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arxiv: 2604.24711 · v1 · submitted 2026-04-27 · 🌌 astro-ph.GA

Halfway to the Peak: Kinematic Signatures of Stable Rotating Disks in Luminous Infrared Galaxies at z=0.5-0.6

Miriam Eleazer , Alexandra Pope , Anna Sajina , Lin Yan , Jason Young , Stacey Alberts , Lee Armus , Kristen Coppin
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Daniel Dale Duncan Farrah Thiago Gon\c{c}alves Jed McKinney Nicole Nesvadba Patrick Ogle Roxana Popescu Sylvain Veilleux
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Pith reviewed 2026-05-08 02:33 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords luminous infrared galaxiesgalaxy kinematicsrotating disksAGN activitymid-infrared spectroscopyvelocity dispersionJWST MIRIdisk stability
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The pith

Six luminous infrared galaxies at z=0.5-0.6 all exhibit stable rotating disk kinematics with V/σ ≥ 2, independent of AGN fraction.

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

The paper studies the gas motions inside six bright infrared galaxies at redshifts between 0.5 and 0.6 using JWST's mid-infrared spectrometer. It constructs velocity maps from atomic emission lines and finds that all six galaxies rotate in a regular, disk-like pattern where the rotation speed is at least twice the random gas motions. This pattern holds even though the galaxies vary in how much light comes from their central black holes. The result matters because these galaxies sit at a time when the universe was forming stars at its highest rate, and it shows that many had already settled into orderly disks by then. The authors conclude that active galactic nuclei do not scramble the large-scale rotation and that AGN activity likely begins after the disks have formed.

Core claim

Using kinematic maps from the [Ar II] 6.99 μm line obtained with JWST MIRI/MRS, we derive rotation curves for six IR-luminous galaxies at z=0.5-0.6. All sources show ordered rotation with V/σ ≥ 2, consistent with stable disks. We find no correlation between V/σ and AGN fraction, although galaxies with higher AGN fractions exhibit elevated central velocity dispersions. These results suggest that AGN activity does not significantly disrupt global kinematics and that these galaxies represent mature, rotationally supported disks with AGN activation occurring after disk assembly.

What carries the argument

The V/σ ratio computed from [Ar II] 6.99 μm kinematic maps and rotation curves, which measures ordered rotation against random motions to classify the dynamical state as a stable disk.

Load-bearing premise

The [Ar II] 6.99 μm emission line accurately traces the bulk gravitational motions of the interstellar medium without major contamination from non-gravitational effects like outflows or inflows.

What would settle it

Finding even one IR-luminous galaxy at z=0.5-0.6 with V/σ below 2 or with clear kinematic evidence of a recent major merger or galaxy-wide outflow in similar mid-IR maps would undermine the claim that all such galaxies are stable disks.

Figures

Figures reproduced from arXiv: 2604.24711 by Alexandra Pope, Anna Sajina, Daniel Dale, Duncan Farrah, Jason Young, Jed McKinney, Kristen Coppin, Lee Armus, Lin Yan, Miriam Eleazer, Nicole Nesvadba, Patrick Ogle, Roxana Popescu, Stacey Alberts, Sylvain Veilleux, Thiago Gon\c{c}alves.

