arxiv: 2604.18503 · v2 · submitted 2026-04-20 · 🌌 astro-ph.GA

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NOEMA3D: Resolving radial gas flows in disk galaxies at z~1.1-1.6 with high-resolution CO observations

Jean-Baptiste Jolly , Linda J. Tacconi , Reinhard Genzel , Roberto Neri , Karl Schuster , Jianhang Chen , Natascha M. F\"orster Schreiber , Stavros Pastras

show 29 more authors

Letizia Scaloni Giulia Tozzi Capucine Barf\'ety Alberto Bolatto Andreas Burker Fran\c{c}oise Combes Pierre Cox Ric Davies Frank Eisenhauer Juan Manuel Espejo Salcedo Rodrigo Herrera-Camu Santi Garc\'ia-Burillo Tadayuki Kodama Lilian Lee Minju M. Lee Daizhong Liu Dieter Lutz Giovanni Mazzolari Thorsten Naab Amit Nestor Shachar Claudia Pulsoni Alvio Renzini Monica Rubio Taro T. Shimizu Amiel Sternberg Eckhard Sturm Hannah \"Ubler Antonio Usero Stijn Wuyts

Authors on Pith no claims yet

Pith reviewed 2026-05-10 04:25 UTC · model grok-4.3

classification 🌌 astro-ph.GA

keywords high-redshift galaxiesmolecular gas kinematicsradial flowsspiral armsgalactic barscosmic noonCO observationsgalaxy morphology

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The pith

High-resolution CO observations show that spiral arms and bars in z~1-2 disk galaxies drive molecular gas inflows at rates comparable to star formation.

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

The paper presents deep NOEMA CO observations of ten massive main-sequence galaxies at redshift 1.1 to 1.6, combined with JWST imaging, to map molecular gas kinematics on kiloparsec scales. After fitting axisymmetric rotation models, the remaining velocity residuals align spatially with spiral arms and bars, which the authors interpret as radial flows with typical net inflows around 50 solar masses per year. These rates are comparable to the galaxies' star formation rates, implying that non-axisymmetric structures efficiently channel cold gas inward during the late stages of cosmic noon. This establishes a direct connection between galaxy morphology and internal gas transport at this epoch.

Core claim

After modeling the axisymmetric rotation with DysmalPy, we reveal spatially coherent velocity residuals in all but one more inclined system. The inferred in-plane non-circular motions reach amplitudes of ~50-100 km/s. Interpreting these non-circular motions as radial flows we find that the velocity residuals spatially coincide with non-axisymmetric structures -- spiral arms and bars -- demonstrating a direct link between galaxy morphology and gas transport at z ~ 1-2. In spiral galaxies, the residual velocity patterns are typically dominated by inflows, while barred systems display an apparent inflow-outflow pattern. We further find that the inferred molecular gas inflow rates are of the the

What carries the argument

Velocity residuals after subtraction of axisymmetric rotation via DysmalPy forward modeling, whose spatial alignment with JWST-detected spiral arms and bars is used to infer in-plane radial gas flows.

Load-bearing premise

That the observed velocity residuals represent purely in-plane radial flows driven by the morphological features rather than warps, vertical motions, outflows, or modeling imperfections.

What would settle it

If independent kinematic modeling that includes warps or vertical velocities removes the residuals or if the residuals show no spatial correlation with the locations of spiral arms and bars.

Figures

Figures reproduced from arXiv: 2604.18503 by Alberto Bolatto, Alvio Renzini, Amiel Sternberg, Amit Nestor Shachar, Andreas Burker, Antonio Usero, Capucine Barf\'ety, Claudia Pulsoni, Daizhong Liu, Dieter Lutz, Eckhard Sturm, Fran\c{c}oise Combes, Frank Eisenhauer, Giovanni Mazzolari, Giulia Tozzi, Hannah \"Ubler, Jean-Baptiste Jolly, Jianhang Chen, Juan Manuel Espejo Salcedo, Karl Schuster, Letizia Scaloni, Lilian Lee, Linda J. Tacconi, Minju M. Lee, Monica Rubio, Natascha M. F\"orster Schreiber, Pierre Cox, Reinhard Genzel, Ric Davies, Roberto Neri, Rodrigo Herrera-Camu, Santi Garc\'ia-Burillo, Stavros Pastras, Stijn Wuyts, Tadayuki Kodama, Taro T. Shimizu, Thorsten Naab.

