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Classical Milky Way satellites show tidal features that MOND predicts and cold dark matter cannot.

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2026-07-11 06:43 UTC pith:F24K2HCU

load-bearing objection Clean pericentric η ranking for the classical satellites that matches observed disturbance in MOND and not in CDM; the soft spot is imported thresholds, not the ranking itself. the 3 major comments →

arxiv 2607.05502 v1 pith:F24K2HCU submitted 2026-07-06 astro-ph.GA

The tidal features of the classical Milky Way satellites: Expected in MOND but inconsistent with cold dark matter models

Elena Asencio , Indranil Banik , Pavel Kroupa This is my paper
classification astro-ph.GA
keywords MONDtidal susceptibilityclassical satellitesMilky Way dwarfsexternal field effectcold dark mattertidal featuresvelocity dispersion
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.

Most of the classical Milky Way satellites show clear signs of tidal disturbance: elongated shapes, outer stellar halos, substructure, and in some cases elevated velocity dispersions. Cold dark matter models surround those dwarfs with massive protective dark-matter halos, so their half-mass radii should sit well inside their tidal radii at pericentre and the systems should be resilient. This paper calculates that same tidal susceptibility ratio in both frameworks and finds the opposite for MOND: once the external-field effect is included, most classical satellites are expected to be at least mildly disturbed, and the three most susceptible (Draco, Ursa Minor, Sextans) lie near or above the instability threshold. The observed morphological and kinematic features line up with those MOND predictions, while remaining unexplained in the dark-matter picture. The result therefore offers a single dynamical reason why the satellites look disturbed and why some of them appear too hot for their baryonic masses.

Core claim

Comparing half-mass radius to theoretical tidal radius at pericentre shows that most classical satellites have tidal susceptibility η_MOND ≳ 0.4 (and Draco, Ursa Minor and Sextans near or above ~1), so they are expected to be tidally perturbed in MOND and their observed tails, ellipticity, outer excesses and elevated dispersions match those expectations; the same satellites remain resilient (η_CDM ≤ 0.3) under cold dark matter.

What carries the argument

Tidal susceptibility η ≡ r_h,3D / r_tid evaluated at pericentre, with the MOND tidal radius incorporating the external-field effect that weakens the satellite’s self-gravity near the Milky Way.

Load-bearing premise

The thresholds that turn a given η into observable radius growth, ellipticity and velocity-dispersion boost are taken from earlier N-body runs of more massive Fornax-cluster dwarfs and are assumed to transfer to the lower-mass classical satellites.

What would settle it

Dedicated MOND N-body simulations of each classical satellite that start from its observed stellar mass, size and orbit and either recover the measured ellipticity, outer excess and velocity dispersion or fail to do so.

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

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 / 4 minor

Summary. The paper computes the tidal susceptibility η ≡ r_h,3D / r_tid at pericentre for the eight classical Milky Way satellites (excluding Sagittarius and the Magellanic Clouds) in both CDM and MOND. Using published distances, proper motions, stellar masses and velocity dispersions together with the QUMOND tidal-radius formula (Eq. 8) and a dynamical M⋆–M_DM relation (Eq. 7), it finds η_CDM ≤ 0.3 (resilient) while η_MOND ≳ 0.4 for all but Leo II (and η_MOND ≳ 0.8 for Draco, Ursa Minor and Sextans). These rankings are then compared with observed morphological and kinematic signatures (King radii, BTFR residuals, ellipticities, extra-tidal stars) and with the disturbance thresholds previously calibrated on MOND N-body runs, concluding that the observed tidal features are expected in MOND but inconsistent with CDM.

Significance. If the ranking and the mapping from η to observable disturbance hold, the work supplies a quantitative, falsifiable challenge to CDM for the best-studied Local Group dwarfs and simultaneously offers a natural explanation for both their tidal morphology and the elevated velocity dispersions of the most susceptible systems. Strengths include fully transparent orbital integrations with error propagation, explicit tables of η and r_tid (Tables 3–5), a conservative dynamical DM-fraction choice that still leaves CDM resilient, and an open discussion of alternative mass estimates and of the Júlio et al. (2025) analysis. The paper therefore constitutes a useful, data-driven contribution to the ongoing Local Group test of gravity models.

