MIGHTEE-HI / LADUMA: Investigating the link between baryons and dynamics with 130 resolved HI-selected galaxies

Abhisek Mohapatra; Anastasia A. Ponomareva; Andreea A V\u{a}r\u{a}\c{s}teanu; Andrew J. Baker; Danail Obreschkow; Harry Desmond; Ian Heywood; Kristine Spekkens; Laurent Chemin; Maarten Baes

REVIEW 3 major objections 5 minor 172 references

MIGHTEE-HI / LADUMA: Investigating the link between baryons and dynamics with 130 resolved HI-selected galaxies

T0 review · 3 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read With 130 HI-selected galaxies out to z≈0.09, the radial acceleration relation remains tight, and the apparent baryonic Tully-Fisher zero-point evolution is mostly selection bias.

desk verdict The largest homogeneous HI-selected RAR/bTFR sample beyond z=0, with a clean central measurement but a known 5-sigma a0 systematic that the abstract understates; worth serious review. read the letter →

arxiv 2608.03576 v1 pith:VV6SVPVY submitted 2026-08-04 astro-ph.GA

Andreea A Vărăşteanu , Matt J. Jarvis , Harry Desmond , Anastasia A. Ponomareva , Tariq Yasin , Michalina Maksymowicz-Maciata , Ian Heywood , Natasha Maddox

show 10 more authors

Andrew J. Baker Laurent Chemin Martin Meyer Danail Obreschkow Kristine Spekkens Natalia Stylianou Rohan G. Varadaraj Marcin Glowacki Maarten Baes Abhisek Mohapatra

This is my paper · ORCID

classification astro-ph.GA

keywords radialaccelerationrelationbaryonicTully-FisherMONDinterpolatingfunctionHI-selectedgalaxiesMIGHTEE-HILADUMAredshiftevolutionselectionbias

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 sets out to measure how closely galaxy rotation tracks the mass of visible baryons using 130 galaxies selected purely by their neutral-hydrogen emission, observed with MeerKAT in the MIGHTEE and LADUMA surveys out to z≈0.09. It claims the radial acceleration relation (RAR) holds out to this redshift with an acceleration scale $a_0=(1.50\pm0.05)\times10^{-10}\,\mathrm{m\,s^{-2}}$ and an intrinsic scatter of $0.096\pm0.006$ dex, matching local results. It further claims the MOND interpolating-function shape parameter is $\delta=4.10^{+1.4}_{-0.68}$, consistent with Solar System gravitational constraints and a null Wide Binary Test, and that the apparent redshift evolution of the baryonic Tully-Fisher (bTFR) zero-point is mostly a selection artefact: the forward fit shows an $8.7\sigma$ trend, which drops to $3.4\sigma$ when the fit conditions on baryonic mass. If true, these results show that the tight baryon-dynamics coupling extends beyond the local Universe and that reported evolution of scaling relations needs re-examination for selection bias.

What carries the argument

The central object is the radial acceleration relation $g_{\rm obs}=\mathcal{F}(g_{\rm bar})$, linking the observed centripetal acceleration to the acceleration predicted from the baryonic mass distribution alone, together with its deep-MOND limit $V_f^4\propto G M_{\rm bar} a_0$, which yields the baryonic Tully-Fisher relation. The analysis is carried by three devices: resolved SED fitting that lets the stellar mass-to-light ratio vary with radius, 3D Barolo tilted-ring fits to the HI data cubes that give rotation curves and gas surface densities, and the Roxy marginalised normal regression that handles uncertainties in both coordinates and intrinsic scatter. For the redshift-evolution claim, the decisive step is fitting the bTFR in the inverse direction, conditioning on $M_{\rm bar}$ rather than $V_{\rm out}$, because the HI flux selection acts on $M_{\rm HI}$ and hence on $M_{\rm bar}$.

