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arxiv: 2606.11444 · v1 · pith:L3IFKCDQnew · submitted 2026-06-09 · 🌌 astro-ph.GA

Investigating the role of turbulence in the interstellar medium in zsim3 dusty star-forming galaxies using kpc-resolution ALMA dust and gas maps

B. A. Westoby , J. A. Hodge , P. Sharda , P. E. Mancera Pi\~na , M. Rybak , E. da Cunha , J. Li , I. Smail
show 23 more authors
A. M. Swinbank A. Battisti L. A. Boogaard W. N. Brandt G. Calistro Rivera C.-C. Chen P. Cox M. Cracraft H. Dannerbauer R. Decarli T. R. Greve S. Kendrew K. Knudsen C.-L. Liao J. van Marrewijk O. Nayak M. Neeleman L. E. Rowland E. Schinnerer F. Walter J. L. Wardlow A. Weiss P. van der Werf
This is my paper

Pith reviewed 2026-06-27 12:07 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dusty star-forming galaxiesALMA observationsmolecular gasstar formation relationsturbulencehigh-redshift galaxiesinterstellar mediumkinematics
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The pith

High-resolution ALMA maps of z~3 galaxies show their star formation matches models that include turbulence but not those that omit it.

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

The paper maps molecular gas and dust emission at roughly 2 kiloparsec scales in three distant dusty star-forming galaxies. It finds that the gas follows the dust structures but extends farther out, matching the scale of the stellar light. Kinematic modeling fits the galaxies as rotating discs with mostly ordered motions. When the authors compare local star formation rates to gas densities, the measurements sit away from standard theoretical predictions yet line up with models that build in turbulence. This points to turbulence as a key regulator of star formation in these early systems.

Core claim

Utilizing the high-resolution 870 micron dust continuum and CO data, the galaxies' kpc-scale star-formation scaling relations are found to be offset from theoretical predictions that do not take turbulence into account, but consistent with gravo-turbulent models, suggesting turbulence plays a central role in regulating star formation at high redshift.

What carries the argument

Comparison of observed kpc-scale star-formation scaling relations against theoretical predictions that either include or exclude turbulence.

If this is right

  • The molecular gas distribution is significantly more extended than the dust emission and comparable in size to the stellar emission.
  • The two galaxies at the same redshift are consistent with interacting systems.
  • Kinematic fits indicate rotating discs with ordered-to-random motion ratios of 5 to 6.
  • Theoretical star-formation models must incorporate turbulence to reproduce the observed relations at these redshifts.

Where Pith is reading between the lines

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

  • Similar maps at lower redshifts could test whether turbulence's role weakens as galaxies settle into more stable configurations.
  • Cosmological simulations that currently under-predict turbulent support might need revised sub-grid prescriptions to match high-redshift observations.
  • If the turbulence interpretation holds, the efficiency of star formation on kiloparsec scales would depend on local velocity dispersion rather than gas density alone.

Load-bearing premise

The analysis assumes a constant CO-to-H2 conversion factor and excitation ratio across the observed regions.

What would settle it

A measurement showing that the CO-to-H2 conversion factor varies by more than a factor of two between different regions within the same galaxy would remove the reported offset from non-turbulent models.

Figures

Figures reproduced from arXiv: 2606.11444 by A. battisti, A. M. Swinbank, A. Weiss, B. A. Westoby, C.-C. Chen, C.-L. Liao, E. da Cunha, E. Schinnerer, F. Walter, G. Calistro Rivera, H. Dannerbauer, I. Smail, J. A. Hodge, J. Li, J. L. Wardlow, J. van Marrewijk, K. Knudsen, L. A. Boogaard, L. E. Rowland, M. Cracraft, M. Neeleman, M. Rybak, O. Nayak, P. Cox, P. E. Mancera Pi\~na, P. Sharda, P. van der Werf, R. Decarli, S. Kendrew, T. R. Greve, W. N. Brandt.