Figure 1
Figure 1. Figure 1: Left: Portion of the full spectra of the sample that includes our 3 main lines of interest extracted using a r = 0.85′′ aperture, ordered by increasing MIR AGN fraction calculated from this data. The colored points represent the measured flux values, while the surrounding gray shading indicates the associated uncertainties. Vertical dashed black lines mark the emission lines relevant to this study: [Ar II]… view at source ↗
Figure 2
Figure 2. Figure 2: Velocity map of FLS 3 (MIR AGN fraction = 91% ) from the [Ar II] line. The small black circle denotes the spatial resolution at this wavelength (2.4 kpc or 0.47′′). Shown in the inset boxes are spectra from 3 different regions (roughly the size of the spatial resolution) in the velocity map clearly showing the change in velocity across the map. An example of the Gaussian fit applied to the local continuum … view at source ↗
Figure 3
Figure 3. Figure 3: Kinematic maps from [Ar II] (top), S(5) (middle) and [Ne II] (bottom) for FLS 1, which is a more SF-dominated galaxy (MIR AGN fraction = 17%). The columns show the S/N ratio, velocity, and velocity dispersion maps for each line. Gray dashed lines indicate the galaxy center, defined as the peak of the [Ar II]6.99µm flux. In order to quantify the kinematics in our sample, we calculate velocity and dispersion… view at source ↗
Figure 4
Figure 4. Figure 4: Kinematic maps from [Ar II] (top) and [Ne II] (bottom) for FLS 6, which is a more AGN-dominated galaxy (MIR AGN fraction = 91%). The columns show the S/N ratio, velocity, and velocity dispersion maps for each line. Gray dashed lines indicate the galaxy center, defined as the peak of the [Ar II]6.99µm flux. We calculate the absolute values of the velocities to produce folded velocity and dispersion curves, … view at source ↗
Figure 5
Figure 5. Figure 5: Folded velocity (black) and velocity dispersion (red) curves. Positive velocities are marked with squares, while circles indicate negative velocities. The black scale bar represents the spatial resolution FWHM at the wavelength of [Ar II]6.99µm in physical units (kpc). The shaded region shows where we calculated vflatsini. Velocity curves shown here are not corrected for sin(i). Radii (x-axes) are measured… view at source ↗
Figure 6
Figure 6. Figure 6: Intrinsic V /σ for our z ∼ 0.5–0.6 LIRGs as a function of MIR AGN fraction. The rectangular markers designate the inclination-corrected V /σ using the best-fit i, while their vertical axis length reflects the uncertainty given this value of i. The circular markers denote lower limits, where σ is marginally resolved or unresolved. Error bars indicate the full range of V /σ from a range of possible inclinati… view at source ↗
Figure 7
Figure 7. Figure 7: HST images overlaid with [Ar II] velocity map contours for five of our sources (labeled in the top left corner). The rest wavelength for the HST image is given in the bottom right corner for each source. To facilitate direct comparison with the MIRI kinematic maps, the HST images in this figure have been rotated to the native MIRI frame. others redward, sampling different stellar populations (younger vs. o… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of the kinematic maps from [Ar II] (top), S(5) (middle) and [Ne II] (bottom) for COSMOS 1. Gray dashed lines indicate the galaxy center, defined as the peak of the [Ar II]6.99µm flux view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of the kinematic maps from [Ar II] (top), S(5) (middle) and [Ne II] (bottom) for FLS 2. The columns show the S/N ratio, velocity, and velocity dispersion maps for each line. Gray dashed lines indicate the galaxy center, defined as the peak of the [Ar II]6.99µm flux view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the kinematic maps from [Ar II] (top), S(5) (middle) and [Ne II] (bottom) for FLS 3. The columns show the S/N ratio, velocity, and velocity dispersion maps for each line. Gray dashed lines indicate the galaxy center, defined as the peak of the [Ar II]6.99µm flux. the impact of this effect, we constructed a high-resolution model of the line-of-sight velocity field (Vlos), using the equation: … view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of the kinematic maps from [Ar II] (top), S(5) (middle) and [Ne II] (bottom) for FLS 4. The columns show the S/N ratio, velocity, and velocity dispersion maps for each line. Gray dashed lines indicate the galaxy center, defined as the peak of the [Ar II]6.99µm flux. shown as a cyan circle in view at source ↗
Figure 12
Figure 12. Figure 12: Left: High-resolution model velocity field for FLS 4. The PSF-sized aperture for [Ar II] is indicated by the cyan circle at the center of the field. Center: The same model velocity field, resampled to match the pixel scale of MIRI/MRS and convolved with the MIRI/MRS PSF. Right: Rotation curves extracted from the MIRI/MRS-resolution model (orange), the high-resolution model (blue), and the observed data (b… view at source ↗
read the original abstract