What would settle it

A definitive check is to repeat the bTFR analysis on a sample selected by stellar mass or with a fully characterised HI selection function, or to split the present sample into redshift bins with matched HI-mass distributions and test whether the inverse-fit zero-point shift persists; a surviving 3.4σ signal under complete selection modelling would indicate genuine evolution, while a vanishing signal would confirm that the forward 8.7σ is selection bias.

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Extended reading notes

Core claim

Using 130 HI-selected galaxies with resolved HI rotation curves and resolved baryonic mass profiles, the paper measures the radial acceleration relation and the baryonic Tully-Fisher relation out to z≈0.09. The RAR is tight: $a_0=(1.50\pm0.05)\times10^{-10}\,\mathrm{m\,s^{-2}}$ and intrinsic scatter $0.096\pm0.006$ dex with direct-aperture photometry, and the acceleration scale is robust to the photometric pipeline. The fiducial inverse bTFR fit gives a slope of $0.27\pm0.01$ (forward-equivalent $3.72\pm0.16$) with an orthogonal scatter of about $0.05$ dex. Fitting the $\delta$-family of MOND interpolating functions returns $\delta=4.10^{+1.4}_{-0.68}$, a steep transition that is consistent with Cassini quadrupole and wide-binary null results, unlike the SPARC-preferred $\delta\approx1$. The paper finds no significant redshift evolution of the RAR acceleration scale ($a_1=-1.6\pm2.3\times10^{-10}\,\mathrm{m\,s^{-2}}$), while the bTFR zero-point shows an apparent evolution that depends strongly on fit direction: $8.7\sigma$ in the forward fit, reduced to $3.4\sigma$ in the inverse fit conditioning on $M_{\rm bar}$, within about $2\sigma$ of the RAR constraint. The paper interprets this as the signature of HI flux selection biasing the forward fit.

Load-bearing premise

The load-bearing premise is that conditioning the bTFR fit on baryonic mass leaves only a small residual selection bias, so the surviving 3.4σ inverse-fit signal is not genuine evolution; if the HI flux selection also correlates with rotation velocity, rotation-curve extent, or data quality that tracks redshift, the residual signal could be real.

Editorial extensions

If this is right

The RAR's intrinsic scatter near 0.1 dex and acceleration scale matching local values imply the baryon-dynamics coupling is already in place by z≈0.09, not just at z=0.
A MOND interpolating-function shape of approximately 4.1 would reconcile galaxy-scale RAR data with Solar System and wide-binary constraints under the MOND interpretation, easing the reported tension with SPARC.
Apparent bTFR zero-point evolution measured with forward fits in HI flux-limited samples should be treated with caution; inverse fits conditioning on $M_{\rm bar}$ are a necessary safeguard.
Future claims of bTFR redshift evolution from HI-selected samples must model the selection function, since conditioning on $M_{\rm bar}$ mitigates but does not fully remove the bias.
Under the fiducial inverse fit, the RAR and bTFR remain mutually consistent within about $2\sigma$ over the redshift range probed, so genuine evolution is neither required nor excluded by the data.

Reading between the lines

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

Not claimed in the paper, but following from its results: if $\delta\approx4.1$ is the true MOND transition shape, the Solar System quadrupole should sit near its current upper bound and wide-binary MOND signals should remain undetected, sharpening the MOND programme's testable predictions.
The paper's selection-bias argument generalises to other flux-limited HI samples: scaling relations that place a selection-correlated mass on the ordinate should show spurious redshift evolution, so inverse fits or relations with that quantity on the abscissa are safer diagnostics. Re-running the analysis on optical emission-line samples with an explicit HI-equivalent selection model would test th
If a future sample with a fully characterised selection function still recovers the $3.4\sigma$ inverse-fit signal, that would point to a mild genuine evolution of the baryon-dynamics coupling, possibly tied to gas-fraction evolution rather than to MOND's acceleration scale.
The paper's comparison with SPARC anchoring suggests sample-specific systematics dominate once a z≈0 anchor is added; extending the homogeneous HI-selected analysis to a longer redshift baseline with one consistent baryonic model is the direct way to separate those systematics from cosmology.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