major comments (3)
  1. [Sections 4.1, 5 and Appendix A] Sections 4.1, 5 and Appendix A: the quantitative claims of “good agreement” rest on the η thresholds (η_MOND ≳ 0.4 for stripping/ellipticity enhancement; η_MOND ≳ 1 for σ_v enhancement and instability) and the radial-oscillation behaviour taken from the higher-mass Fornax-cluster N-body suite of Asencio et al. (2022). The paper itself notes that e, g_ratio and t_peri also control the response and that dedicated simulations are still required; without a quantitative assessment of how those thresholds shift for the lower-mass, lower-acceleration classical satellites, the morphological and BTFR comparisons remain only directionally supportive rather than confirmatory.
  2. [Section 5.1, Fig. 2] Section 5.1 and Fig. 2: Fornax is the only object whose nominal Δr_tid is inconsistent with the expected near-zero expansion, although the large uncertainty on r_tid,MOND still allows consistency at 1σ. Because Fornax is the most massive classical satellite and the only one with a published dedicated MOND simulation (Bílek & Zhao 2025), this mild tension should be quantified more carefully (or shown to be resolved by the globular-cluster interactions already discussed) before the overall “good agreement” statement is retained at the present strength.
  3. [Section 3.1, Eqs. 5 and 8] Section 3.1 (Eqs. 5 and 8) and the comparison paragraph after Eq. 8: the Newtonian and MOND tidal radii are defined along different principal axes of the Roche lobe (r1 versus r2). The paper correctly notes that a factor 3/2 must be applied for direct numerical comparison, yet the subsequent discussion of η_CDM versus η_MOND and of the King-radius residuals does not consistently apply or propagate this geometric factor. Because the factor is of the same order as several of the reported η differences, it should be included (or shown to be negligible) in the tabulated values and in the figures.
minor comments (4)
  1. [Table 1] Table 1 caption: the Plummer deprojection formula is written r_h,3D = r_h / √(4^{1/3}-1); the conventional factor is 1/√(2^{2/3}-1) ≈ 1.3. Clarify which convention is used and whether it affects the subsequent η values.
  2. [Section 2] Section 2: the solar motion (U,V,W) = (14.1,14.6,6.9) km s^{-1} is taken from Francis & Anderson (2014); a brief note on sensitivity to the more commonly adopted Schönrich et al. (2010) values would help readers assess robustness of the pericentre distances.
  3. [Fig. 1] Fig. 1 and the accompanying text: the horizontal blue line at η_MOND ≈ 0.4 is described as the onset of both ellipticity enhancement and tidal stripping, yet the Asencio et al. (2022) suite only directly constrains the former. A short clarifying sentence would avoid conflating the two thresholds.
  4. [Appendix C] Appendix C: the isophote panels are useful but the figure captions do not uniformly state the source of the King radius over-plotted on each image; adding that information would make the visual comparison self-contained.

Circularity Check

3 steps flagged

Partial circularity: load-bearing η–disturbance thresholds and radial/σ_v/ellipticity responses are imported from the authors’ own 2022 N-body suite without re-derivation; observational ranking and CDM comparison remain independent.

specific steps
  1. self citation load bearing [Section 4.1 / Appendix A (reproducing Asencio et al. 2022 fig. 13)]
    "Since Asencio et al. (2022) presented their results in terms of the dwarfs’ η_MOND values—as in this study—we mainly focus on their simulations for our analysis. The results of their simulations are concisely displayed in their fig. 13. For an easier comparison, we have reproduced their fig. 13 in Appendix A. … The simulations of Asencio et al. (2022) estimate that the tidal susceptibility threshold at which a dwarf becomes unstable is η_MOND > 1.0 +0.0 −0.3."

    The quantitative thresholds that convert the paper’s computed η_MOND values into the claim ‘expected to be tidally perturbed / unstable / σ_v-enhanced’ are taken from the authors’ own prior N-body suite. No independent derivation or external calibration of those thresholds is supplied; the present paper simply imports them and maps the classical satellites onto them.

  2. self citation load bearing [Section 4.1.1–4.1.3 and Section 5 (application of thresholds)]
    "Therefore, according to this model, only Ursa Minor, and possibly Draco and Sextans, should experience an enhancement of their σ_v with respect to tidally unperturbed dwarfs (see Fig. 1). … The squashing effect, i.e. the increase in their ellipticity, can already become appreciable at η_MOND ≈ 0.4 … From Bílek & Zhao (2025), we can infer that Fornax-like dwarfs (η_MOND ≈ 0.4) should already be tidally susceptible enough to experience tidal stripping in MOND."

    The statements that η_MOND ≳ 0.4 produces ellipticity enhancement and stripping, and that η_MOND ≳ 1 produces σ_v enhancement, are not re-derived; they are the direct application of the Asencio et al. (2022) thresholds (with a secondary Bílek & Zhao 2025 citation for stripping). The ‘good agreement with MOND expectations’ claim therefore rests on those self-sourced thresholds.

  3. self citation load bearing [Section 3.1 (Eq. 7) and Section 6.2]
    "This led to the following M⋆ − M_DM relation (eq. 1 in Asencio et al. 2025): log10(M_DM/M⋆ + 1) = 4.089 − 0.396 log10(M⋆/M⊙). … Therefore, our nominal total dwarf mass (M_tot,CDM) for the CDM paradigm was obtained under the assumption of a Newtonian gravitational law and of a DM mass fraction consistent with that of isolated dwarf galaxies in the Local Group."