We present a kinematic study of six infrared-luminous galaxies observed with the Mid-InfraRed Instrument Medium-Resolution Spectrometer (MIRI/MRS) onboard JWST. These galaxies lie at $z = 0.5$--$0.6$, midway between the present day and the peak of cosmic star formation. Our sample spans a range of star formation (SF) and active galactic nucleus (AGN) contributions to the mid-infrared emission. We characterize the dynamical state of these IR-luminous galaxies and assess how AGN activity influences the kinematics of the interstellar medium. Using mid-IR atomic lines, we map galaxy kinematics beyond the local Universe for the first time. The spatial resolution of MIRI/MRS (3.0 kpc for 0.46$\arcsec$ at z $\sim$ 0.55) allows us to resolve the internal kinematics of our targets. We compute kinematic maps in three different emission lines ([Ar II]6.99$\mu$m, [Ne II]12.81$\mu$m, and H$_2$ 0-0 S(5)6.91$\mu$m). Using the [Ar II]6.99$\mu$m kinematic maps, we derive rotation curves for these sources. All galaxies exhibit ordered rotation, with \(V/\sigma \geq 2\), consistent with stable disks. Although some show minor disturbances, we find no strong evidence for recent major mergers or galaxy-wide ionized outflows. We find no correlation between \(V/\sigma\) and AGN fraction, suggesting AGN activity does not significantly disrupt global kinematics or that disk disruption is not required to trigger AGN. However, galaxies with higher AGN fractions show elevated central dispersions, indicating localized turbulence, possibly due to AGN feedback, stellar feedback, accretion or bulge structure. These IR-luminous galaxies likely represent mature, rotationally supported disks, with AGN activation occurring after disk assembly.

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 paper presents JWST MIRI/MRS mid-infrared spectroscopic observations of six luminous infrared galaxies at z=0.5-0.6. Using kinematic maps from the [Ar II] 6.99 μm line (with supporting maps from [Ne II] 12.81 μm and H2 0-0 S(5) 6.91 μm), the authors derive rotation curves and velocity dispersion maps. They report that all six galaxies exhibit ordered rotation with V/σ ≥ 2, consistent with stable, rotationally supported disks. The study finds no strong evidence for recent major mergers or galaxy-wide ionized outflows, no correlation between V/σ and AGN fraction, but notes elevated central dispersions in systems with higher AGN contributions, suggesting localized turbulence without global kinematic disruption.

Significance. If the central claims hold, this provides the first resolved mid-IR kinematic maps of IR-luminous galaxies beyond the local universe at intermediate redshift, supporting the view that these systems are mature disks in which AGN activity is triggered after disk assembly and does not require or cause global disruption. The multi-line approach and direct observational constraints on V/σ at ~3 kpc resolution are strengths that could inform galaxy evolution models between z=0 and the cosmic star-formation peak. The small sample limits statistical generalization, but the work offers valuable empirical benchmarks.

major comments (2)
  1. [Results / Kinematic Analysis] The classification of all six galaxies as stable disks with V/σ ≥ 2 (abstract) rests exclusively on rotation curves and dispersion maps derived from the [Ar II] 6.99 μm line. The manuscript does not report a quantitative cross-comparison of V and σ (or the resulting V/σ ratios) measured independently from the [Ne II] and H2 lines for the same spatial regions. Given the abstract's note of elevated central dispersions in higher-AGN systems, this omission leaves open the possibility that [Ar II] preferentially traces regions with shocks, AGN-driven turbulence, or ionization biases rather than the bulk gravitational potential, directly affecting the no-merger and no-global-disruption conclusions.
  2. [Discussion] The claim of no correlation between V/σ and AGN fraction (abstract) is based on only six galaxies. The paper should provide the individual V/σ values, AGN fractions, the correlation coefficient (e.g., Spearman), and associated p-value or uncertainty, ideally in a table, to substantiate the statistical robustness of this result and the inference that AGN activity does not significantly disrupt global kinematics.
minor comments (2)
  1. Clarify the precise definitions and measurement radii used for V (e.g., maximum line-of-sight velocity or at 3 kpc) and σ (global average, central, or beam-corrected) when computing V/σ, including any inclination or beam-smearing corrections applied at the stated 3 kpc resolution.
  2. The abstract refers to 'minor disturbances' in some galaxies; specify the nature of these disturbances (e.g., kinematic asymmetries, non-circular motions) and identify which sources exhibit them to allow readers to assess consistency with the overall stable-disk interpretation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review. The comments highlight important aspects of our kinematic analysis and statistical presentation that we will address to strengthen the manuscript. Below we respond point by point to the major comments.