Figure 1
Figure 1. Figure 1: CO spectra and curve-of-growth analysis showing flux as a function of aperture radius. The left hand panels show the single Gaussian fits to the spectra, we also show a dashed double Gaussian for ALESS3.1 and ALESS9.1. The dotted vertical black lines in the right-hand panels are the apertures used to extract the spectra, the dashed horizontal black lines are the final fluxes extracted from the zeroth momen… view at source ↗
Figure 2
Figure 2. Figure 2: Naturally weighted 2 ′′ × 2 ′′ zeroth moment maps of the CO line emission (1st column) alongside dust continuum maps (Hodge et al. 2019) (2nd column) and NIRCam RGB(F444W/F356W/F200W) images (Hodge et al. 2025) (3rd column), centered on the positions in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Flux density profiles of CO line emission, dust continuum (Hodge et al. 2019) and stellar continuum traced by NIRCam filters (Hodge et al. 2025). Dashed lines correspond to effective radii, Re. Dotted lines correspond to the CO PSF. CO(1–0). The difference we see between the extents of the molecular gas and 870µm dust continuum is potentially due to gradients in the dust temperature and optical depth withi… view at source ↗
Figure 4
Figure 4. Figure 4: Kinematic modelling for ALESS3.1 (upper) and ALESS9.1 (lower): (Left) Moment 0, 1 and 2 maps with 50 km s−1 velocity contours, model and beam ellipses (Right) position-velocity (PV) diagrams of the minor and major axes with minimum contours at 2σrms, increasing in steps of 2σrms. The best-fit kinematic model is shown with red contours and the data are shown with positive blue contours and negative grey con… view at source ↗
Figure 5
Figure 5. Figure 5: Star formation relation comparison showing annular regions for ALESS3.1 (circle) and ALESS9.1 (square) along with both resolved and unresolved literature values from SFGs and SMGs. Also plotted are the Kennicutt (1998), De Los Reyes & Kennicutt (2019), Pessa et al. (2021), Wang et al. (2022) relations (general Kennicutt-Schmidt relation, left panel), Krumholz et al. (2012) relation (incorporating free-fall… view at source ↗
read the original abstract

We present ALMA high-resolution ($\sim$0.25$^{\prime\prime}$/2 kpc) CO(5-4) and CO(4-3) observations of three $z\sim 3$ submillimetre-selected dusty galaxies from the ALESS survey. These data complement existing [sub]-kpc scale ALMA 870$\mu$m continuum imaging and JWST NIRCam and MIRI imaging from the ALESS-JWST program, allowing us to trace the molecular gas, dust-obscured star formation, and stellar populations on similar spatial scales. We spectroscopically confirm that two of the sources lie at the same redshift and are likely interacting. We find that the molecular-gas distribution broadly follows the dusty star-forming structures seen in the 870$\mu$m dust continuum imaging, but that the gas reservoirs are significantly more extended than the dust emission with a spatial extent comparable to the rest-frame near-infrared stellar emission. By modeling the kinematics for the two highest signal-to-noise sources, we find that the galaxies are well-fit by rotating disc models with high ratios of ordered to random motion ($V_{\rm{max}}/\overline{\sigma}=5\pm1$ and $6\pm1$), although smaller-scale kinematic deviations cannot be ruled out at the current sensitivity and spatial resolution. Finally, utilizing the high-resolution 870$\mu$m dust continuum and CO data, we investigate star-formation scaling relations on kpc-scales in these high-redshift galaxies. Assuming a constant CO-to-H$_{2}$ conversion factor and excitation ratio, we find that the data are offset from theoretical star-formation relation predictions that do not take turbulence into account, but consistent with gravo-turbulent models, thereby suggesting that turbulence plays a central role in regulating star formation at high redshift.