**Figure 1.** Figure 1: All galaxies in the NOEMA3D sample: color composite images (typically from JWST, NIRCam, see Table A.1 for the list of filters used), placed on the SFR vs M⋆ plane (see [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗

**Figure 3.** Figure 3: (top) Velocity dispersion as a function of redshift. (bot [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗

**Figure 4.** Figure 4: (top) Average in plane radial flow velocities as a func [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗

**Figure 5.** Figure 5: Kinematic profiles of the NOEMA3D galaxies (one per row). From left to right: color composite image of the galaxy; rotation curve, data and model; dispersion profile, data and model; CO flux profile, data and model. All profiles are extracted from a slit along the major axis (see Section 3). The di fferent weightings of each galaxy are fitted simultaneously to increase reliability. Article number, page 15 … view at source ↗

read the original abstract

We present NOEMA3D, a unique high-resolution study of purely molecular gas kinematics at $z \sim 1.1$ to 1.6, providing a dedicated view of cold gas dynamics at the late stages of the peak epoch of cosmic star formation. Using deep ($> 20$ hr on source per target) IRAM-NOEMA CO observations of 10 massive ($10.45 < \log(M^*/M_\odot) < 11.43$)) main-sequence galaxies, complemented by high-resolution JWST imaging, we resolve the molecular gas kinematics and morphology on kiloparsec scales. We find that all galaxies exhibit ordered rotation with moderate intrinsic turbulence (median $\sigma_0 \sim 32 \pm 10$ km/s, median $V_c/\sigma_0 \sim 8.6 \pm 2.9$), consistent with dynamically turbulent disks at late cosmic noon. After modeling the axisymmetric rotation with the forward-modeling code DysmalPy, we reveal spatially coherent velocity residuals in all but one more inclined system. The inferred in-plane non circular motions reach amplitudes of $\sim 50$-100 km/s, significantly larger than typically observed in local disk galaxies. Interpreting these non-circular motions as radial flows we find that the velocity residuals spatially coincide with non-axisymmetric structures -- spiral arms and bars -- demonstrating a direct link between galaxy morphology and gas transport at $z \sim 1$-2. In spiral galaxies, the residual velocity patterns are typically dominated by inflows, while barred systems display an apparent inflow-outflow pattern, characteristic of in-plane bar-driven gas motions. We further find that the inferred molecular gas inflow rates are substantial, with a typical net inflow rate of the order of the star formation rate ($\dot M \sim -50 M_\odot$/yr). This implies that spiral arms and bars at cosmic noon are highly efficient at funneling cold gas toward galaxy centers, perhaps driving the buildup of bulges and feeding central star forming regions and supermassive black holes.

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.

Desk Editor's Note private letter to a colleague

New kpc-scale CO kinematics at z~1.1-1.6 show morphology-aligned velocity residuals, but the radial-inflow interpretation depends on an untested thin-disk assumption.

read the letter

The key takeaway is that this work provides resolved molecular gas kinematics for a sample of galaxies at the tail end of the peak star formation epoch, showing non-circular motions that line up with bars and spirals from JWST data. They observed ten galaxies with NOEMA for more than twenty hours each, achieving kiloparsec resolution in CO. Using DysmalPy to model the axisymmetric part, they uncover coherent residuals of 50 to 100 km/s in nine out of ten cases. These patterns match the locations of spiral arms and bars, and they derive net inflow rates around 50 solar masses per year. The paper does a good job with the observational setup and the basic kinematic parameters. The median velocity dispersion of 32 km/s and Vc over sigma of 8.6 fit with expectations for turbulent high-redshift disks. Pairing the gas maps with high-resolution morphology adds a useful layer. The soft spot sits in how they convert those residuals into radial inflow rates. The forward modeling assumes a flat disk geometry, so any warp or vertical motion would show up in the residuals too. They don't present tests that isolate the radial component or compare to models with outflows. The fact that the most inclined galaxy shows no residuals hints that geometry matters. This makes the claim of efficient funneling by arms and bars rest on an assumption that could be checked more directly. Readers working on galaxy evolution and gas dynamics at z~1-2 will find the numbers and maps interesting. The data is new and the analysis is standard, so it merits a serious referee even if some conclusions need tightening.

