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arxiv: 2606.27853 · v1 · pith:JVQJJQN2new · submitted 2026-06-26 · 🌌 astro-ph.GA

MSA-3D: Rotation Curves and Dark Matter Fractions at z~0.5-1.7 with JWST/NIRSpec

Juan M. Espejo Salcedo , Danail Obreschkow , Karl Glazebrook , Tucker Jones , Ivana Bari\v{s}i\'c , Natascha M. F\"orster Schreiber , Takafumi Tsukui , Xin Wang
show 12 more authors
Mengting Ju Qianqiao Zhou Amit Nestor-Schachar Ryan L. Sanders Stavros Pastras Namrata Roy Alaina Henry Kyle Westfall Themiya Nanayakkara Matthew Malkan Fahmi M. Al Farisy Isaac Kanowski
This is my paper

Pith reviewed 2026-06-29 03:41 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords rotation curvesdark matter fractionshigh-redshift galaxiesJWST observationsstar-forming disksTully-Fisher relationgalaxy kinematicsdynamical modelling
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The pith

JWST observations of 23 galaxies at z~0.5-1.7 show dark matter fractions ranging from 0.1 to 0.9 with a median of 0.63.

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

The paper uses JWST/NIRSpec to measure ionised-gas kinematics and rotation curves in 30 star-forming galaxies across redshifts 0.5 to 1.7, extending down to stellar masses of 10^9 solar masses. Forward modelling of these data with NIRCam imaging separates baryonic and dark matter contributions, revealing that most systems are rotationally supported disks. Dark matter fractions within the effective radius display substantial galaxy-to-galaxy variation, and rotation curves reaching beyond 2Re fall into rising, flat, or falling categories that track the balance between rotation and dispersion support. The stellar Tully-Fisher relation matches expectations from local samples evolved under self-similar Lambda-CDM scaling, while a seeing test indicates resolution effects contribute to but do not fully account for offsets seen in other high-redshift work.

Core claim

For the 23 galaxies in the primary statistical sample, the data show predominantly rotationally supported disks with intrinsic dispersions 31-65 km/s and dark matter fractions f_DM(R_e) from 0.1 to 0.9 (median 0.63, scatter 0.2 dex). Among the 19 galaxies reaching at least 2R_e, six have rising, six flat, and seven falling rotation curves; these map to an observed sequence from rotation-dominated, dark-matter-rich disks (V_rot/sigma_0 ~4, f_DM >0.7) to dispersion-supported systems with centrally concentrated baryons (V_rot/sigma_0 ~2, f_DM <0.55). The stellar Tully-Fisher relation lies close to the local relation evolved under the adopted self-similar Lambda-CDM scaling, and a simplified see

What carries the argument

Forward dynamical modelling that combines spatially resolved ionised-gas kinematics from JWST/NIRSpec with JWST/NIRCam imaging to constrain the separate baryonic and dark matter contributions inside R_e.

If this is right

  • Star-forming disks near z~1 span a broad range of dynamical states and inner mass distributions.
  • The stellar Tully-Fisher relation at these redshifts is consistent with the local relation after Lambda-CDM evolution.
  • Spatial resolution contributes to but does not fully explain differences among high-redshift Tully-Fisher measurements.
  • Previous surveys are extended toward lower stellar masses spanning 9.0 < log(M_star/M_sun) < 11.2.

Where Pith is reading between the lines

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

  • The observed link between rotation-curve shape and dark matter fraction could be tested by measuring how these quantities evolve with redshift in larger samples.
  • The 0.2 dex scatter in dark matter fractions may reflect differences in how individual galaxies assembled their mass.
  • Connecting the dynamical classes to star-formation efficiency would help test whether baryon concentration drives the shift from rotation- to dispersion-supported states.

Load-bearing premise

Forward dynamical modelling accurately separates baryonic and dark matter contributions despite the spatial resolution limits of the observations and the assumptions required about mass distributions and inclinations.

What would settle it

Higher-resolution kinematic maps or a larger sample that instead shows dark matter fractions clustered tightly around 0.5 with little scatter would falsify the reported wide range and ordering by rotation-curve shape.

Figures

Figures reproduced from arXiv: 2606.27853 by Alaina Henry, Amit Nestor-Schachar, Danail Obreschkow, Fahmi M. Al Farisy, Isaac Kanowski, Ivana Bari\v{s}i\'c, Juan M. Espejo Salcedo, Karl Glazebrook, Kyle Westfall, Matthew Malkan, Mengting Ju, Namrata Roy, Natascha M. F\"orster Schreiber, Qianqiao Zhou, Ryan L. Sanders, Stavros Pastras, Takafumi Tsukui, Themiya Nanayakkara, Tucker Jones, Xin Wang.

