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arxiv: 2604.19543 · v1 · submitted 2026-04-21 · 🌌 astro-ph.GA

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Dynamically cold discs in high-redshift galaxies: comparison between ALMA observations and TNG50

Filippo Fraternali, Hang Yang, Qi Guo, Shihong Liao, Yi He

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Pith reviewed 2026-05-10 02:12 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords high-redshift galaxiesgalaxy kinematicshydrodynamical simulationsTNG50ALMA observationsgas accretiondynamical cold discsvelocity dispersion
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The pith

TNG50 shows that aligned gas accretion can produce rare dynamically cold discs at z=3-5, while most galaxies remain hotter due to misaligned infall.

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

The paper constructs mock ALMA [CII] datacubes from the TNG50 simulation to measure gas kinematics in massive star-forming galaxies at redshifts 3 to 5. Most simulated systems show V/σ ratios of only 2-3, indicating dynamically hot discs unlike many real observations, but a minority reach V/σ >5. These colder discs, when selected at z=4, stay relatively cold through the redshift range and form when incoming gas carries angular momentum aligned with the existing disc. A single extreme case reaches V/σ ≳10 but lasts no longer than 200 Myr. The cold subset also exhibits lower accretion rates and better alignment between stellar and dark-matter angular momenta, with one-third evolving into massive discs and two-thirds into early-type galaxies by the present day.

Core claim

Dynamically cold disc formation in TNG50 is promoted by gas accretion with angular momentum aligned with the pre-existing disc, while most galaxies undergo misaligned accretion; such cold discs selected at z=4 remain dynamically colder than most of the TNG population across z=3-5, and a galaxy with V/σ ≳10 appears in a transient phase that lasts ≤200 Myr.

What carries the argument

The V/σ ratio of gas rotation velocity to velocity dispersion, extracted from mock emission-line datacubes that replicate ALMA [CII] observational methods and resolution effects.

If this is right

  • Cold discs selected at z=4 stay dynamically colder than the average TNG50 population across the entire z=3-5 interval.
  • The most extreme cold disc with V/σ ≳10 exists only transiently for no more than 200 Myr.
  • Cold discs display lower mass accretion rates and more aligned stellar and dark-matter angular momentum vectors than the general population.
  • By z=0, one-third of the cold high-redshift discs become massive disc galaxies while two-thirds become early-type galaxies.

Where Pith is reading between the lines

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

  • If the alignment requirement is physically realistic, then the frequency of cold discs in real high-redshift galaxies may trace the prevalence of coherent gas inflows rather than merger rates alone.
  • The short lifetime of the highest-V/σ phase suggests that very cold discs should be rare in any snapshot survey and may be caught only during brief windows of aligned accretion.
  • The split evolution toward both disc and early-type galaxies by z=0 implies that high-redshift cold discs do not exclusively seed today's spiral galaxies.

Load-bearing premise

The mock emission line datacubes constructed from TNG50 accurately reproduce the observational effects, resolution, and analysis methods applied to real ALMA [CII] observations, including any beam smearing or noise that affects the measured V/σ ratios.

What would settle it

Direct ALMA observations that measure a substantially higher fraction of galaxies with V/σ >5 at z=4 than appears in the TNG50 sample, or that show no preference for aligned accretion in the coldest systems.

Figures

Figures reproduced from arXiv: 2604.19543 by Filippo Fraternali, Hang Yang, Qi Guo, Shihong Liao, Yi He.