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

1 major / 0 minor

Summary. The manuscript presents ALMA high-resolution (~0.25 arcsec / 2 kpc) CO(5-4) and CO(4-3) observations of three z~3 submillimetre-selected dusty galaxies from the ALESS survey, combined with existing 870 μm continuum and JWST NIRCam/MIRI imaging. It maps the molecular gas distribution (more extended than dust but comparable to stellar emission), spectroscopically confirms an interacting pair, models the kinematics of the two highest-S/N sources as rotating disks with V_max/σ ≈ 5–6, and examines kpc-scale star-formation scaling relations. Under the assumption of constant CO-to-H2 conversion factor and excitation ratio, the data points are reported as offset from non-turbulent theoretical predictions but consistent with gravo-turbulent models, implying turbulence regulates star formation at high redshift.

Significance. If the constant-conversion-factor assumption holds and the model comparison is robust, the resolved multi-tracer maps and kinematic results would provide valuable constraints on the physical conditions in high-z DSFGs and observational support for turbulence-regulated star formation on kpc scales, complementing lower-resolution studies.

major comments (1)
  1. [Abstract and star-formation scaling relations section] Abstract and star-formation scaling relations section: the central claim that the kpc-scale points support gravo-turbulent regulation (offset from non-turbulent predictions) rests entirely on the assumption of spatially and source-invariant α_CO and r_54. No quantitative offsets, error bars on the model comparison, or tests of alternative conversion-factor values (e.g., varying with density or turbulence) are provided; if these parameters shift systematically, the data could move onto the non-turbulent locus, undermining the turbulence conclusion.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address the single major comment below and indicate the revisions we will incorporate.

read point-by-point responses

  1. Referee: [Abstract and star-formation scaling relations section] Abstract and star-formation scaling relations section: the central claim that the kpc-scale points support gravo-turbulent regulation (offset from non-turbulent predictions) rests entirely on the assumption of spatially and source-invariant α_CO and r_54. No quantitative offsets, error bars on the model comparison, or tests of alternative conversion-factor values (e.g., varying with density or turbulence) are provided; if these parameters shift systematically, the data could move onto the non-turbulent locus, undermining the turbulence conclusion.

    Authors: We agree that the interpretation depends on the stated assumption of constant α_CO and r_54, which is explicitly noted in the abstract and scaling-relations section. In the revised manuscript we will add quantitative offsets between the observed kpc-scale points and the non-turbulent model locus, together with error bars that incorporate the reported uncertainties on the data. We will also expand the discussion to examine how plausible systematic variations in α_CO (e.g., with density or turbulence) could shift the points, while noting that the present data remain consistent with gravo-turbulent predictions under the standard conversion factors adopted in the high-redshift DSFG literature. Comprehensive spatially resolved tests of variable conversion factors lie beyond the sensitivity and tracer coverage of the current observations. revision: partial

Circularity Check

0 steps flagged

No significant circularity; comparison to external models is independent

full rationale

The paper's central claim rests on placing observed kpc-scale gas and SFR surface densities (derived from CO luminosities under a stated constant α_CO and excitation ratio) onto star-formation relation diagrams and noting their offset from non-turbulent theoretical tracks while matching gravo-turbulent ones. This comparison uses external models as benchmarks rather than deriving the models or the offset from the paper's own fitted quantities or self-citations. No self-definitional equations, fitted-input-as-prediction reductions, or load-bearing self-citation chains appear in the provided derivation chain; the result remains falsifiable against independent theory and is therefore self-contained.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The claim depends on two constant scaling factors treated as fixed and on the applicability of rotating-disk kinematic models and standard star-formation relations to these high-redshift systems.

free parameters (2)
  • CO-to-H2 conversion factor
    Assumed constant; no value or variation discussed in abstract
  • excitation ratio
    Assumed constant for the CO(5-4) and CO(4-3) lines
axioms (2)
  • domain assumption Rotating disc models adequately describe the gas kinematics
    Invoked for the two highest S/N sources
  • standard math The ~0.25 arcsec resolution corresponds to ~2 kpc physical scales at z~3
    Used to claim kpc-resolution analysis

pith-pipeline@v0.9.1-grok · 6052 in / 1406 out tokens · 38060 ms · 2026-06-27T12:07:11.505194+00:00 · methodology

discussion (0)

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Reference graph

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