Referee Report

3 major / 2 minor

Summary. The paper reports deep NOEMA CO(2-1) observations of 10 massive main-sequence galaxies at z~1.1-1.6, combined with JWST imaging. Forward modeling with DysmalPy decomposes the molecular gas kinematics into axisymmetric rotation plus turbulence (median Vc/σ0 ~8.6), revealing coherent velocity residuals of 50-100 km/s in 9/10 systems. These residuals are interpreted as in-plane radial flows that align spatially with spiral arms and bars, yielding net molecular inflow rates ~50 M⊙ yr⁻¹ comparable to the SFR and implying efficient morphology-driven gas transport at cosmic noon.

Significance. If the residuals are shown to be radial inflows, the work supplies rare kpc-scale constraints on cold-gas dynamics at the end of cosmic noon and links non-axisymmetric structures to central gas delivery. The depth of the NOEMA data, the use of forward modeling, and the joint kinematic-morphological analysis are clear strengths that would advance models of bulge growth and AGN fueling if the interpretation holds.

major comments (3)

[§4] §4 (Kinematic modeling): The DysmalPy fits adopt a thin-disk geometry containing only circular rotation and isotropic turbulence. No alternative models that include warps, vertical motions, or residual beam-smearing are presented to test whether they can reproduce the observed 50-100 km/s coherent residuals. The single inclined galaxy that lacks residuals already suggests possible projection or geometric dependence that should be quantified.
[§5.1] §5.1 (Non-circular motions): The statement that velocity residuals 'spatially coincide with non-axisymmetric structures—spiral arms and bars—demonstrating a direct link' rests on visual comparison. No quantitative measure of spatial overlap, correlation, or statistical significance is reported, weakening the causal claim between morphology and gas transport.
[§5.2] §5.2 (Inflow rates): The conversion of residual velocities into net inflow rates (Ṁ ~ -50 M⊙ yr⁻¹) assumes a specific deprojection, gas surface-density distribution, and radial integration range. The manuscript does not detail how these quantities are derived, how beam-smearing affects the residuals, or how uncertainties are propagated, making it difficult to assess whether the rates are robustly comparable to the SFR.

minor comments (2)

[Figures 3-4] Figure 3 and 4: Overplotting JWST morphological contours on the residual velocity maps would make the claimed spatial alignment more transparent to the reader.
[Table 2] Table 2: The reported median values for Vc/σ0 and σ0 should include the full sample statistics and any inclination-dependent trends to allow direct comparison with the text.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and positive report on our manuscript. Their comments have identified areas where we can strengthen the presentation and robustness of our analysis. We address each major comment point-by-point below and have revised the manuscript accordingly.

read point-by-point responses

Referee: [§4] §4 (Kinematic modeling): The DysmalPy fits adopt a thin-disk geometry containing only circular rotation and isotropic turbulence. No alternative models that include warps, vertical motions, or residual beam-smearing are presented to test whether they can reproduce the observed 50-100 km/s coherent residuals. The single inclined galaxy that lacks residuals already suggests possible projection or geometric dependence that should be quantified.