You should look at this one. It is the first RAR/bTFR measurement on a large, homogeneous HI-selected sample beyond z≈0: 130 galaxies from MIGHTEE and LADUMA, with resolved rotation curves and resolved baryonic mass profiles from SED fitting. That alone is a real step forward. The paper does several things well. Two independent photometry pipelines give a0 consistent at the 0.1-0.3 sigma level, which is genuinely reassuring. The intrinsic scatter is statically nonzero and in line with local values. The delta-family fit yielding delta~4.1, consistent with Solar System and wide-binary constraints, is an interesting and honest result, though the posterior is broad. And the forward-vs-inverse bTFR comparison is a clean demonstration of selection bias, with the forward 8.7-sigma evolution dropping to 3.4-sigma in the inverse fit.

The soft spots are real but mostly acknowledged in the text. The big one is Table 2: splitting by photometric consistency gives a0 = 1.80±0.08 for the 61 'well-behaved' galaxies and 1.31±0.06 for the 69 'less well-behaved' ones, a 5-sigma offset. The paper says the RAR's tightness is robust even when a0 is not, which is fair, but the abstract quotes a0 = 1.50±0.05 without a systematic term. That is misleading. The reader's stress-test is right: this systematic should be in the headline or the claim softened. It matters because the delta-family inference and the a0-anchored bTFR evolution fits inherit this scale.

The second soft spot is the selection function. The paper conditions on Mbar to mitigate HI flux selection and is careful to say this 'mitigates but does not fully remove' the bias. But the residual 3.4-sigma inverse-fit evolution could still be genuine, or could be a residual of unmodeled selection on Vout, rotation-curve extent, or data quality. I don't think this kills the paper—the interpretation as selection is plausible and the evidence for it is decent—but it is not a closed case.

Minor: data availability says 'available on request' and no code is released. That is weak for a paper this method-heavy.

Verdict: the central RAR measurement is likely sound; the evolution conclusions are plausible but not definitive. I would send this to a serious referee, with a request that the authors add a systematic term to a0, model the selection function more explicitly, and release the data products. It deserves to be in the literature after revision.

Referee Report

3 major / 5 minor

Summary. This paper presents measurements of the baryonic Tully-Fisher relation (bTFR) and the radial acceleration relation (RAR) for 130 purely HI-selected galaxies from MIGHTEE and LADUMA out to z≈0.09. The authors derive resolved stellar mass profiles via SED fitting using two independent photometry pipelines (direct aperture photometry and Sérsic fits), combine these with 3D Barolo HI rotation curves, and fit the RAR and bTFR with the Roxy/MNR framework. The main results are a RAR acceleration scale a0=(1.50±0.05)×10^-10 m/s^2 with intrinsic scatter 0.096±0.006 dex; a delta-family MOND interpolating-function shape δ=4.10(+1.4,-0.68) reported as consistent with Solar System and wide-binary constraints; a bTFR inverse slope s'=0.27±0.01 with orthogonal scatter ≈0.05 dex; and a redshift-evolution analysis in which the bTFR zero-point evolution drops from an 8.7σ preference in the forward fit to 3.4σ in the inverse fit, interpreted as largely arising from HI flux selection.

Significance. If the results hold, this is the first RAR and bTFR measurement from a purely HI-selected sample beyond the local Universe with fully resolved baryonic mass profiles, and the inferred δ value would ameliorate the known tension between SPARC-based RAR fits and Solar System/wide-binary MOND constraints. The paper has notable strengths: it uses two independent photometric pipelines, explicitly examines systematic effects through a well-behaved/less well-behaved sample split, applies an inverse bTFR fit to mitigate selection, and makes use of publicly available fitting and analysis packages. The central demonstration that selection effects and baryonic modeling choices, rather than statistics alone, control apparent redshift evolution of dynamical scaling relations is an important and timely contribution.

major comments (3)

