.5 \times 10^9\,M_\odot$, the median dynamical mass is $1.4 \pm 0.9 \times 10^{11}\,M_\odot$, and the gas fractions $M_{\rm gas}/M_\star$ range from $0.02$ to $0.32$ with median $0.06 \pm 0.09$. These values sit below both inactive main-sequence galaxies at the same redshift and obscured quasar populations (red quasars and hot dust-obscured galaxies) at comparable luminosity. The authors interpret the ordering obscured/gas-rich $\rightarrow$ unobscured/gas-poor as an evolutionary trend: the same luminous phase that evacuates nuclear dust and gas leaves a gas-poor host. They also present tentative evidence that quasars with stronger disk winds (C IV blueshifts above $1000\ \mathrm{km\,s^{-1}}$ and weak He II) have somewhat higher gas fractions, and they find no strong sign that these quasars live in extremely dense environments.

Load-bearing premise

The entire depletion signal rests on assuming every quasar's molecular gas sits in a rotating disk of radius $5\,\mathrm{kpc}$ inclined at 30 degrees; if the true sizes are closer to $2\,\mathrm{kpc}$, the paper's own calculation shifts the median gas fraction upward by about half a decade and the gap to star-forming galaxies narrows considerably.

Editorial extensions

If this is right

  • If the depletion is real, the most luminous unobscured quasars at $z\sim2$ are not sites of ongoing vigorous star formation but hosts whose molecular fuel has been largely consumed or expelled.
  • Gas fractions rise with obscuration across comparable luminous samples, so the molecular reservoir shrinks as the quasar sheds its dusty cocoon; the ordering is consistent with a gas-rich obscured phase preceding the unobscured phase.
  • Quasars with the strongest broad-line winds (C IV blueshift above $1000\ \mathrm{km\,s^{-1}}$) tend toward higher gas fractions, suggesting that disk winds are more easily launched when some cold gas remains rather than in fully depleted hosts.
  • Only about 15 percent of the sample shows CO-bright companions at the achieved sensitivity, so luminous quasars at this epoch do not appear to require extreme overdensities; deeper observations could still uncover fainter companions.

Reading between the lines

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

  • A direct extension the authors leave implicit: if the gas-poor unobscured phase is the end state, the same targets should show recently removed gas — for example broad molecular outflows or excess ionised gas — at a rate that scales with how far below the main sequence each object sits; stacking the non-detections for broad wings, which the paper begins to do, is a cheap test.
  • The tentative C IV/gas-fraction link could be sharpened by testing whether gas fraction correlates more tightly with Eddington ratio or with wind velocity, using the same sample's measured black-hole masses and $L/L_{\rm Edd}$ values.
  • Because stellar masses are here derived rather than measured, the cleanest independent check is rest-frame optical or near-infrared SED fitting for a subsample; higher stellar masses would make the depletion stronger, while lower stellar masses would weaken it.
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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

2 major / 6 minor

Summary. This paper presents ALMA CO observations of 41 luminous unobscured quasars at z∼2 from SDSS, comprising a main sample of 32 sources observed in CO(3-2) plus 9 archival sources observed in CO(3-2), CO(4-3), or CO(7-6). The authors measure CO luminosities, derive gas masses using fixed conversion factors (α_CO = 0.8, r31 = 0.97, r41 = 0.87, r71 = 0.2), and compute dynamical masses from CO line widths under the assumption of ordered rotation with a fixed radius r = 5 kpc and inclination i = 30° for all sources (Eq. 3). Stellar masses are then obtained as M★ = M_dyn − M_BH − M_gas (Eq. 7), so gas fractions (Eq. 8) depend directly on the assumed geometry. The central finding is that these quasars have low gas fractions, median ∼0.06, 'generally lower than both inactive galaxies and obscured quasars at similar redshifts', which the authors attribute to an evolutionary trend from gas-rich obscured quasars to gas-poor unobscured quasars. They also report a tentative correlation with C IV blueshift / He II EW and identify a few CO-detected companions. A sensitivity analysis in Section 4.1 shows that changing the radius to 2 kpc raises the median log10 f_gas from −1.22 to −0.76 (median f_gas ≈ 0.17) and that implausible values (r31 ≈ 0.1 or α_CO ≈ 11) would be required to erase the deficit entirely.

