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REVIEW 3 major objections 2 minor 88 references

Dynamical models of galaxies in two galaxy clusters produce velocity dispersion profiles that fit observations better than those from strong lensing models.

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T0 review · grok-4.3

2026-06-28 05:08 UTC pith:UQNL6ALO

load-bearing objection New dynamical sigma0 and rt values for 109 members are reported, but the claim that these are more robust than SL models does not follow because the dynamical fits are tuned to the kinematics while SL predictions are not. the 3 major comments →

arxiv 2606.05298 v2 pith:UQNL6ALO submitted 2026-06-03 astro-ph.GA

Dynamical models of cluster members to probe the total mass properties of cluster subhalos. I. A comparison with parametric strong lensing models

Nicola Bianchetti , Claudio Grillo , Giovanni Granata , Pietro Bergamini , Massimo Meneghetti , Amata Mercurio , Piero Rosati , Eros Vanzella
show 1 more author
Gabriel B. Caminha
This is my paper
classification astro-ph.GA
keywords dynamical modelsstrong lensingcluster subhalosvelocity dispersionFaber-Jackson relationAbell 2744MACS J0416MUSE spectroscopy
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper develops dynamical models for 109 early-type cluster members in Abell 2744 and MACS J0416 using MUSE spectroscopy and HFF photometry. It shows that these models recover central stellar velocity dispersions accurately and truncation radii for many galaxies. The models provide better fits to the measured line-of-sight velocity dispersion profiles than parametric strong lensing models do. The resulting Faber-Jackson relations have higher normalization than previous kinematic and lensing-based ones, suggesting that earlier estimates were biased by not correcting for the point spread function.

Core claim

By modeling cluster galaxies with dPIE total mass and Jaffe stellar density profiles fitted to MUSE kinematic data, the authors derive central velocity dispersions and truncation radii that yield superior matches to observed dispersion profiles compared to strong lensing reconstructions, and produce Faber-Jackson relations with systematically higher normalization.

What carries the argument

Spectral fitting pipeline for line-of-sight velocity dispersion profiles combined with dPIE and Jaffe density models to infer sigma_0 and r_t

Load-bearing premise

Previous kinematic estimates were biased by not accounting for the effects of the point spread function in the spectral measurements.

What would settle it

High-resolution kinematic observations of the same galaxies that avoid point spread function effects and yield velocity dispersions matching those from strong lensing models would falsify the claim of superior robustness.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • The dynamical measurements should be used as improved initial prescriptions in future strong lensing models.
  • Faber-Jackson scaling relations calibrated this way have higher normalization and compatible slope and scatter.
  • The approach resolves biases in previous kinematic estimates due to PSF effects.
  • This provides an independent probe of total mass properties of cluster subhalos.

Where Pith is reading between the lines

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

  • Applying the same method to additional clusters could test whether the discrepancy with cosmological simulations on subhalo masses is resolved.
  • Wider adoption might revise the inferred subhalo mass functions in strong lensing analyses of clusters.
  • The higher central velocity dispersions could imply more massive subhalos, with consequences for models of galaxy quenching in dense environments.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 2 minor

Summary. The manuscript develops dynamical models for 109 early-type cluster members in Abell 2744 and MACS J0416.1-2403 using MUSE spectroscopy and HFF photometry. Assuming dPIE total mass and Jaffe stellar density profiles, it measures central velocity dispersion σ₀ (accurately recovered for all) and truncation radius r_t (reliable for a subset with extended coverage), shows that the resulting models fit observed LOS velocity dispersion profiles better than predictions from strong-lensing (SL) models, calibrates Faber-Jackson relations with higher normalization than prior kinematic and SL works, and concludes that the new measurements are more robust (owing to PSF treatment) and should serve as improved priors for future SL modeling.

Significance. If the superiority claim survives a controlled comparison that avoids fitting bias, the work would supply observationally calibrated subhalo mass parameters that could reduce the reported tension between SL-derived subhalo masses and cosmological simulations. The independent MUSE dataset and explicit spectral-fitting pipeline constitute clear methodological assets.