[§4.2, Table 2] The headline value a0=(1.50±0.05)×10^-10 m/s^2 is quoted in the abstract and Section 5(i) without an accompanying systematic term. The authors' own Table 2 shows that the well-behaved and less well-behaved subsamples yield a0=(1.80±0.08) and (1.31±0.06)×10^-10 m/s^2, a ~5σ offset with comparable intrinsic scatters. Because a0 enters the δ-family inference (Section 4.3) and the a0-anchored bTFR evolution fits (Eq. 17), the quoted statistical error understates the model uncertainty in the central claim. The paper should report a0 with a systematic term derived from the pipeline split (for example, half the difference of the subsample values added in quadrature) and should state whether the no-evolution RAR result is robust when the evolution fit is repeated separately for the two subsamples, since photometric consistency could correlate with redshift or with the number of resolved rings.
[§4.6.2, Eq. (17)] The interpretation that the bTFR evolution is largely selection bias rests on the inverse fit reducing the evolution preference from 8.7σ to 3.4σ. The text correctly says that conditioning on Mbar mitigates but does not fully remove the bias, yet the abstract's 'within ≈2σ of the RAR evolution constraint' and conclusion (vi) present the residual 3.4σ signal as a selection artifact. Because the HI selection function is not modeled, and because redshift correlates with M_HI, M*, and the number of resolved rings (Figs. 14–15), the residual could be genuine evolution. I recommend adding a synthetic-selection or forward-model test that quantifies how much of the measured a1 in the inverse fit is removed under a realistic selection function, or, failing that, explicitly stating in the abstract and conclusions that the data cannot distinguish residual selection from moderate evolution.
[§4.1, Eq. (10)] The RAR fit treats all 476 radial bins as independent data points. Rotation-curve rings are spaced at half the beam and the baryonic profiles are smoothed, so adjacent points within a galaxy are likely correlated. This can bias the quoted intrinsic scatter sigma_int=0.096±0.006 dex and the formal uncertainties on a0. The paper should either model within-galaxy covariance (for example through resampling or a per-galaxy random effect) or demonstrate, such as by fitting a single point per galaxy, that the conclusions are unchanged. This is particularly relevant to the claim that the intrinsic scatter is clearly non-zero statistically.

minor comments (5)

[§4.1 vs §5(ii)] Section 4.1 states the two photometric pipelines agree on a0 at the 0.1σ level, while Section 5(ii) says 0.3σ; the numbers should be made consistent.
[Table 2] The COSMOS reference intrinsic scatter is listed as 0.045±0.002 dex in Table 2 but quoted as 0.045±0.022 dex in Section 4.1; the table entry appears to be a typo.
[§2.4] The statement that excluding galaxies with foreground stellar contaminants 'does not bias our Hi-selected sample in any way' is too strong; masking decisions can in principle correlate with galaxy properties. Please soften the claim or provide justification.
[§4.4, Table 3] The text reports the vertical intrinsic scatter as 0.054±0.011 dex, while Table 3 gives 0.054±0.006 dex; also, the 'direct-equivalent zero-point I=2.39±0.33' is actually -I/s' in Eq. (13), so the notation should be clarified to avoid confusion with the fitted intercept.
[Fig. 7 caption] The caption says a0=1.50×10^-10 for both panels, but the Sérsic-based fit gives a0=(1.48±0.04)×10^-10; the caption should indicate that the displayed curve is the fiducial fit rather than the Sérsic fit value.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the RAR and bTFR measurements are empirical fits, and the δ and evolution comparisons rely on independent external constraints.

