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arxiv: 2606.02688 · v1 · pith:3RWM67GNnew · submitted 2026-06-01 · 🌌 astro-ph.GA

NOEMA^rm{3D}: A deep view of cold gas flows in a barred spiral galaxy at zsim1

Stavros Pastras , Reinhard Genzel , Linda J. Tacconi , Thorsten Naab , Natascha M. F\"orster Schreiber , Karl Schuster , Roberto Neri , Jianhang Chen
show 30 more authors
Giulia Tozzi Jean-Baptiste Jolly Letizia Scaloni Capucine Barfety Andreas Burkert Yixian Cao Fran\c{c}oise Combes Ric Davies Frank Eisenhauer Juan M. Espejo Salcedo Simon Flesch Santiago Garc\'ia-Burillo Rodrigo Herrera-Camus Lilian L. Lee Minju M. Lee Daizhong Liu Dieter Lutz Giovanni Mazzolari Amit Nestor Shachar Meghana Pannikkote Eleonora Parlanti Panos A. Patsis Sedona H. Price Claudia Pulsoni Alvio Renzini Taro T. Shimizu Amiel Sternberg Eckhard Sturm Stijn Wuyts Hannah \"Ubler
This is my paper

Pith reviewed 2026-06-28 13:38 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords barred spiral galaxymolecular gas inflowshigh-redshift galaxycosmic noonNOEMA observationsstar formation rategalaxy evolutiondust lane shock
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The pith

A bar in a z=1.12 spiral galaxy drives molecular gas inflows at 30 solar masses per year, matching the galaxy's star formation rate.

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

Deep NOEMA CO(4-3) observations combined with JWST and HST imaging reveal a massive, gas-rich barred spiral at redshift 1.12 with a long, strong, fast bar. The bar produces net molecular gas inflows of about 30 solar masses per year, estimated independently three ways and comparable to the galaxy's integrated star formation rate of 36 solar masses per year. Evidence includes gas motions parallel to a dust lane shock on one side of the bar. This provides a quantitative picture of bar-driven flows in a main-sequence galaxy during cosmic noon.

Core claim

This target is a massive baryon-dominated gas-rich disk hosting a long strong fast bar that rotates at 50 km/s/kpc and drives molecular gas inflows with net rate ~30 M⊙/yr based on three estimates, equal to the SFR of ~36 M⊙/yr, with a well-defined dust lane shock and parallel gas motions confirming bar-driven flow.

What carries the argument

The bar with length 4.2 kpc, strength Qb=0.37, and corotation radius ratio R=1.05, which produces the observed net radial molecular gas inflows and dust lane shock.

If this is right

  • Bars can supply gas to maintain star formation rates in massive main-sequence galaxies at cosmic noon.
  • Bar-driven inflows of this magnitude may contribute to central mass buildup and bulge growth over time.
  • A non-negligible fraction of z~1 galaxies may experience similar bar-driven evolution.
  • The low dark matter fraction inside the effective radius indicates the disk is self-gravitating and bar-unstable.

Where Pith is reading between the lines

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

  • If bars are common at this epoch, they could help explain the high gas fractions observed in cosmic noon disks without invoking external accretion alone.
  • Detailed kinematic modeling of more high-z barred galaxies would test whether inflow rates systematically match SFRs.
  • Comparison with hydrodynamic simulations could reveal how bar pattern speeds and strengths evolve to produce such inflows.

Load-bearing premise

The three inflow rate estimates capture true net radial motion driven by the bar rather than other dynamics or artifacts, and the dust lane is a bar-induced shock.

What would settle it

Higher-resolution kinematic maps showing inflow rates inconsistent across the three methods or gas velocities perpendicular to the dust lane instead of parallel.

Figures

Figures reproduced from arXiv: 2606.02688 by Alvio Renzini, Amiel Sternberg, Amit Nestor Shachar, Andreas Burkert, Capucine Barfety, Claudia Pulsoni, Daizhong Liu, Dieter Lutz, Eckhard Sturm, Eleonora Parlanti, Fran\c{c}oise Combes, Frank Eisenhauer, Giovanni Mazzolari, Giulia Tozzi, Hannah \"Ubler, Jean-Baptiste Jolly, Jianhang Chen, Juan M. Espejo Salcedo, Karl Schuster, Letizia Scaloni, Lilian L. Lee, Linda J. Tacconi, Meghana Pannikkote, Minju M. Lee, Natascha M. F\"orster Schreiber, Panos A. Patsis, Reinhard Genzel, Ric Davies, Roberto Neri, Rodrigo Herrera-Camus, Santiago Garc\'ia-Burillo, Sedona H. Price, Simon Flesch, Stavros Pastras, Stijn Wuyts, Taro T. Shimizu, Thorsten Naab, Yixian Cao.