major comments (3)
  1. [Abstract] Abstract: the statement that dynamical models 'predicted LOS velocity dispersion profiles that fit the measured ones better than those inferred from SL models' compares models whose parameters (σ₀, r_t) were optimized directly to the 109 MUSE profiles against unfitted extrapolations from SL constraints. This renders the reported improvement expected by construction and does not, by itself, establish greater robustness of the dynamical total-mass properties; a quantitative test (e.g., predictive residuals on held-out kinematic data or on an independent observable) is required.
  2. [Abstract] Abstract / Faber-Jackson section: the higher normalization reported for the new relations is derived from the fitted σ₀ values. Attribution of the offset solely to PSF correction (rather than to the adopted dPIE+Jaffe parametrization or other modeling choices) requires an explicit isolation of the PSF effect, for example by re-processing earlier kinematic catalogs with the new pipeline.
  3. [Results on r_t] Results on r_t: the abstract notes that r_t is reliably recovered only for the subset of galaxies with sufficiently extended radial coverage. The final claim that these values 'should therefore be adopted as improved initial prescriptions in future SL models' must be qualified by the fraction of the sample for which r_t is robust and by the propagated uncertainty on total subhalo mass.
minor comments (2)
  1. Provide explicit goodness-of-fit statistics (χ², rms residuals, or equivalent) for the dynamical versus SL profile comparisons rather than qualitative statements.
  2. State the precise number (and fraction) of galaxies with reliable r_t measurements and reference the corresponding table or figure.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive comments that help clarify the scope and limitations of our analysis. We respond to each major comment below and indicate where revisions will be made.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the statement that dynamical models 'predicted LOS velocity dispersion profiles that fit the measured ones better than those inferred from SL models' compares models whose parameters (σ₀, r_t) were optimized directly to the 109 MUSE profiles against unfitted extrapolations from SL constraints. This renders the reported improvement expected by construction and does not, by itself, establish greater robustness of the dynamical total-mass properties; a quantitative test (e.g., predictive residuals on held-out kinematic data or on an independent observable) is required.

    Authors: We agree that the reported improvement is expected by construction because the dynamical models are optimized to the MUSE data while the SL extrapolations are not. The scientific value lies in demonstrating that SL-derived subhalo parameters systematically fail to reproduce independent kinematic observations, which bears on the reported tension with simulations. To address the concern, we will add a quantitative cross-validation test (e.g., predictive residuals on a held-out subset of the kinematic profiles) and revise the abstract to qualify the comparison accordingly. revision: yes

  2. Referee: [Abstract] Abstract / Faber-Jackson section: the higher normalization reported for the new relations is derived from the fitted σ₀ values. Attribution of the offset solely to PSF correction (rather than to the adopted dPIE+Jaffe parametrization or other modeling choices) requires an explicit isolation of the PSF effect, for example by re-processing earlier kinematic catalogs with the new pipeline.

    Authors: The offset in normalization arises from our σ₀ measurements, which incorporate a full treatment of the MUSE PSF during spectral fitting. While we cannot re-process the earlier catalogs (which are not publicly available in the required form), we will expand the discussion section to compare methodological differences explicitly, including the impact of PSF modeling versus profile assumptions, and will avoid claiming the offset is due solely to the PSF. revision: partial

  3. Referee: [Results on r_t] Results on r_t: the abstract notes that r_t is reliably recovered only for the subset of galaxies with sufficiently extended radial coverage. The final claim that these values 'should therefore be adopted as improved initial prescriptions in future SL models' must be qualified by the fraction of the sample for which r_t is robust and by the propagated uncertainty on total subhalo mass.

    Authors: We agree that the claim requires qualification. In the revised manuscript we will state the exact fraction of the 109 galaxies for which r_t is robustly recovered, report the associated uncertainties, and discuss how these propagate to total subhalo mass before recommending the values as priors for future SL modeling. revision: yes

Circularity Check

1 steps flagged

Dynamical models fitted to MUSE LOS profiles; claimed superior fit vs. SL predictions is by construction

specific steps
  1. fitted input called prediction [Abstract]
    "Our dynamical models predicted LOS velocity dispersion profiles that fit the measured ones better than those inferred from SL models."

    Galaxies are modeled with dPIE total mass + Jaffe stellar density and optimized to the MUSE LOS velocity dispersion profiles of 109 cluster members to infer σ0 and rt. The resulting models are then stated to fit the measured profiles better than SL-inferred profiles. Since the dynamical models are fitted to the data while SL models are not, superior fit quality is guaranteed by construction and does not independently demonstrate more robust total mass properties.

full rationale

The paper's key claim that dynamical models 'predicted LOS velocity dispersion profiles that fit the measured ones better than those inferred from SL models' reduces directly to the fact that the dPIE+Jaffe models are optimized to the same MUSE kinematic data used for the comparison, while SL models are not. This matches the fitted_input_called_prediction pattern. The subsequent Faber-Jackson calibration uses the fitted σ0 values. No self-citation load-bearing, ansatz smuggling, or other patterns are present; the MUSE spectroscopy itself is an independent input. The central robustness conclusion therefore inherits the tautology.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; the modeling assumes standard dPIE and Jaffe functional forms whose parameters are fitted to the data, but no explicit list of free parameters or background axioms is provided.

pith-pipeline@v0.9.1-grok · 5917 in / 1298 out tokens · 21826 ms · 2026-06-28T05:08:14.549202+00:00 · methodology