full rationale

I walked the derivation chain and found no step in which a claimed prediction or first-principles result reduces by construction to its inputs. The RAR is measured by fitting the McGaugh et al. (2016) interpolating function (Eq. 10) and the δ-family (Eq. 11) directly to 130 galaxies' resolved acceleration data; the acceleration scale a0 and scatter are fitted parameters, not outputs of the model being tested. The inferred δ=4.10 is then compared with independent Cassini quadrupole (Park et al. 2026) and wide-binary (Banik et al. 2024) constraints; this is a genuine external benchmark, not a self-imported uniqueness claim. The bTFR redshift-evolution analysis fits a1 in Eq. 17 with a0 fixed from the RAR, but a1 is still constrained by the bTFR data themselves, and the paper additionally provides the MOND-independent power-law parametrisation of Eq. 18, which reaches the same qualitative conclusion (γ=9.1±3.0 vs γ_MOND≈+1.0). The comparison between the RAR-derived and bTFR-derived evolution is a consistency check between two fits to different projections of the data, not a definitional identity. The paper's own Table 2 shows that a0 shifts from 1.80±0.08 to 1.31±0.06 between 'well-behaved' and 'less well-behaved' baryonic-model subsamples; this is a systematic robustness concern, not circularity, and the text explicitly acknowledges that 'the tightness of the RAR is thus relatively robust to the details of the baryonic modelling, even when the a0 is not.' Self-citations (Vărăşteanu et al. 2025, Bartlett & Desmond 2023, Ponomareva et al. 2021/2026) are used for methodology and code, but the central analysis is recomputed here and does not depend on those papers for its conclusions. Against external benchmarks (SPARC, Cassini, wide binaries) the paper is self-contained, so no circularity score above zero is warranted.

Assumptions & free parameters 10 free parameters · 7 assumptions · 0 invented entities

The central claims rest on a small number of fitted parameters (a0, delta, scatters, slopes, evolution amplitudes) and on standard astrophysical modelling assumptions about disc geometry, molecular gas scaling, and the HI selection function. No new physical entities are introduced.

free parameters (10)

a0 (RAR acceleration scale, canonical IF) = 1.50 +/- 0.05 x 10^-10 m/s^2 (direct photometry)
Fitted via Roxy/MNR to the 130-galaxy RAR (Eq 10); sets the RAR normalisation.
a0 (delta-family) = 1.86 +/- 0.06 x 10^-10 m/s^2
Fitted jointly with delta using Eq 11; differs from canonical IF, showing degeneracy.
delta (MOND IF shape) = 4.10 (+1.4, -0.68)
Fitted to RAR with Eq 11; compared to Solar System and wide-binary constraints.
sigma_int_RAR = 0.096 +/- 0.006 dex (direct photometry)
Intrinsic scatter of RAR from Roxy.
bTFR inverse slope s' = 0.27 +/- 0.01
Slope of log10 Vout vs log10 Mbar (Eq 13); forward-equivalent 3.72 +/- 0.16.
bTFR intercept I = -0.65 +/- 0.11
Intercept of inverse bTFR (Eq 13).
bTFR vertical scatter sigma_V = 0.054 +/- 0.006 dex
Intrinsic vertical scatter in inverse bTFR fit.
RAR evolution a1 = -1.60 +/- 2.33 x 10^-10 m/s^2
Linear redshift evolution of a0 in Eq 14; consistent with zero.
bTFR evolution a1 (inverse) = -8.10 +/- 2.41 x 10^-10 m/s^2
Redshift evolution of bTFR zero-point under MOND-motivated model (Eq 17); 3.4 sigma from zero.
bTFR power-law evolution gamma = 9.06 +/- 3.02
MOND-independent zero-point evolution (Eq 18); 3.0 sigma from zero.

assumptions (7)