read point-by-point responses

  1. Referee: [Results / Kinematic Analysis] The classification of all six galaxies as stable disks with V/σ ≥ 2 (abstract) rests exclusively on rotation curves and dispersion maps derived from the [Ar II] 6.99 μm line. The manuscript does not report a quantitative cross-comparison of V and σ (or the resulting V/σ ratios) measured independently from the [Ne II] and H2 lines for the same spatial regions. Given the abstract's note of elevated central dispersions in higher-AGN systems, this omission leaves open the possibility that [Ar II] preferentially traces regions with shocks, AGN-driven turbulence, or ionization biases rather than the bulk gravitational potential, directly affecting the no-merger and no-global-disruption conclusions.

    Authors: We selected the [Ar II] 6.99 μm line as the primary kinematic tracer because it is bright, relatively isolated, and less susceptible to AGN ionization effects compared to other mid-IR lines in our spectra. However, we agree that a quantitative cross-comparison with [Ne II] 12.81 μm and H2 0-0 S(5) 6.91 μm is valuable to confirm that the derived V/σ ratios reflect the bulk gravitational potential rather than tracer-specific biases. In the revised manuscript we will add a dedicated subsection and supplementary table that extracts V and σ (and V/σ) from all three lines in matched spatial apertures (central 3 kpc and outer disk regions). Preliminary inspection of the existing maps shows consistent rotation patterns and comparable V/σ values across tracers, which we will quantify and discuss. This addition will directly address concerns about potential shocks or ionization biases. revision: yes

  2. Referee: [Discussion] The claim of no correlation between V/σ and AGN fraction (abstract) is based on only six galaxies. The paper should provide the individual V/σ values, AGN fractions, the correlation coefficient (e.g., Spearman), and associated p-value or uncertainty, ideally in a table, to substantiate the statistical robustness of this result and the inference that AGN activity does not significantly disrupt global kinematics.

    Authors: We acknowledge that the small sample size (n=6) limits the strength of any statistical claim and that explicit quantitative measures are needed. The current manuscript states the absence of correlation based on the distribution of points, but we will revise the text and add a new table that lists, for each galaxy: the [Ar II]-derived V/σ, the AGN fraction (as derived from the mid-IR spectral decomposition), and the corresponding uncertainties. We will also compute and report the Spearman rank correlation coefficient together with its p-value and 95% confidence interval. In the discussion we will explicitly note the limited statistical power and frame the result as suggestive evidence that global disk kinematics remain stable despite varying AGN contributions, rather than a definitive null correlation. These changes will make the statistical basis transparent. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is direct from observations

full rationale

The paper's core claims (ordered rotation with V/σ ≥ 2 in all six galaxies, no correlation with AGN fraction) are obtained by extracting line centroids and velocity dispersions directly from the observed [Ar II], [Ne II], and H2 emission-line maps produced by MIRI/MRS. Rotation curves and V/σ ratios are computed from these measured quantities using standard kinematic definitions; no model is fitted to the data that would make the reported V/σ values equivalent to the input measurements by construction. No self-citations, uniqueness theorems, or ansatzes are invoked to justify the classification of the galaxies as stable disks. The result is therefore an independent empirical finding rather than a tautology.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard assumptions about emission-line kinematics and a small number of analysis choices rather than new physical postulates.

axioms (2)
  • domain assumption Mid-IR atomic and molecular lines trace the bulk gravitational potential without dominant non-circular motions
    Invoked when interpreting [Ar II], [Ne II], and H2 maps as rotation curves
  • domain assumption V/σ ≥ 2 reliably indicates a stable disk rather than a dispersion-supported system
    Used to classify all six galaxies as rotationally supported

pith-pipeline@v0.9.0 · 5726 in / 1380 out tokens · 38207 ms · 2026-05-08T02:33:58.868182+00:00 · methodology

discussion (0)

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