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REVIEW 3 major objections 6 minor 56 references

Prospects for high-resolution probes of galaxy dynamics tracing background cosmology in MaNGA

T0 review · 3 major / 6 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read This paper argues that the MaNGA survey's large sample can control scatter in the mean of three position angles to about one percent, making stacked rotation curves a viable probe of background cosmology.

desk verdict A useful descriptive measurement of PA consistency scatter in MaNGA, but the one-percent stacked-RC precision claim rests on an unmeasured coupling and does not follow from the data as stated. read the letter →

arxiv 2501.11882 v1 pith:FCLAB4HS submitted 2025-01-21 astro-ph.CO astro-ph.GA

Gyeong-Min Lee , Maurice H.P.M. van Putten This is my paper · ORCID
classification astro-ph.COastro-ph.GA
keywords MaNGAgalaxyrotationcurvesstackedpositionanglesdeSitteraccelerationbaryonicTully-FisherrelationHubbletensioncosmologicalprobes
topics The Hubble Tension
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper argues that the large MaNGA survey can control scatter in the mean of three position angles (photometric, gas, and stellar) to about one percent, by selecting sub-samples whose three orientations agree within $\theta \le 30^\circ$. With samples of size $N=N_i(\theta)$, the scatter in the mean $\sigma/\sqrt{N}$ reaches one-percent levels and is differentiated by inclination. This matters because scatter in the mean is a lower bound to the uncertainty of stacked rotation curves; at one percent, stacked RCs would be sensitive to a proposed transition in galaxy dynamics at the de Sitter acceleration $a_{dS}=cH$, and to the baryonic Tully-Fisher relation, turning galaxy dynamics into a probe of background cosmology. The authors present this as a preliminary feasibility step: the actual stacked rotation curves and the calibration factor $\kappa$ are left for future work.

What carries the argument

The central mechanism is PA-consistency control on subsample size. Three position angles are measured per galaxy: $PA_{\rm ph}$ from photometry and $PA_g$, $PA_s$ from least-squares sine fits to gas and stellar velocity fields; the paper then forms $\Delta_1{\rm PA} = PA_g - PA_s$ and $\Delta_2{\rm PA} = PA_{\rm ph} - (PA_g+PA_s)/2$. Selecting sub-samples by $|\Delta_k{\rm PA}|<\theta$ (or the joint box $|\Delta_b{\rm PA}|<\theta$) fixes $N=N_i(\theta)$ in bins of inclination, and the scatter in-the-mean $\sigma/\sqrt{N}$ of these PA differences is used as the noise control. The standard error of an ensemble average is written $SE = \sqrt{\kappa^2\sigma^2+\cdots}/\sqrt{N}$, with $\kappa_k = \partial SE/\partial(\sigma/\sqrt{N})_k$; since $\Delta_1$ and $\Delta_2$ are nearly uncorrelated, $\sigma_b \simeq \sqrt{\sigma_1^2+\sigma_2^2}$. The fitted relations (8) and (10) quantify how $\sigma/\sqrt{N}$ falls with $\theta$, reaching one percent. This machinery converts survey size into a statistical-error statement without yet stacking any rotation curves.

What would settle it

Stack actual MaNGA rotation curves in the same PA-selected sub-samples for $\theta = 10^\circ, 20^\circ, 30^\circ$, and compare the measured standard error in the mean of $V_c(r)$ at fixed normalized radius with $\kappa\sigma/\sqrt{N}$ from PA scatter; if the RC-stack error does not track the PA scatter with $\kappa$ of order unity, the one-percent cosmological prospect fails.

Watch

Extended reading notes

Core claim

On the authors' terms, the central result of Sections 3 and 4 is that MaNGA's large sample provides the required $N$ to control scatter in-the-mean of three position angles, taken from photometry and from gas and stellar velocity fields, down to one-percent levels. Within the joint box $|\Delta_b{\rm PA}|<\theta$, the scatter in-the-mean satisfies $(\sigma/\sqrt{N})_b \simeq (0.625 + 0.031\theta)\,[\%\,{\rm rad}]$, giving about $1.6\%$ rad at $\theta=30^\circ$ and $0.94\%$ rad at $\theta=10^\circ$ for $i<80^\circ$, with the two PA-difference variables statistically independent. Since scatter in the mean enters the standard error as $\kappa\sigma/\sqrt{N}$ with $\kappa$ of order unity, the authors take this as a lower bound to the total uncertainty budget of stacked rotation curves, offering resolution sufficient to test the sharp $C^0$-transition at $a_{dS}=cH$ and, further out, the baryonic Tully-Fisher relation. The paper is explicit that this is a prospect, pending measurement of $\kappa$ and demonstration that PA scatter proxies the full noise budget.