Figure 1
Figure 1. Figure 1: Star-formation rate as a function of stellar mass for our kinematic sample (0 [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Colour composite images of a representative subsample of galaxies from the MSA-3D Cycle 1 sample. For each galaxy, [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Summary of imaging and kinematic properties for galaxy [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Position–velocity (PV) diagram for galaxy [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Intrinsic velocity dispersion σ0 as a function of rota￾tional support, quantified by Vrot(Re)/σ0, where Vrot(Re) is the rotation velocity evaluated at the effective radius. Blue-filled cir￾cles show galaxies in the golden sample, while open triangles indicate the good sample; this colour and symbol convention is adopted throughout the remainder of the paper unless noted otherwise. The vertical dashed lines… view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between the rotational-support parameter [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: MSA-3D stellar Tully–Fisher relation. Blue symbols and empty triangles show the MSA-3D measurements for the [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Comparison between the MSA-3D stellar Tully–Fisher [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Example of kinematic forward modelling with [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: Within the MSA-3D sample, we find at most a weak [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 11
Figure 11. Figure 11: Dark matter fraction within one effective radius, fDM(Re), as a function of stellar mass M⋆. Blue circles show the MSA-3D galaxies, with vertical error bars indicating the 1σ uncertainties derived from the DysmalPy forward modelling. Green diamonds denote the RC100 (redshift- and mass-matched) comparison sample. Orange diamonds and the dashed line indi￾cate the median trend reported by Sharma et al. (2021… view at source ↗
Figure 12
Figure 12. Figure 12: Dark matter fraction within one effective radius, fDM(Re), as a function of the surface baryonic density within Re. The red solid curve shows the empirical relation of (Wuyts et al. 2016, Eq. 6), log10 fbar = −0.34 + 0.51[log10(Σbar) − 8.5], converted to dark matter fraction via fDM = 1 − fbar. The red shaded region spans ±0.2 dex in log fbar, corresponding to bounds fDM = 1 − 10log10 fbar±0.2 . Orange di… view at source ↗
Figure 13
Figure 13. Figure 13: Rotation curves for the galaxies in the MSA-3D sample, shown as a mosaic. In each panel, the orange curve shows the best [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Distribution of kinematic, structural, and environmen [PITH_FULL_IMAGE:figures/full_fig_p019_14.png] view at source ↗
read the original abstract

We present rotation curves and inner mass distributions for 30 star-forming galaxies at $0.5<z<1.7$, observed with JWST/NIRSpec as part of the MSA-3D Cycle 1 survey. Combining spatially resolved ionised-gas kinematics with JWST/NIRCam imaging, we constrain baryonic and dark matter contributions through forward dynamical modelling for galaxies extending down to stellar masses of $\sim10^{9}M_\odot$. For the 23 galaxies in our primary statistical sample, we find predominantly rotationally supported disks with intrinsic dispersions $\sigma_0\sim31$-65 km s$^{-1}$ and a wide range of dark matter fractions, $f_{DM}(R_e)\sim0.1$-0.9, with a median of 0.63 and substantial galaxy-to-galaxy scatter of $\sim0.2$ dex. These results are supported by a complementary consistency check using stellar mass maps and SFR-derived gas profiles. Among the 19 galaxies reaching $\gtrsim2R_e$, we identify six rising, six flat, and seven falling rotation curves. These classes define an observed ordering from rotationally dominated, dark-matter-rich disks ($V_{rot}/\sigma_0\approx4$, $f_{DM}\gtrsim0.7$) to more dispersion-supported systems with centrally concentrated baryonic mass distributions ($V_{rot}/\sigma_0\approx2$, $f_{DM}\lesssim0.55$). The stellar Tully-Fisher relation lies close to the local relation evolved under the adopted self-similar $\Lambda$CDM scaling. A simplified seeing-degradation test shifts the inferred normalisation by ~0.2 dex at fixed $V_c$, suggesting that spatial resolution contributes to, but does not fully explain, differences among high-redshift Tully-Fisher measurements. Overall, MSA-3D provides a high-resolution extension of previous surveys toward lower stellar masses, spanning $9.0 < \log(M_\star/M_\odot) < 11.2$, and reinforces that star-forming disks near $z\sim1$ span a broad range of dynamical states and inner mass distributions.

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 / 1 minor

Summary. The manuscript reports JWST/NIRSpec IFU observations of ionised-gas kinematics in 30 star-forming galaxies at 0.5<z<1.7, combined with NIRCam imaging. Forward dynamical modelling is used to derive rotation curves, intrinsic dispersions (σ0∼31-65 km s−1), and dark matter fractions fDM(Re) for a primary sample of 23 galaxies, yielding a median fDM(Re)=0.63 with ∼0.2 dex scatter. Among the 19 galaxies reaching ≳2Re, rotation curves are classified as rising (6), flat (6), or falling (7), with correlations to Vrot/σ0 and fDM. A consistency check with stellar mass maps and SFR-derived gas profiles is presented, along with a simplified seeing-degradation test affecting the Tully-Fisher normalisation by ∼0.2 dex.