0 comments
read the original abstract

In this series of papers, we present dynamical models of cluster members in strong lensing (SL) galaxy clusters to independently probe the persistent discrepancy reported between SL models and cosmological simulations, in terms of total mass properties for the cluster subhalos. In this work, we focused our study on early-type galaxies within Abell 2744 ($z=0.309$) and MACS J0416.1-2403 ($z=0.397$). We took advantage of deep MUSE spectroscopic data, complemented with HFF photometry. We used a pipeline based on spectral fitting to perform kinematic measurements of the LOS velocity dispersion profiles of 109 cluster members. We modeled the galaxies assuming a dPIE total mass density distribution and a Jaffe stellar mass density distribution. From the models, we inferred the values of the central stellar velocity dispersion, $\sigma_0$, and the truncation radius, $r_t$, for the galaxies in our sample. We found that $\sigma_0$ is accurately recovered for all of the cluster members, while $r_t$ is reliably measured for a fraction of galaxies in our sample, with sufficiently extended radial kinematic coverage. Our dynamical models predicted LOS velocity dispersion profiles that fit the measured ones better than those inferred from SL models. We then exploited the $\sigma_0$ measurements obtained from the dynamical models to calibrate the Faber-Jackson scaling relations for the cluster members in both galaxy clusters. When comparing our relations to those obtained in previous kinematics and SL works, we found systematically higher normalization and compatible slope and scatter values. We conclude that our dynamical measurements of $\sigma_0$ and $r_t$, along with calibrated scaling relations, are more robust than previous kinematic estimates which are biased by not taking into account the effects of the PSF, and should therefore be adopted as improved initial prescriptions in future SL models.

Figures

Figures reproduced from arXiv: 2606.05298 by Amata Mercurio, Claudio Grillo, Eros Vanzella, Gabriel B. Caminha, Giovanni Granata, Massimo Meneghetti, Nicola Bianchetti, Piero Rosati, Pietro Bergamini.

Figure 1
Figure 1. Figure 1: Spectrum of the cluster galaxy 80726 in M0416, extracted from a circular aperture with radius r = 0.5 ′′ centered on the galaxy luminos￾ity center. The black line shows the measured spectrum, while the red line shows the fitted spectrum, obtained with the pPXF pipeline, from rest-frame 3700 Å to 5100 Å. On the bottom, the residuals between the two spectra are shown as green dots. The gray bands highlight m… view at source ↗
Figure 3
Figure 3. Figure 3: Measured LOS velocity dispersion profile of galaxy 80726 as a function of the radial distance from the center, in both arcsec (bottom) and kpc (top). The red lines along the horizontal axis show the uncer￾tainty on the measurement position due to each annulus width, as shown in [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Corner plot obtained from the inference procedure on the cluster galaxy 83064 in M0416. The posterior probability distributions for σ0 and rt and their correlation are shown. The median values and 16th and 84th percentiles are reported at the top and highlighted with blue and green lines. 0.0 1.0 4.0 7.0 9.0 12.0 r [kpc] 0.00 0.25 0.75 1.25 1.75 2.25 0 50 100 150 200 250 300 ap [km s 1] Measured r [arcsec]… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison between measured and model-predicted velocity dispersion profiles. In black, we show the profile obtained from the kine￾matic measurements (red data points) of the cluster member 83064 in M0416. As orange solid lines, we plot 100 profiles obtained with the dynamical model by sampling the posterior distributions of the free pa￾rameters, drawn from the MCMC optimization and shown in [PITH_FULL_IM… view at source ↗
Figure 6
Figure 6. Figure 6: Corner plots of the central stellar ve￾locity dispersion, σ0, and truncation radius, rt , for two cluster members (38729 on the left and 34423 on the right) in A2744, obtained from the inference procedure. The posterior proba￾bility distributions of σ0 and rt and their corre￾lations are shown. The median values and per￾centiles are highlighted as in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: , we plot the measured LOS velocity dispersion profile (in black, with red error bars) for a galaxy (ID: 83064) in M0416 and compare it with 100 profiles obtained from the dPIE-J dynami￾cal model (in orange) and the F-J scaling relations calibrated in the B+21 (in green) and B+23b (in blue) SL models, sampling the posterior probability distributions of the model parameters. From the figure, it can be concl… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison between kinematic measurement (‘RS’ sample in Tab. 1) and dynamical model F-J scaling relations for the clusters of galaxies A2744 (on the left) and M0416 (on the right). In green, we plot the MCMC best-fitting F-J scaling relations obtained from B+23a and B+21. In orange, we present the best-fitting F-J scaling relations of our dynamical model. The measured kinematic and dynamical σ values (σ0 … view at source ↗

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Reference graph

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