Load-bearing premise

The conclusion depends on an unmeasured premise: that scatter among the three position angles faithfully represents the total noise budget of stacked rotation curves, with a proportionality factor $\kappa$ near unity.

Editorial extensions

If this is right

  • MaNGA stacked rotation curves could reach a standard error in the mean near one percent, matching the precision of modern $H_0$ measurements.
  • Sub-samples binned by inclination and PA consistency remain large enough (hundreds of galaxies) to measure $\kappa$ per bin at a few percent uncertainty, so the error budget can be calibrated empirically.
  • An independent, large-$N$ confirmation of the claimed $C^0$-transition across $a_{dS}=cH$ becomes feasible, with transition radius $r_t=\sqrt{R_GR_H}\simeq 4.7\,{\rm kpc}\,M_{11}^{1/2}$.
  • Resolving $a_{dS}$ would let galaxy dynamics estimate $H_0$, potentially distinguishing the two sides of the Hubble tension, and via $a_0=c^2/(2\pi)\sqrt{J}$ provide an estimate of the deceleration parameter $q_0$.
  • At larger radii, the same stacked RCs can probe the baryonic Tully-Fisher relation over MaNGA's mass range.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Editorial extension: The one-percent claim is a lower bound only if PA scatter actually proxies all significant noise in stacked rotation curves; a direct measurement of the stacked-RC standard error is needed before the cosmological program stands.
  • Editorial extension: The PA-consistency cut may preferentially select galaxies with simple, axisymmetric kinematics; if misalignment correlates with environment, bars, or non-circular motions, the reduced scatter could partly reflect selection rather than noise reduction.
  • Editorial extension: If the $a_{dS}=cH$ transition is real, its location scales with the Hubble radius, so redshift-binned samples from future large-$N$ surveys could separate this cosmological signal from a fixed-acceleration alternative; the present MaNGA sample mostly tests the present epoch.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper analyzes MaNGA DR17 spiral galaxies to measure consistency among three position angles (photometric PA, gas kinematic PA, stellar kinematic PA). It defines differences Δ1PA = PAg − PAs and Δ2PA = PAph − PAvf, selects sub-samples with |ΔkPA| < θ, and reports σ/√N as a function of θ and inclination bin, finding angular scatter in the mean of about 1% rad at θ ≈ 10°. It interprets this as a lower bound on the standard error of ensemble-averaged (stacked) rotation curves and argues that MaNGA can therefore probe the de Sitter acceleration scale a_dS = cH and the baryonic Tully-Fisher relation with percent-level statistical precision.

Significance. If the connection between PA scatter and stacked-RC noise were established, the paper would provide a useful first step: MaNGA's large N does allow sub-samples with internal PA consistency at the level where the standard error of the PA differences reaches about 1% rad, and the Pearson analysis supports approximate, though not perfect, independence of the two PA differences. The cross-checks with literature PAs and the use of public MaNGA data are strengths. However, the central cosmological prospect is not currently supported, because the paper never constructs stacked RCs, never measures κ in Eq. (2), and does not derive how PA scatter maps onto RC amplitude errors.