Significance. If the baryon-DM decompositions hold, the work provides valuable new constraints on inner mass distributions and dynamical states in star-forming disks at intermediate redshift, extending prior surveys to lower stellar masses (down to ∼10^9 M⊙). The reported range of fDM values and rotation-curve morphologies, plus the Tully-Fisher comparison, would offer empirical input for galaxy formation simulations.

major comments (2)
  1. [dynamical modelling description and abstract] The headline median fDM(Re)=0.63 (with 0.2 dex scatter) for the 23-galaxy sample rests on forward dynamical modelling whose robustness to key assumptions is not fully quantified. The abstract notes a simplified seeing-degradation test and a consistency check with SFR-derived gas profiles, but these do not include systematic variation of the DM halo functional form (e.g., NFW versus cored profiles), inclination priors, or gas dispersion assumptions. At the reported NIRSpec resolution (∼0.8-1.5 kpc), beam-smearing and inclination-DM degeneracies can trade central baryonic concentration against fDM without altering the observed line-of-sight velocities, directly affecting the load-bearing claim.
  2. [sample and modelling sections] For the lower-mass end of the sample (∼10^9 M⊙), Re is comparable to or smaller than the spatial resolution; the paper does not report the posterior width on fDM(Re) when the baryonic surface-density parametrisation is varied (exponential versus NIRCam-derived) or when alternative inclination constraints are adopted. This leaves the reported galaxy-to-galaxy scatter and the ordering by rotation-curve class vulnerable to modelling systematics.
minor comments (1)
  1. [abstract] The abstract states the primary statistical sample comprises 23 galaxies but does not explicitly list the selection cuts (e.g., S/N, inclination range, or spatial coverage) that distinguish it from the full 30-galaxy set.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful and constructive review. The comments identify areas where additional quantification of modelling assumptions will strengthen the manuscript. We address each point below and will incorporate the suggested tests in the revised version.

read point-by-point responses

  1. Referee: [dynamical modelling description and abstract] The headline median fDM(Re)=0.63 (with 0.2 dex scatter) for the 23-galaxy sample rests on forward dynamical modelling whose robustness to key assumptions is not fully quantified. The abstract notes a simplified seeing-degradation test and a consistency check with SFR-derived gas profiles, but these do not include systematic variation of the DM halo functional form (e.g., NFW versus cored profiles), inclination priors, or gas dispersion assumptions. At the reported NIRSpec resolution (∼0.8-1.5 kpc), beam-smearing and inclination-DM degeneracies can trade central baryonic concentration against fDM without altering the observed line-of-sight velocities, directly affecting the load-bearing claim.

    Authors: We agree that systematic tests of these assumptions are warranted to better support the robustness of the median fDM value. In the revised manuscript we will add an expanded discussion and new figures in the dynamical modelling section that vary the DM halo functional form (NFW versus cored), explore the effect of different inclination priors, and test alternative gas dispersion assumptions. We will also quantify the impact of beam-smearing and inclination-DM degeneracies on the derived fDM(Re) values. These additions will directly address the concern while retaining the existing consistency check and seeing-degradation test as supporting evidence. revision: yes

  2. Referee: [sample and modelling sections] For the lower-mass end of the sample (∼10^9 M⊙), Re is comparable to or smaller than the spatial resolution; the paper does not report the posterior width on fDM(Re) when the baryonic surface-density parametrisation is varied (exponential versus NIRCam-derived) or when alternative inclination constraints are adopted. This leaves the reported galaxy-to-galaxy scatter and the ordering by rotation-curve class vulnerable to modelling systematics.

    Authors: We acknowledge that explicit reporting of these sensitivities is needed, particularly for the lower-mass galaxies where resolution effects are more pronounced. The revised manuscript will include new material in the sample and modelling sections (and an associated appendix) that reports the posterior widths on fDM(Re) for the affected galaxies and demonstrates the changes when the baryonic surface-density parametrization is switched between exponential and NIRCam-derived profiles, as well as under alternative inclination constraints. This will allow direct assessment of the robustness of the reported scatter and rotation-curve classifications. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results derived from new observations via forward modeling

full rationale

The paper's central results (rotation curves, intrinsic dispersions, and f_DM(Re) values for 23 galaxies) are obtained by applying forward dynamical modeling directly to new JWST/NIRSpec kinematic data and NIRCam imaging for galaxies at 0.5<z<1.7. No load-bearing step reduces to a fitted parameter from prior data, a self-citation chain, or a self-definitional relation; the Tully-Fisher comparison uses an external local benchmark evolved under standard ΛCDM scaling. The derivation is self-contained against external benchmarks, with the seeing-degradation test serving as an internal consistency check rather than a circular input.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The paper relies on standard assumptions in galactic dynamics but introduces no new free parameters or entities in the abstract.

axioms (2)
  • domain assumption Galaxies are assumed to be in dynamical equilibrium for the modelling to apply.
    Forward dynamical modelling requires this to separate components.
  • domain assumption The ionised gas traces the gravitational potential accurately.
    Used for kinematics.

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Reference graph

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