Significance. If the result holds, it is an important piece of evidence for AGN-driven gas depletion in the most luminous quasars at cosmic noon, a regime where simulations currently do not predict depleted reservoirs. The paper's strengths are its relatively large and uniformly selected sample, the homogeneous ALMA processing, the explicit sensitivity analysis in Section 4.1 (which correctly identifies the magnitude of the geometric prior), and the connection drawn between BLR/NLR outflow indicators and the molecular ISM. The paper also includes upper limits for non-detections and makes the reduced data available on request. These features make the work potentially valuable to the AGN feedback community, provided the central geometric assumption is either better justified or the conclusions are appropriately caveated.

major comments (2)
  1. [3.3 (Eq. 3) and 4.1] The central claim of universal gas depletion rests on a single assumed CO-emitting radius r = 5 kpc and inclination i = 30° for every source, although only three objects are spatially resolved (sizes 0.53–0.65 arcsec ≈ 5 kpc). Because the stellar mass is not independently measured but is defined by M★ = M_dyn − M_BH − M_gas (Eq. 7), the assumed radius propagates directly into every gas fraction. The paper's own test in Section 4.1 shows that adopting r = 2 kpc changes the median log10 f_gas from −1.22 to −0.76, i.e., the median f_gas rises from ≈0.06 to ≈0.17, reducing the contrast with star-forming galaxies by roughly a factor of three. At smaller radii or larger inclinations (the sin^2(i) dependence in Eq. 3 is significant) the gap could close further. Since only a single discrete sensitivity check is reported rather than a marginalisation over physically plausible (r, i), the 'universal' conclusion is conditional on an unverified geometric prior. I ask the authors to (a) adopt resolved sizes where available and marginalise over plausible radius and inclination distributions, or (b) substantially soften the wording in the abstract and conclusions, quantifying how the significance of the deficit changes with r and i.
  2. [4.1, Fig. 7, Table 2] The comparison that justifies the statement that gas fractions are 'generally lower than both inactive galaxies and obscured quasars' mixes literature samples with widely different α_CO and line-ratio conventions (Table 2: α_CO ranges from 0.8 to 3.6 for Perna+18, is 3.6 for Circosta+21, and 0.66–15.22 for Sanders+23 SFGs). Since f_gas scales linearly with the assumed α_CO (Eq. 6), the apparent deficit relative to star-forming galaxies could partly reflect these convention differences rather than an intrinsic physical depletion. The sensitivity test in Section 4.1 (r31 ≈ 0.1 or α_CO ≈ 11 would erase the deficit) is reassuring, but it applies only to the authors' own measurements, not to the comparison samples. I recommend that the authors recompute all literature gas fractions with a common set of conversion factors (as already done for the obscured quasars in Fig. 8) or explicitly quantify how the deficit depends on adopting plausible alternative α_CO and line ratios for the comparison samples.
minor comments (6)
  1. [Abstract] The abstract uses 'CIV' but the main text uses 'Civ'; please standardise the notation for the C IV line.
  2. [3.3 (Eq. 3)] Eq. (3) as printed appears dimensionally inconsistent (FWHM appears without a square, and sin^2(i) appears in the numerator); please verify the expression against Wang et al. (2013) and Bischetti et al. (2021), and specify the units of each term.
  3. [4.1] The sentence 'Molecular gas at 5kpc has been identified but as outflows and not part of the mainbulkrotation' is incomplete and unclear; please rephrase to state whether such 5 kpc gas is associated with rotation or with outflows, and cite the relevant literature.
  4. [Table 3] For non-detections the gas fraction column lists values such as '<0.05', but the caption does not explicitly state that these are 3σ upper limits computed with the assumed median line width; please clarify the caption.
  5. [Fig. 7] The grey line for main-sequence star-forming galaxies from Tacconi et al. (2020) should be accompanied by a statement of the stellar mass and the α_CO / line-ratio assumptions used to place it on the plot.
  6. [3.7] There is a typo: 'J1606+16735' should be 'J1606+1735' as listed in Table 3; also check 'J0052+0104' versus 'J0052+0140' for consistency.