major comments (3)
  1. [§4 and Eq. (2)] The claim that one-percent PA scatter in the mean constitutes a lower bound on the standard error of stacked RCs is not established. The standard error of the mean PA offset, σ/√N, is not the same as the fractional error in a stacked RC amplitude. For a disk with a PA error δ, the derived circular velocity enters through a factor such as cosδ, so the leading effect is second order in δ: a systematic bias of order ⟨δ²⟩/2 that does not decrease with N, plus a statistical term of order σ_δ²/√N. With σ_δ ≈ 10°, the bias is about 1.5%, while the statistical term is far below 1% for N ≳ 1000. Thus the displayed 1% rad scatter in the mean does not translate to 1% RC amplitude precision, and the paper's 'lower bound' is not a lower bound on the RC noise budget. The authors should either derive the actual mapping, construct stacked RCs, or explicitly reframe the result as PA consistency being a necessary but not sufficient condition.
  2. [§3, Eq. (7)] κ is defined but never measured. The statement that κ can be measured 'by varying the control parameter θ' is not demonstrated and is questionable: varying θ changes both σ and N and also selects different galaxy subsamples, so without a model of how the other noise terms in Eq. (2) depend on θ and N, the partial derivative in Eq. (7) cannot be isolated from the data presented. At minimum, the paper should provide a toy model or a direct measurement of the RC stack noise as a function of θ to validate the assumed linear relationship.
  3. [§3, Eq. (10) and abstract] The reported quantity σ/√N has units of degrees or radians, and the paper states values such as '1.6 % rad' and '0.94 % rad'. Calling this a 'one-percent lower bound' on the standard error of stacked RCs without a conversion factor that defines κ in Eq. (2) is a category error: a 1% rad angular scatter is not a 1% fractional error in velocity or acceleration. The units should be clarified, and the claim should be limited to angular PA scatter unless a physical mapping to the dynamical observable is provided.
minor comments (6)
  1. [§2 and Table 1] The exclusion of the i ≥ 80° bin in Fig. 4 as 'anomalous results' is not explained; the reader should know why those galaxies behave differently and whether the main conclusions depend on their removal.
  2. [Table 2] The statement that Δ1PA and Δ2PA are 'essentially uncorrelated' is not fully supported by the table: several rows show r12√Ni values near or above 2 (e.g., i < 30° box: 2.58; 60°–70°: 2.82), which indicate correlations that are not negligible relative to 1/√Ni. The text acknowledges 'finite correlations slightly away from zero' but the earlier claim is too strong.
  3. [§3, Eq. (8) and (10)] The fitted coefficients in Eqs. (8) and (10) are presented without uncertainties or goodness-of-fit information, making it difficult to judge whether the claimed trends are significant.
  4. [Figure 2] The cross-checks with Graham et al. (2018) and Pilyugin et al. (2019) are described only qualitatively; a quantitative comparison (e.g., median offset and scatter) would be more informative.
  5. [Keywords] The keywords list 'white dwarfs, mass-radius relation, Chandrasekhar', which appears unrelated to the paper's content and should be corrected.
  6. [Throughout] There are typographical issues such as 'MaNGRA' in the Fig. 4 caption and 'anomous reviewer' in the acknowledgments; these should be fixed in revision.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular derivation: the one-percent PA-scatter result is measured directly from MaNGA data, while the load-bearing κ-proxy assumption is an openly stated conditional premise rather than a circular reduction.

full rationale

The paper's central statistical result — that scatter in-the-mean σ/√N of the three position angles reaches one-percent levels in MaNGA sub-samples — is computed directly from public MaNGA DR17 data and external catalogs (MDLM-VAC, MPP-VAC, PCA-VAC), with cross-checks against Graham et al. (2018) and Pilyugin et al. (2019). No fitted parameter is repackaged as a prediction: Eq. (10) is a fit to the measured PA scatter itself, not to a stacked rotation curve. The bridge to the cosmological prospect is Eq. (2), SE = √(κ²σ²+···)/√N, with κ introduced in Eq. (7) but never measured; the paper itself states this limitation in Section 3 ('A full account of this contribution to the total noise budget requires measuring κ in (2) by varying the control parameter θ') and in Section 4 ('provided that the present scatter in PAs provides an effective proxy for any additional sources of noise and uncertainty'). That is an explicitly conditional, unvalidated assumption about the noise budget, not a circular identification of the output with the input. The adS/C0-transition and Eq. (12) are taken from van Putten's prior work, but they are used to frame the outlook and motivate future stacking, not to construct the PA-scatter measurement; the one-percent scatter result is data-driven and independently checkable. Because the self-citations are present but not load-bearing for the measured quantity, the appropriate score is low.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

No new physical entities are postulated. The paper's central contribution is the empirical scatter measurement; the physical framework (a_dS, a0, C0-transition) is imported from prior work by the same group and functions as an assumed background, not as something derived here. The only fitted numbers are descriptive polynomial coefficients for scatter versus theta.