Figure 1
Figure 1. Figure 1: Gas surface densities of neutral hydrogen in three simulated galaxies at 𝑧 = 4.43, from TNG50. This figure is rendered using the Py-SPHViewer code (Benitez-Llambay 2015). The leftmost panel shows a cold disc with high 𝑉/𝜎, while the middle and right panels show two chaotic galaxies, with a 𝑉/𝜎 close to the average value in TNG50 massive galaxies at this redshift. The upper and lower panels show the face-on… view at source ↗
Figure 2
Figure 2. Figure 2: Intensity map, velocity field and position-velocity slices (along the major, 𝜙 = 90◦ , and minor, 𝜙 = 180◦ , axes), extracted from our neutral hydrogen mock observations for the three selected TNG50 galaxies presented in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of 𝑉/𝜎 values of dynamically cold discs in TNG50 obtained either directly from the simulations (x-axis) or from the mock dat￾acubes (y-axis). Each point represents one simulated galaxy, coloured by its asymmetry (𝐴) value. Horizontal and vertical error bars indicate simula￾tion and mock uncertainties, respectively. The solid green line marks the 1:1 relation and the dashed line the 1-sigma scatt… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of the asymmetry parameter 𝐴 for simulated cold disc galaxies, all star-forming simulated galaxies, and observed galaxies from Roman-Oliveira et al. (2023). Galaxies with 𝐴 < 0.35 are classified as symmetric. to 1. For all simulated galaxies, the asymmetry parameter is widely distributed, from 0.1 to 0.7. The dynamically cold discs exhibit values ranging from 0.15 to 0.6, and a peak between 0.… view at source ↗
Figure 6
Figure 6. Figure 6: Evolution of gas properties of simulated galaxies selected as cold discs at 𝑧 = 4 (coloured solid lines for single galaxies, deep blue dashed lines show the median value, deep blue shaded region for 16th to 84th percentiles) compared to the general TNG50 population of star-forming galaxies at 𝑧 = 4 (light blue dashed line for median, light blue shaded region for 16th to 84th percentiles). By gas, we always… view at source ↗
Figure 7
Figure 7. Figure 7: Evolution of stellar properties of simulated galaxies selected as dynamically cold discs at 𝑧 = 4 (coloured solid lines for single galaxies, deep blue dashed lines show the median value, deep blue shaded region for 16th to 84th percentiles) compared to the general TNG50 population of star-forming galaxies at 𝑧 = 4 (light blue dashed line for median, light blue shaded region for 16th to 84th percentiles). T… view at source ↗
Figure 8
Figure 8. Figure 8: Evolution of the angle between the spin direction of the gas in the galaxies and two reference axes of host dark matter subhalos and halos. Markers are the same as in [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Redshift evolution of 𝑉/𝜎 in this work, compared with results from other studies. The blue line and shaded region represent the median and 16th-84th percentiles of our sample. The blue crosses are cold discs. The yellow line corresponds to the median value for H𝛼 in the TNG50 simulations from Pillepich et al. (2019). The pink and green lines represent H𝛼 and [CII] data from Serra simulations (Kohandel et a… view at source ↗
Figure 10
Figure 10. Figure 10: Stellar component in three simulated galaxies presented in [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Normalized star formation rate distribution of all TNG galaxies in our samples, galaxies with cold discs and observed galaxies from Rizzo et al. 2020, 2021; Roman-Oliveira et al. 2023. clearly overlap with the most massive local ETGs (slow rotators) in the circular speed-baryonic mass plane, indicating that these high-𝑧 galaxies are nearly fully formed ETGs, except for their rapid rotation, which requires… view at source ↗
read the original abstract

Observations of highly rotationally supported gas discs in high redshift ($z$ > 3) star-forming galaxies challenge our understanding of galaxy formation, as the prevailing view holds that galaxies in the early universe are dynamically hot due to frequent mergers, gas accretion, and strong stellar feedback. We examined the kinematic properties of massive ($M_{\star} \geq 10^{10}\,M_{\odot}$) star-forming galaxies in the TNG50 cosmological hydrodynamical simulation in the redshift range $3\leq z \leq 5$. Mock emission line datacubes were constructed and analysed using the same methodology as for [CII] observations with ALMA. We measured the ratio of the gas rotation velocity ($V$) to velocity dispersion ($\sigma$) finding that most galaxies have $V/\sigma\sim$ $2-3$, lower than observed. However, a few simulated galaxies show $V/\sigma$ > 5. Such "cold" discs, selected at $z=4$, remain dynamically colder than most of the TNG population across $z=3-5$. A galaxy with $V/\sigma\gtrsim10$ appears in a transient phase that lasts $\leq200$ Myr. Dynamically cold disc formation in TNG50 is promoted by gas accretion with angular momentum aligned with the pre-existing disc, while most galaxies undergo misaligned accretion. Dynamically cold discs also show lower mass accretion rates and better aligned stellar and dark-matter angular momentum vectors. By tracing their evolution to $z = 0$, we find that one-third become massive disc galaxies and two-thirds become ETGs.

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 compares the gas kinematics of massive (M⋆ ≥ 10¹⁰ M⊙) star-forming galaxies in TNG50 at 3 ≤ z ≤ 5 against ALMA [CII] observations. Mock emission-line datacubes are generated and analysed with the same pipeline used on real data; the authors report that the majority of simulated galaxies have V/σ ∼ 2–3 (lower than observed), while rare cold discs (V/σ > 5) arise from aligned gas accretion, remain dynamically cold across z = 3–5, are transient (≤ 200 Myr), and evolve into a mixture of massive discs and ETGs by z = 0.