Circularity Check

0 steps flagged · score 1.0 of 10

No circular derivation: gas masses and dynamical masses come from independent ALMA measurements plus external conversion factors; the acknowledged self-reference in Eq. 7 and the assumed 5 kpc radius are limitations, not built-in predictions.

full rationale

The central claim of low gas fractions rests on ALMA CO detections. Gas masses are derived from L'_CO using external alpha_CO = 0.8 (Downes & Solomon 1998; Bolatto et al. 2013) and literature line ratios r31 = 0.97, r41 = 0.87, r71 = 0.2; none of these is fitted to the present sample. Dynamical masses come from measured CO FWHM and an assumed ordered-rotation geometry (Eq. 3), and stellar masses are defined as the residual Mdyn - MBH - Mgas (Eq. 7). The paper explicitly flags that fgas then depends on the gas-mass assumptions, and Section 4.1 presents a sensitivity test showing that adopting r = 2 kpc changes the median log10(fgas) from -1.22 to -0.76; this is an acknowledged conditional assumption, not a result forced by construction. The evolutionary interpretation comparing obscured and unobscured quasars is a literature comparison rather than a self-derived prediction. Self-citations to Rankine et al. (2020), Temple et al. (2023), and Molyneux et al. (2024) provide sample selection, spectral products, and line-ratio priors, but none is load-bearing in the sense of substituting for the new ALMA measurements or invoking a uniqueness theorem. No step reduces a claimed prediction to its own input by construction, so no circular step is listed.

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

The central quantities (gas masses, dynamical masses, gas fractions) all depend on several externally chosen conversion factors and geometric assumptions that are not fitted to the data. The most influential is the single size r=5 kpc adopted for all unresolved targets. No new physical entities are introduced.

free parameters (5)
  • CO-emitting radius r = 5 kpc (assumed for all targets; only 3 resolved with 0.53-0.65 arcsec)
    Used in Eq. 3 to compute dynamical masses and hence stellar masses and gas fractions for all galaxies; Section 4.1 shows r=2 kpc changes median log10 fgas to -0.76 from -1.22.
  • Inclination i = 30 degrees
    Average inclination assumed for Type 1 quasars (Mountrichas et al. 2021); enters Eq. 3 as sin(i)^2.
  • alpha_CO = 0.8 Msun/(K km/s pc^2)
    CO-to-H2 conversion factor from Downes & Solomon 1998; used in Eq. 6 to derive gas masses; sensitivity tested in Section 4.1.
  • CO line ratios r31, r41, r71 = 0.97, 0.87, 0.20
    Adopted from Carilli & Walter 2013 and Molyneux et al. 2024 to convert observed CO transitions to CO(1-0); central to gas mass estimates.
  • FWHM for non-detections = Median FWHM of detections (~170-620 km/s)
    Assumed to convert 3-sigma rms to luminosity upper limits; affects upper-limit gas fractions.
assumptions (5)
  • domain assumption CO-emitting gas is in ordered circular rotation
    Eq. 3 uses FWHM_CO with sin(i) to compute dynamical mass; non-circular or outflow-dominated kinematics would bias Mdyn.
  • domain assumption Dark matter fraction is negligible within the CO-emitting radius
    Stated in Section 3.3 before Eq. 3; if dark matter contributes significantly, Mdyn overestimates baryonic mass.
  • domain assumption CO luminosity traces the bulk molecular gas reservoir
    Standard assumption in Section 3.4; if CO excitation or optical depth varies, gas masses change.
  • domain assumption Literature line ratios and alpha_CO apply to these luminous quasars
    Section 3.4 adopts r31=0.97, r41=0.87, r71=0.2 and alpha_CO=0.8 from other quasar studies; deviation would alter gas masses and gas fractions.
  • domain assumption Stellar mass equals Mdyn - MBH - Mgas
    Eq. 7; this ignores other baryonic components and assumes all dynamical mass is accounted for by BH plus gas plus stars; noted by the authors as making fgas dependent on gas mass assumptions.

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Cite this review

Pith. "Pith review of Evidence for universal gas depletion in a sample of 41 luminous Type 1 quasars at z $\sim$ 2." pith.science (2026). https://pith.science/paper/GROTC75V

@misc{pith2026250503884,
  author       = {Pith},
  title        = {Pith review of: Evidence for universal gas depletion in a sample of 41 luminous Type 1 quasars at z $\sim$ 2},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GROTC75V}},
  note         = {Machine review of arXiv:2505.03884}
}
abstract