Authors: We thank the referee for this important suggestion. The thin-disk model with isotropic turbulence is well-motivated by the observed high Vc/σ0 ratios (median ~8.6), which indicate dynamically cold disks, and DysmalPy explicitly forward-models beam-smearing. Nevertheless, we agree that explicit tests of alternatives would increase confidence in the residuals. In the revised manuscript we will add a new subsection in §4 presenting results from models that include mild warps and vertical motions; these show that such geometries do not reproduce the observed coherent 50-100 km/s residuals as effectively as the in-plane radial-flow interpretation. For the single more inclined galaxy lacking residuals, we interpret this as a projection effect (in-plane flows become harder to detect at higher inclinations) and will quantify this expectation using mock observations in the revision. revision: yes
Referee: [§5.1] §5.1 (Non-circular motions): The statement that velocity residuals 'spatially coincide with non-axisymmetric structures—spiral arms and bars—demonstrating a direct link' rests on visual comparison. No quantitative measure of spatial overlap, correlation, or statistical significance is reported, weakening the causal claim between morphology and gas transport.

Authors: We acknowledge that the current link relies on visual alignment. To address this, the revised manuscript will include a quantitative analysis of the spatial correspondence between the velocity-residual maps and the non-axisymmetric morphological features extracted from the JWST imaging. We will compute overlap fractions and Pearson correlation coefficients between the residual velocity fields and masks of spiral arms and bars, together with statistical significance assessed via Monte-Carlo randomization of the residual maps. revision: yes
Referee: [§5.2] §5.2 (Inflow rates): The conversion of residual velocities into net inflow rates (Ṁ ~ -50 M⊙ yr⁻¹) assumes a specific deprojection, gas surface-density distribution, and radial integration range. The manuscript does not detail how these quantities are derived, how beam-smearing affects the residuals, or how uncertainties are propagated, making it difficult to assess whether the rates are robustly comparable to the SFR.

Authors: We agree that additional methodological detail is needed. In the revised §5.2 we will expand the description of the inflow-rate calculation to include: (i) the exact deprojection formula applied to the residual velocities, (ii) the adopted molecular-gas surface-density profiles derived from the NOEMA CO maps, (iii) the radial integration limits used, and (iv) the full uncertainty budget that propagates errors from velocity residuals, density, inclination, and distance. We will also explicitly discuss the residual impact of beam-smearing (already mitigated by the DysmalPy forward modeling) and present sensitivity tests varying the integration range and density assumptions. revision: yes

Circularity Check

0 steps flagged

Minor self-citation in modeling tool but derivation self-contained from new observations

full rationale

The paper applies DysmalPy to fit axisymmetric rotation to new high-resolution NOEMA CO data, then interprets residuals as radial flows via spatial coincidence with JWST morphology and computes inflow rates as an inference step. No step reduces by construction to its inputs, no fitted parameter is relabeled as prediction, and no load-bearing uniqueness theorem or ansatz is imported solely via self-citation. The central morphology-transport link and ~50 M⊙/yr inflow claim rest on independent data and standard decomposition rather than definitional equivalence, consistent with a low circularity score.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard galactic-kinematics assumptions and the interpretation of residuals; no new entities are postulated and no free parameters are introduced beyond those internal to the DysmalPy fit.

free parameters (1)

DysmalPy model parameters (inclination, position angle, turbulence)
Fitted to match the observed velocity field before residual extraction.

axioms (1)

domain assumption The molecular gas distribution can be described by an axisymmetric rotating disk with moderate intrinsic turbulence that DysmalPy can forward-model accurately.
Invoked when subtracting the rotation model to isolate non-circular residuals.

pith-pipeline@v0.9.0 · 5877 in / 1516 out tokens · 61519 ms · 2026-05-10T04:25:12.499131+00:00 · methodology

discussion (0)

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas
astro-ph.GA 2026-05 unverdicted novelty 7.0

A large DESI sample reveals thousands of infalling cold gas absorbers at low redshift, with velocity distributions indicating multiple accretion pathways including radial inflows and satellite accretion.
NOEMA3D: Spatially resolved dust, CO, and [C I] in massive star-forming main sequence galaxies at cosmic noon
astro-ph.GA 2026-04 unverdicted novelty 5.0

Spatially resolved NOEMA observations reveal extended molecular gas disks in main-sequence galaxies at z=1.1-1.6, supporting steady accretion via spirals or bars instead of merger-driven starbursts.

Reference graph

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