domain assumption The RAR interpolating function (Eq 10) or its delta-family (Eq 11) is the correct description of the baryon-dynamics link.
Both the a0 and delta inferences are made by fitting these empirical functions to the sample; a different functional form would change the results.
domain assumption Rotation curves trace the circular velocity (equilibrium discs; asymmetric drift negligible).
Eqs 8-9 derive g_obs from v_rot^2/r; the paper states asymmetric drift is small for most of the sample (Section 3.3.4).
domain assumption Molecular gas masses follow the Tacconi et al. (2018) depletion-time scaling relations, with mu_mol=0.07 for log M*/M_sun<9.
No direct CO data; this scaling enters Mbar and hence both the RAR gbar and bTFR mass (Section 3.3.3).
domain assumption Inclinations from G-band axis ratio with intrinsic thin-disc q0=0.
Used to deproject velocities (Eq 1); alternative q0 change inclinations by less than 5 degrees.
domain assumption The HI flux selection function is essentially monotonic in M_HI, so inverse fitting conditioned on Mbar reduces selection bias.
Foundation of the fiducial bTFR fit and the interpretation that the forward-fit 8.7 sigma evolution is spurious (Sections 4.4 and 4.6.2).
domain assumption Peculiar velocities are subdominant to recession velocities, so redshifts map to distances with small error.
Section 2.4; fewer than 6 percent of galaxies have z less than 0.02 and peculiar velocities near 300 km/s are subdominant.
domain assumption The stellar mass-to-light ratio varies radially and is recovered by resolved SED fitting with Bagpipes.
The RAR and bTFR baryonic masses rely on this; the paper tests constant versus varying M/L and finds different evolution signals (Table 4).

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Pith. "Pith review of MIGHTEE-HI / LADUMA: Investigating the link between baryons and dynamics with 130 resolved HI-selected galaxies." pith.science (2026). https://pith.science/paper/VV6SVPVY

@misc{pith2026260803576,
  author       = {Pith},
  title        = {Pith review of: MIGHTEE-HI / LADUMA: Investigating the link between baryons and dynamics with 130 resolved HI-selected galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VV6SVPVY}},
  note         = {Machine review of arXiv:2608.03576}
}

abstract

The baryonic Tully-Fisher relation (bTFR) and the radial acceleration relation (RAR) link the observed dynamics in galaxies to that expected from their baryonic mass distributions. The relations' small intrinsic scatters place strong constraints on galaxy formation models, dark matter properties and theories of modified dynamics, yet detailed measurements beyond the very local Universe remain limited. We use 130 purely HI-selected galaxies with resolved HI kinematics and baryonic mass profiles to measure the bTFR and RAR up to $z\approx0.09$. We measure a tight RAR with an acceleration scale $a_0=(1.50\pm0.05)\times10^{-10},{\rm m,s^{-2}}$ and an intrinsic scatter of $0.096\pm0.006$ dex, consistent with local results. We fit the bTFR in the `inverse' direction, conditioning on $M_{\rm bar}$ to mitigate HI flux-related selection effects, measuring a logarithmic slope of $0.27\pm0.01$ (corresponding to a forward slope of $3.72\pm0.16$), with vertical intrinsic scatter $\sigma_\perp\approx0.05$ dex. Fitting the general $\delta$-family of MOND interpolating functions to the RAR, we infer $\delta=4.10^{+1.4}_{-0.68}$, consistent with the value required by Solar System gravitational constraints and a null Wide Binary Test. We find no significant redshift evolution in the RAR acceleration scale for our pure HI-selected sample. However, the bTFR zero-point shows an apparent evolutionary trend that is strongly dependent on the fit direction: the traditional forward fit yields an $8.7\sigma$ preference for $z$ evolution, while for our fiducial inverse fit, this reduces to $3.4\sigma$, within $\approx2\sigma$ of the RAR evolution constraint. This suggests selection effects bias the forward fit; a careful consideration of such effects will be required in future endeavours to robustly measure the redshift evolution of dynamical scaling relations.

Figures

Figures reproduced from arXiv: 2608.03576 by the authors.

**Figure 1.** Distribution of physical properties for the galaxies in our sample. From top-left to bottom-right: redshifts, stellar masses, inclinations and effective radii in the near-infrared H band (1.65𝜇𝑚). 3 METHODS 3.1 Photometry To extract photometry across all 18 wavelengths from optical to farinfrared, contaminant sources must first be masked in each image. For this purpose, we developed a custom photometry workflow th… view at source ↗

**Figure 3.** Distribution of mass-to-light ratios (Υ★) in the 𝐾𝑠-band from the mass-to-light ratio posterior samples derived from SED fitting with Bagpipes. The sample has a median of 0.43+0.11 −0.10. the 𝐾𝑠-band surface brightness, both inclination corrected, derived from our fiducial non-parametric photometry [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