We present ALMA CO observations of the molecular gas in a sample of 41 luminous unobscured quasars at z $\sim$ 2 from the Sloan Digital Sky Survey. 32 targets comprise the main sample observed in CO(3-2) and 9 targets have archival ALMA data of CO(3-2), CO(4-3) and CO(7-6). All quasars have rest-UV to optical spectra tracing ionised gas in the broad line region (e.g. CIV) and the narrow line region (e.g. [OIII]) and they cover the full range of outflow properties in the SDSS quasar population at these redshifts. 15 out of the 32 quasars in the main sample are detected in CO(3-2) and five out of the nine archival quasars are also detected in CO. The median gas mass for all 20 CO detected quasars is 8.0 $\pm$ 1.5 $\times$ 10$^9$ M$_{\odot}$ with a median M$_{dyn}$ of 1.4 $\pm$ 0.9 $\times$ 10$^{11}$ M$_{\odot}$. We find gas fractions in the range 0.02 - 0.32, which are generally lower than both inactive galaxies and obscured quasars at similar redshifts. We suggest an evolutionary trend in gas fractions of quasar host galaxies from obscured and gas rich to unobscured and gas poor. We note a tentative correlation between the gas fractions and the broad-line region properties with quasars showing high CIV blueshifts, indicating stronger broad-line region winds, having higher gas fractions. Six of the quasars corresponding to 15% of the sample also show evidence for at least one companion galaxy detected in CO at the same redshift.

Figures

Figures reproduced from arXiv: 2505.03884 by the authors.

Figure 1
Figure 1. Here we present the sample selection for the quasars presented in this work. We plot the sample in the redshift and 3000Å luminosity parameter space, coloured by the C iv blueshifts. The grey contours/shaded region indicate the full distribution of SDSS DR16 quasars from Rankine et al. 2020; Temple et al. 2023. Diamonds indicate the main sample from ALMA project ID 2021.1.00393.S (PI: M. Temple). We also show archiv… view at source ↗
Figure 2
Figure 2. Example spectrum and spectral fitting for the target J0014+0912. We present the flux density versus velocity, in velocity bins of 50 km s −1 . The solid black line shows the Gaussian fit to the emission line and the dashed vertical line represents the zero velocity at the expected redshift determined from H𝛼. The same format is used for all other spectra presented in this work (shown in [PITH_FULL_IMAGE:figures/ful… view at source ↗
Figure 3
Figure 3. Figure showing the velocity offsets between the CO redshift and the H𝛼 redshift (top panel) and UV redshift (bottom panel). These are plotted against the FWHMCO. on CO size measurements from casa when fitted using the imfit routine. Only three targets were spatially resolved and therefore have reliable size measurements. The sizes ranged between 0.53 and 0.65 arcsec, with an average of 0.6 arcsec, corresponding to 5… view at source ↗
Figures from the paper (12 more)
Figure 5
Figure 5. Figure 5: Here we present the FWHMCO versus the CO luminosity for all targets within our sample with detections. These properties trace the dynam￾ical mass and the gas mass respectively. We plot other quasars and AGN taken from the literature (Wang et al. 2010; Circosta et al. 2…
Figure 6
Figure 6. Figure 6: Violin plots to show the distribution of gas fractions when splitting the sample by different UV/optical properties. The middle solid vertical lines represent the median of the distributions and the outer 2 vertical lines show 16th and 84th quartiles. The larger region…
Figure 7
Figure 7. Figure 7: Figure showing the gas fractions of our sample of quasars in relation to other samples of quasars, AGN and star-forming galaxies up to redshifts of 5. The grey line indicates the relation for main-sequence star-forming galaxies with stellar mass 1011 M⊙ described in Ta…
Figure 8
Figure 8. Figure 8: Gas fraction vs bolometric luminosity. Here we focus on the AGN and quasars above z = 2 and with Lbol > 1046.5 erg s−1 . Open circles and triangles are unobscured, filled circles and triangles are obscured/red quasars. For all samples presented here we calculate the ga…
Figure 9
Figure 9. Figure 9: Left panel: Narrowband image collapsed over the frequency range indicated in the top left of the cutout. The black cross indicates the centre of the observation. The grey ellipse represents the corresponding beam size. The red ellipse indicates the region where the spe…
Figure 9
Figure 9. Figure 9: continued. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p016_9.png]
Figure 9
Figure 9. Figure 9: continued. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p017_9.png]
Figure 9
Figure 9. Figure 9: continued. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p018_9.png]
Figure 10
Figure 10. Figure 10: Spectra of companion galaxies to the quasars. Left panel: Narrowband image collapsed over the frequency range indicated in the top left of the cutout. The black cross indicates the centre of the observation. The grey ellipse represents the corresponding beam size. The…
Figure 10
Figure 10. Figure 10: continued. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p020_10.png]
Figure 11
Figure 11. Figure 11: Continuum images for all those with continuum detections. Black crosses indicate the centre of observations. Black contours begin at 2 sigma. Black dashed contours correspond to negative 2 sigma (where present). MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fi…
Figure 11
Figure 11. Figure 11: continued. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p022_11.png]

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Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.