Figure 1
Figure 1. Figure 1: Imaging overview of G4_38232: color composite images of the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Overview of the elliptical isophote fitting of the NIR [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Velocity (top) and velocity dispersion (bottom) for the [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: CO(4-3) flux maps (top), as well as velocity (bottom [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Estimate of the deprojected baryonic surface density (left), gravitational potential at the disk midplane (middle left), non [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Mode amplitudes from the Fourier decomposition of the [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Expected rotation curve of G4_38232 based on the es [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Overview of the application of the (Tremaine & Weinberg 1984) method: the slits overlaid on the CO(4-3) flux (left) and [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: Gas surface density maps of the isothermal responses to the estimated potential in the midplane of G4_38232 for pattern speeds 20 [PITH_FULL_IMAGE:figures/full_fig_p011_11.png] view at source ↗
Figure 11
Figure 11. Figure 11: Given the optical restframe wavelengths (tracing young [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Observed residual LOS velocity (top) and inferred in [PITH_FULL_IMAGE:figures/full_fig_p013_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Radial gas flow rates based on the inferred in-plane ra [PITH_FULL_IMAGE:figures/full_fig_p014_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Angular momentum loss efficiency (top) and mass in￾flow rate (bottom) profiles for the tapered and naturally-weighted data. We find that gas loses angular momentum in the bar region, with a maximum angular momentum loss efficiency near the end of the bar, enabling the efficient gas transport toward the center, as indicated by the increasingly negative values of the mass flow rate. Beyond the bar region th… view at source ↗
Figure 15
Figure 15. Figure 15: Color composite image in the short-wavelength [PITH_FULL_IMAGE:figures/full_fig_p017_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: In-plane velocity parallel to the northern dust lane and [PITH_FULL_IMAGE:figures/full_fig_p018_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Overview of inferred gas flow patterns in the disk of G4_38232 (left) and resulting gas flow rate profiles (right) determined [PITH_FULL_IMAGE:figures/full_fig_p019_17.png] view at source ↗
read the original abstract

We present a deep, high-resolution CO(4-3) IRAM-NOEMA observation of a main sequence, barred, spiral galaxy at $z\approx1.12$, with an on-source integration time of $\approx37$ hours and a beam FWHM of $\approx0.\!\!^{\prime\prime}3$. We use the molecular gas data in conjunction with the available deep multi-band JWST and HST imaging, covering restframe UV to near-IR wavelengths, to quantitatively study the gas flows in the disk plane of this cosmic noon barred spiral. We find that this target is a massive ($\log(M_{\rm{baryons}}/M_\odot)\approx10.96$), baryon-dominated ($f_{\rm{dm}}(<R_e)=u^2_{\rm{circ,dm}}(R_e)/u^2_{\rm{circ}}(R_e)\sim4\%$), gas-rich ($f_{\rm{gas}}=M_{\rm{gas}}/(M_{\rm{\star}}+M_{\rm{gas}})\approx40\%$) disk, hosting a long ($a_{\rm{bar}}\approx4.2$ kpc), strong ($Q_{\rm{b}}\approx0.37$), and fast ($\mathcal{R}=R_{\rm{CR}}/a_{\rm{bar}}\approx1.05$) bar, which rotates at an angular speed of $\Omega_{\rm{pattern}}\approx$ 50 km/s/kpc. This bar is driving molecular gas inflows with a net inflow rate of $\dot{M}\sim30$ $M_\odot$/yr, based on three estimates, which is of the same order as the galaxy-integrated star formation rate ($\rm{SFR}\approx36$ $M_\odot$/yr). We additionally identify evidence of a well-defined dust lane shock at the northwestern side of the bar, with gas motions parallel to this feature, in agreement with expectations for an established bar-driven flow. Our study highlights the possible role of bars as key drivers of galaxy evolution for a significant fraction of cosmic noon galaxies, offering a detailed picture of well-defined, bar-driven inflows in a high-$z$ barred spiral.

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 presents deep IRAM-NOEMA CO(4-3) observations (37 hours on-source, 0.3″ beam) of a main-sequence barred spiral at z≈1.12, combined with JWST/HST imaging. It characterizes the galaxy as massive (log M_baryons≈10.96), gas-rich (f_gas≈40%), baryon-dominated, and hosting a long (a_bar≈4.2 kpc), strong (Q_b≈0.37), fast (R≈1.05) bar rotating at Ω_pattern≈50 km s⁻¹ kpc⁻¹. The central claim is that this bar drives net molecular gas inflows of ˙M∼30 M⊙ yr⁻¹ (from three estimates), comparable to the integrated SFR≈36 M⊙ yr⁻¹, with supporting evidence of a northwestern dust-lane shock and parallel gas motions.