**Figure 5.** Rotation curves for our sample of 130 galaxies, colour coded by their gas fraction, fg = MHI/Mbar, with measurement uncertainties indicated by the shaded regions. 0 10 20 30 40 50 60 Radius [kpc] 10−1 100 101 ΣHI [M pc −2 ] 0.1 0.2 0.3 0.4 0.5 0.6 fgas [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗

Figures from the paper (10 more)

**Figure 6.** Figure 6: Hi mass surface densities for our sample of 130 galaxies, colourcoded by their gas fraction, fg = MHI/Mbar, with measurement uncertainties indicated by the shaded regions. 3.3.1 Stellar disc The morphologies in our sample are predominantly disc-dominated: most galaxie…

**Figure 7.** Figure 7: Left: The RAR for our sample of 130 late-type galaxies obtained for the direct photometry case, colour-coded by their resolved mass-to-light ratio in the 𝐾𝑠 band, Υ★,𝐾𝑠 [𝑀⊙/𝐿⊙,𝐾𝑠 ]. Right: The RAR with 𝑔bar obtained through Sérsic fits, colour-coded by their resolved m…

**Figure 8.** Figure 8: Left: Σstar comparison across all photometric annuli from the Sérsic fitting and direct photometry pipelines. Right: gbar comparison at all kinematically sampled radii. Both quantities are colour-coded by radius. The dashed black lines in both panels correspond to the …

**Figure 9.** Figure 9: Posterior distribution of the acceleration scale 𝑎0 and shape parameter 𝛿 from the fit of Equation 11 to our sample, and the Solar System quadrupole updated constraints (Park et al. 2026). The 2D contours correspond to 68% and 95% confidence intervals. nitude is desc…

**Figure 10.** Figure 10: Baryonic Tully Fisher relation for our sample of 130 galaxies extending up to 𝑧 ∼ 0.09, colour-coded by their number of resolution elements. The dashed lines overlaid on top show the bTFR at 𝑧 = 0 for SPARC galaxies (Lelli et al. 2019) and the bTFR for a subsample of…

**Figure 11.** Figure 11: The RAR for our sample of galaxies extending up to 𝑧 ∼ 0.09, colour-coded by their resolved mass-to-light ratio, with the outermost points (those used in the bTFR) shown as pink stars. this value is not directly comparable to the forward-equivalent slope implied by th…

**Figure 12.** Figure 12: Left: Posterior distributions of the parameters from the redshift-dependent fit to the RAR for the MIGHTEE+LADUMA sample (𝑎0, 𝑎1, 𝜎int). Right: Posterior distributions of the parameters from the bTFR redshift-dependent fit (conditioned on 𝑀bar; 𝑉out | 𝑀bar) for MIGHTE…

**Figure 13.** Figure 13: Posterior distributions of the parameters from the bTFR redshift-evolution fits (conditioned on 𝑀bar; 𝑉out | 𝑀bar) for the MIGHTEE+LADUMA sample. Left: zero-point evolution parametrised by 𝛾 (Equation 18). Right: slope evolution parametrised by 𝑠1. Contours correspond…

**Figure 14.** Figure 14: Vertical residuals about the non-evolving RAR (Δ log 𝑔obs|𝑔bar, orange) at the outermost ring, forward bTFR (Δ log 𝑀bar |𝑉out, blue), and the fiducial inverse bTFR (Δ log 𝑉out |𝑀bar, green), per galaxy, against redshift (left) and the Hi mass (right). The forward bTFR…

**Figure 15.** Figure 15: Total 𝐾𝑠-band stellar mass-to-light ratio Υ★,𝐾𝑠 (top left), atomic gas fraction 𝑀HI/𝑀★ (top right), stellar mass (bottom left), and Hi mass (bottom right) as a function of redshift for the MIGHTEE+LADUMA sample. Spearman coefficients are quoted in each panel. The tota…

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Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.

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