free parameters (1)
  • Empirical polynomial coefficients for sigma/sqrt(N) vs theta (Eqs. 8 and 10) = 0.104, 0.038, -5.3e-4; 0.244, 0.041, -2.4e-4; 0.625, 0.031
    Quadratic and linear fits to the measured scatter as a function of the PA-consistency cut theta. These are descriptive summaries of the data, not inputs to a predictive model; the one-percent claim is read from the data itself.
assumptions (6)
  • standard math Standard error of the mean of independent samples scales as sigma/sqrt(N)
    Used throughout Sec. 3 to define scatter in-the-mean; assumes Gaussianity and independence of the PA measurements.
  • domain assumption The standard error of ensemble-averaged observables follows SE = sqrt(kappa^2 sigma^2 + ...)/sqrt(N) with kappa of order unity (Eq. 2)
    Invoked in Sec. 1 and Sec. 3 as regular propagation of uncertainty; kappa is defined in Eq. (7) but never measured, so the one-percent lower-bound claim depends on an assumed proportionality.
  • ad hoc to paper PA scatter is an effective proxy for the total noise budget of stacked rotation curves
    Stated explicitly in Sec. 4: 'provided that the present scatter in PAs provides an effective proxy for any additional sources of noise and uncertainty.' This is the load-bearing bridge from the measured PA statistics to the cosmological prospect.
  • domain assumption The de Sitter scale a_dS = cH marks a C0-transition in galaxy dynamics, and a0 relates to cosmology via Eq. (12)
    Taken from van Putten (2017a, 2018, 2024a, 2024b, 2025); not derived or tested in this paper, only used to motivate the outlook.
  • domain assumption Sample selection (P_LTG>0.5, T-Type>0, VC=3, VF=0, DAP quality flags, single-component Sersic, PCAVAC membership) yields an unbiased spiral sample
    Described in Sec. 2; the successive downselection from 5125 to 4053 to 3101 galaxies introduces potential selection effects that are not quantified.
  • domain assumption Delta1PA and Delta2PA are statistically independent, so sigma_b = sqrt(sigma_1^2 + sigma_2^2)
    Justified by Pearson coefficients in Table 2, some of which exceed 2/sqrt(N) (e.g., 2.58 for i<30 degrees, 2.82 for 60-70 degrees), so independence is approximate.

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Cite this review

Pith. "Pith review of Prospects for high-resolution probes of galaxy dynamics tracing background cosmology in MaNGA." pith.science (2026). https://pith.science/paper/FCLAB4HS

@misc{pith2026250111882,
  author       = {Pith},
  title        = {Pith review of: Prospects for high-resolution probes of galaxy dynamics tracing background cosmology in MaNGA},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/FCLAB4HS}},
  note         = {Machine review of arXiv:2501.11882}
}
abstract

Large-$N$ galaxy surveys offer unprecedented opportunities to probe weak gravitation in galaxy dynamics that may contain correlations tracing background cosmology. Of particular interest is the potential of finite sensitivities to the background de Sitter scale of acceleration $a_{dS}=cH$, where $H$ is the Hubble parameter and $c$ is the velocity of light. At sufficiently large $N$, this is possibly probed by ensemble-averaged ("stacked") rotation curves (RCs) at resolutions on par with present estimates of the Hubble parameter $H_0$. Here, we consider the prospect for studies using the large $N$ Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) at APO survey. In a first and preliminary step, we consider unbiased control of sub-sample size by consistency in the three Position Angles, $\theta$ , from photometry and velocity fields of gas and stars by spectroscopy within $30^\circ$. In sub-samples of size $N=N_i(\theta)$, the scatter in-the-mean $\sigma/\sqrt{N}$ is found to reach one percent levels, differentiated over inclination angle $i$ and $\theta$. In regular propagation of uncertainties, this scatter contributes $\kappa\sigma/\sqrt{N}$ to the standard error in-the-mean to the observable, where $\kappa$ is determined by the choice of observables. As a lower bound to scatter in stacked RCs, MaNGA hereby appears promising for high-resolution analysis of sensitivity to RCs to background cosmology, notably across a sharp $C^0$-transition (van Putten 2018) of Newtonian to anomalous dynamics across $a_{dS}$ and, further out, the baryonic Tully-Fisher relation. In turn, these markers provide a novel measurement of cosmological parameters.

Figures

Figures reproduced from arXiv: 2501.11882 by the authors.

Figure 1
Figure 1. Photometric and spectroscopic data of a MaNGA galaxy, 8134-12702 MaNGA galaxy 8134-12702. Top left: SDSS photometric image. Top right: [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. (Left panels.) Cross-check of our PAs with PAs,Graham from Graham et al. (2018), for 934 galaxies in our sample ( [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. The 2D-distribution of ∆1PA in (3) in the velocity fields of gas and stars (horizontal axis) and ∆2PA in (4) between the PA in photometry and the mean of the two PAs in velocity fields (vertical axis). The distribution is largely Gaussian within ±30◦ except for some excess in tails. The top and rightmost plot shows the number distributions versus the control parameter θ according to (3) and (4), further showing the … view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Overview of scatter in-the-mean σ/ √ N of the three PAs in MaNGA over i < 80◦ based on [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]

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