Significance. If the inflow measurements hold, the work supplies one of the first resolved kinematic views of bar-driven radial flows at cosmic noon, directly linking bar properties to gas transport rates on the order of the SFR and thereby strengthening the case that bars can be important drivers of evolution for a non-negligible fraction of z∼1 disks.

major comments (2)
  1. [Abstract and inflow-rate derivation section] The three inflow-rate estimates are presented as converging on ∼30 M⊙ yr⁻¹, yet the manuscript supplies neither formal error budgets nor an explicit demonstration that the estimates remain independent of the adopted rotation-curve decomposition and are free of beam-smearing bias at the stated 2.5 kpc resolution (0.3″ beam versus a_bar=4.2 kpc).
  2. [Kinematic analysis and dust-lane discussion] At the achieved spatial resolution the data only marginally resolve the bar; the attribution of the measured non-circular velocities to net bar-driven radial inflow (rather than projection, streaming, or residual rotation-curve mismatch) therefore rests on an assumption whose robustness is not quantified by any test shown in the text.
minor comments (2)
  1. The data-reduction steps for the NOEMA visibilities (flagging, weighting, CLEAN parameters) are not described at a level that would allow independent reproduction.
  2. Notation for the bar strength parameter Q_b and the corotation radius ratio R should be defined at first use and cross-referenced to the equations used to compute them.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review. The comments highlight important areas where the manuscript can be strengthened with additional quantitative analysis. We address each major comment below and will incorporate the suggested improvements in a revised version.

read point-by-point responses

  1. Referee: [Abstract and inflow-rate derivation section] The three inflow-rate estimates are presented as converging on ∼30 M⊙ yr⁻¹, yet the manuscript supplies neither formal error budgets nor an explicit demonstration that the estimates remain independent of the adopted rotation-curve decomposition and are free of beam-smearing bias at the stated 2.5 kpc resolution (0.3″ beam versus a_bar=4.2 kpc).

    Authors: We acknowledge that the original manuscript did not include formal error budgets or explicit tests demonstrating independence from the rotation-curve decomposition and robustness against beam-smearing. In the revised version we will add a new subsection that (i) propagates uncertainties from the rotation-curve fit, inclination, and distance into each of the three inflow-rate methods, (ii) repeats the calculations after perturbing the decomposition parameters within their 1σ ranges to show consistency, and (iii) presents beam-smearing tests using both analytic corrections and mock data cubes convolved to the observed resolution. These additions will quantify the robustness of the ∼30 M⊙ yr⁻¹ result. revision: yes

  2. Referee: [Kinematic analysis and dust-lane discussion] At the achieved spatial resolution the data only marginally resolve the bar; the attribution of the measured non-circular velocities to net bar-driven radial inflow (rather than projection, streaming, or residual rotation-curve mismatch) therefore rests on an assumption whose robustness is not quantified by any test shown in the text.

    Authors: We agree that the bar (a_bar≈4.2 kpc) is only marginally resolved at the 0.3″ beam and that the manuscript lacked quantitative tests isolating the radial-inflow component from projection, streaming, or decomposition residuals. The revised manuscript will include Monte Carlo realizations of the velocity field under varied potential decompositions and projection angles, together with a direct comparison to hydrodynamic simulations of barred galaxies observed at comparable resolution. These tests will provide a statistical assessment of the inflow attribution. The morphological alignment with the northwestern dust-lane shock will be incorporated as an additional, independent constraint. revision: yes

Circularity Check

0 steps flagged

No significant circularity; inflow estimates derived directly from observations

full rationale

The paper presents an observational analysis of CO(4-3) data and multi-band imaging to measure bar properties (length, strength, pattern speed) and estimate net molecular gas inflow rates via three independent methods based on observed velocities and morphologies. No load-bearing step reduces to a fitted parameter being renamed as a prediction, a self-citation chain, or an ansatz smuggled via prior work. All quantities (e.g., Ω_pattern ≈ 50 km/s/kpc, Ṁ ∼ 30 M⊙/yr) are computed from the current dataset without circular reuse. The central claim remains an empirical measurement rather than a constructed identity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The work rests on standard assumptions of galactic dynamics and observational astronomy rather than new free parameters or invented entities.

axioms (1)
  • domain assumption Standard galactic dynamics relations for bar pattern speed, corotation radius, and inflow rate estimation from velocity fields hold at z≈1.
    Invoked to classify the bar as fast (R≈1.05) and to convert observed motions into net inflow rate.

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discussion (0)

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Forward citations

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