    The M⋆–M_DM relation used for the nominal CDM η values is taken from the authors’ own prior work (Asencio et al. 2022/2025). While the paper also checks the more conservative M_dyn choice (Table 5) and finds CDM still resilient, the primary CDM comparison that appears in the abstract and conclusions uses this self-sourced mass–mass relation.

full rationale

The paper’s central claim is that classical MW satellites have η_MOND ≳ 0.4 (and three near/above the instability threshold) so their observed tidal features match MOND, while η_CDM ≤ 0.3 implies resilience. The ranking itself (Tables 3–4) is computed from independent observational inputs (Pace et al. 2022, McConnachie & Venn 2020, published King radii) plus the QUMOND tidal-radius formula (Eq. 8) and the dynamical M⋆–MDM relation (Eq. 7). That part is not circular. What is load-bearing and self-sourced is the mapping from those η values onto expected morphological/kinematic responses: the thresholds η_MOND ≳ 0.4 for stripping/ellipticity and η_MOND ≳ 1 for σ_v enhancement/instability, plus the radial-oscillation behaviour for e ≳ 0.3, are taken directly from Asencio et al. (2022) fig. 13 (reproduced as Appendix A) without new derivation or external calibration. The paper itself notes that e, g_ratio and t_peri also matter and that dedicated simulations are still required. Because the observational comparison and the CDM side remain independent, the circularity is partial (score 4) rather than definitional.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The calculation rests on standard MOND ingredients (a0, simple interpolating function, EFE), a fixed MW baryonic mass, a mass-to-light ratio of 2, and the transfer of η-thresholds from earlier cluster-scale simulations. No new free parameters are fitted to the classical-satellite data themselves; the CDM comparison uses an empirical M⋆–MDM relation calibrated on isolated Local-Group dwarfs rather than a simulation abundance-matching relation.

free parameters (4)
  • a0
    Fixed to the conventional 1.2e-10 m s^-2; not re-fitted here but the entire MOND boost depends on it.
  • MW baryonic mass Mb,MW
    Set to 6.7e10 M⊙ (Banik & Zhao 2018b); controls the external field and therefore every r_tid,MOND.
  • stellar mass-to-light ratio
    Fixed at 2 (Telford et al. 2020) to convert MV to M⋆; directly scales every dwarf’s self-gravity.
  • η instability threshold
    Taken as 1.0 +0.0/-0.3 from Asencio et al. 2022 simulations; used to decide which dwarfs should show elevated σv.
axioms (4)
  • domain assumption QUMOND with the simple interpolating function correctly describes the Galactic potential and the internal dynamics of the satellites once the EFE is included.
    Invoked throughout §§2–3 and Eqs. 1–3, 8; the entire MOND column of Tables 3–4 rests on it.
  • domain assumption The dynamical M⋆–MDM relation measured for isolated Local-Group dwarfs (Asencio et al. 2022 fig. 16 / 2025 erratum) is the appropriate CDM mass for classical satellites.
    Used to construct Mtot,CDM and therefore η_CDM (Eq. 7, Table 3); the paper also tests the more conservative Mdyn case.
  • ad hoc to paper η thresholds and radial-oscillation behaviour calibrated on Fornax-cluster-mass N-body runs apply to classical MW satellites.
    Explicitly adopted in §4.1 and Appendix A; the paper notes that dedicated lower-mass simulations are still needed.
  • domain assumption Observed morphological and kinematic features (King radii, ellipticities, extra-tidal stars, BTFR outliers) are primarily tidal rather than merger- or feedback-driven.
    Underpins the entire comparison in §5; alternative explanations are discussed but not quantitatively modelled.

pith-pipeline@v1.1.0-grok45 · 40011 in / 3193 out tokens · 29355 ms · 2026-07-11T06:43:17.899027+00:00 · methodology

0 comments
read the original abstract

Most classical satellites of the Milky Way are known to display signs of tidal disturbance (e.g. tidal tails, substructures, and distorted shapes). This cannot be explained by the standard model of cosmology due to its prediction that the dark matter haloes of the classical satellites confer them with very strong self-gravity and make them resilient to the Milky Way's gravitational tides. In this work, we estimate the tidal susceptibility of the classical satellites by comparing their half-mass radius with their theoretical tidal radius at pericentre in both the standard model and in the Milgromian dynamics (MOND) model. With this approach, we demonstrate that most classical satellites are expected to be tidally perturbed in MOND, so their observed tidal features are generally in good agreement with MOND expectations. Since gravitational tides can also enhance the velocity dispersion of the satellites, we argue that MOND can plausibly explain the unusually high velocity dispersions reported for some of the classical satellites.

Figures

Figures reproduced from arXiv: 2607.05502 by Elena Asencio, Indranil Banik, Pavel Kroupa.

Figure 13
Figure 13. Figure 13: fig. 13. For an easier comparison, we have reproduced their [PITH_FULL_IMAGE:figures/full_fig_p005_13.png] view at source ↗
Figure 1
Figure 1. Figure 1: summarises the predicted properties of the con￾sidered classical satellites in the MOND model. According to this, the radius of Draco, Ursa Minor, Leo I, Leo II, Sculptor, and Sextans oscillated throughout their trajec￾tory. Among these, only Ursa Minor, and possibly Draco and Sextans, are in the unstable regime, which means that they are not expected to recover their previous apocen￾tric rh,3D value in th… view at source ↗
Figure 2
Figure 2. Figure 2: Upper panel: Comparison of the observed King tidal [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Circular velocity and stellar mass of the classical [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Ellipticity of the classical satellites ( [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗

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