Significance. If the forward modelling of TNG50 to ALMA observables is robust, the work supplies a concrete prediction for the rarity and formation channel of dynamically cold high-redshift discs, together with falsifiable evolutionary tracks to z = 0. The identification of aligned accretion as the key driver and the quantification of the transient timescale are valuable additions to galaxy-formation theory.

major comments (2)
  1. [§3] §3 (mock datacube construction): the description of how beam smearing, noise, channelisation and the precise V/σ extraction algorithm are implemented must be expanded and validated against the actual ALMA data properties. Because the central claim of a systematic discrepancy (simulated V/σ lower than observed) rests on the fidelity of this forward model, any mismatch in resolution or noise treatment could alter the reported offset and the inferred rarity of cold discs.
  2. [§4] §4 (results on V/σ distributions): the text does not report the exact sample size, the distribution of measurement uncertainties on V/σ, or the precise definition and aperture used to extract V and σ from the mock cubes. These omissions prevent a quantitative assessment of the statistical significance of the difference with the ALMA sample.
minor comments (2)
  1. [Figures] Figure 2 (or equivalent): the colour scale and contour levels for the V/σ maps should be stated explicitly so that readers can reproduce the visual classification of cold discs.
  2. [Abstract and §2] The abstract and §2 should include the precise numerical sample size and the exact star-formation-rate threshold used to select the TNG50 galaxies.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We agree that the robustness of the forward modeling and the clarity of the reported statistics are central to the strength of our conclusions, and we have revised the manuscript accordingly to address both major comments.

read point-by-point responses

  1. Referee: §3 (mock datacube construction): the description of how beam smearing, noise, channelisation and the precise V/σ extraction algorithm are implemented must be expanded and validated against the actual ALMA data properties. Because the central claim of a systematic discrepancy (simulated V/σ lower than observed) rests on the fidelity of this forward model, any mismatch in resolution or noise treatment could alter the reported offset and the inferred rarity of cold discs.

    Authors: We agree that the description in §3 requires expansion to demonstrate the fidelity of the mock datacubes. In the revised manuscript we will provide a substantially more detailed account of the implementation of beam smearing, noise addition, channelisation, and the precise V/σ extraction algorithm. We will also add a validation subsection that directly compares the mock data properties (resolution, noise characteristics, and channelisation) to those of the ALMA [CII] observations used in the comparison. This will allow readers to assess whether any differences in treatment could affect the reported V/σ offset. revision: yes

  2. Referee: §4 (results on V/σ distributions): the text does not report the exact sample size, the distribution of measurement uncertainties on V/σ, or the precise definition and aperture used to extract V and σ from the mock cubes. These omissions prevent a quantitative assessment of the statistical significance of the difference with the ALMA sample.

    Authors: We acknowledge that these quantitative details were omitted from the original text. In the revised manuscript we will explicitly state the sample size of TNG50 galaxies analysed at each redshift, report the distribution (or median and 16–84 percentile range) of the measurement uncertainties on V/σ, and provide the precise definitions of V and σ together with the aperture (or radial range) used for their extraction from the mock cubes. These additions will enable a direct statistical comparison with the ALMA sample. revision: yes

Circularity Check

0 steps flagged

No circularity: results follow directly from independent simulation analysis and external data comparison

full rationale

The paper extracts kinematic ratios from TNG50 snapshots, constructs mock datacubes using the same pipeline as the external ALMA observations, and compares the resulting V/σ distributions without fitting any parameters to the target data. Accretion alignment, transience, and descendant tracing are performed entirely within the simulation volume using its native particle data. No self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citations appear in the derivation; the mock construction is a forward-modeling step whose fidelity is an assumption but does not create circular equivalence to the inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The work relies on the existing TNG50 cosmological simulation without introducing new fitted parameters or postulated entities; assumptions are inherited from the simulation's subgrid models for gas dynamics, star formation, and feedback.

axioms (1)
  • domain assumption The TNG50 hydrodynamical simulation and its subgrid physics prescriptions accurately capture the kinematic evolution of gas discs in massive star-forming galaxies at 3 ≤ z ≤ 5.
    Central comparison and evolutionary tracking depend on the fidelity of the simulation model.

pith-pipeline@v0.9.0 · 5604 in / 1637 out tokens · 59644 ms · 2026-05-10T02:12:00.354092+00:00 · methodology

discussion (0)

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