The galaxy-halo connection of disc galaxies over six orders of magnitude in stellar mass

Antonino Marasco; Claudia del P. Lagos; Gabriele Pezzulli; Jos\'e A. Benavides; Justin I. Read; Marcin Glowacki; Pavel E. Mancera Pi\~na; Stacy Kim

REVIEW 2 major objections 5 minor 2 cited by

The galaxy-halo connection of disc galaxies over six orders of magnitude in stellar mass

T0 review · 2 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Rotation curves of 49 disc galaxies reveal five 'baryon-deficient dwarfs' with stellar masses 20–60 times below the abundance-matching expectation for their haloes, a population current models do not produce.

desk verdict A genuinely useful sample paper whose two flashiest claims—baryon-deficient dwarfs and low-mass c200 deviations—are real possibilities but softer than the abstract makes them sound. read the letter →

arxiv 2505.22727 v3 pith:DAFKS72N submitted 2025-05-28 astro-ph.GA astro-ph.CO

Pavel E. Mancera Piña , Justin I. Read , Stacy Kim , Antonino Marasco , José A. Benavides , Marcin Glowacki , Gabriele Pezzulli , Claudia del P. Lagos This is my paper

classification astro-ph.GAastro-ph.CO PACS 98.62.-g98.62.Dm98.62.Gq

keywords galaxy-haloconnectiondwarfgalaxiesrotationcurvedecompositiondarkmatterhaloesbaryonretentionfractionabundancematchingcoreNFWhaloprofileHikinematics

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

Using rotation curves of 49 gas-rich disc galaxies spanning nearly six orders of magnitude in stellar mass, this paper builds a dynamical census of how baryons sit inside dark matter haloes. Its central finding is a population of five 'baryon-deficient dwarfs' (BDDs): galaxies whose stellar masses are roughly 20 to 60 times lower than abundance matching predicts at their inferred halo masses, with their cold gas likewise depleted relative to halo mass. Cold gas, by contrast, is tightly regulated: gas-rich galaxies hold about 4 per cent of the cosmic baryon fraction in gas across the whole halo mass range, while stellar content varies enormously at fixed halo mass, with some massive spirals retaining essentially all of their baryons. The paper argues the BDDs are unlikely to be artefacts, citing a check against an extrapolation-free halo speed and independent weak-lensing measurements, while noting that their halo masses carry large uncertainties. Because abundance matching, the DarkLight model, and the TNG50 and Simba simulations do not reproduce the BDDs or the full spread in baryon retention, the paper concludes that galaxy formation models need more stochastic baryon retention and more diverse feedback implementations.

What carries the argument

The argument is carried by rotation curve decomposition: each galaxy's observed circular speed $V_{\rm circ}$ is reproduced as the quadrature sum of stellar disc, bulge, gas (H\,I and H$_2$), and dark matter contributions. The halo is described by the coreNFW profile, a Navarro-Frenk-White profile modified to allow a constant-density core of size $r_c = \eta R_e$ with free parameters $M_{200}$, concentration $c_{200}$, and $\eta$; the gas disc's flared scale height is solved simultaneously from vertical hydrostatic equilibrium, so halo parameters, stellar mass-to-light ratios, and gas thickness come out self-consistently. The quantity that exposes the BDDs and the scatter is the baryon retention fraction $\tilde{f}_i = M_i / (f_{\rm bar,cosmic} M_{200})$ evaluated for the stellar, gas, and baryonic components. The comparison baselines — the abundance-matching relation, the semi-empirical DarkLight model, and the TNG50 and Simba hydrodynamical simulations — supply what 'expected' means against which the BDDs are defined.

What would settle it

Deep, wide-field Hi or CO mapping of the five baryon-deficient dwarfs (DDO 190, LVHIS 017, LVHIS 072, LVHIS 080, UGC 8508) to extend their rotation curves well beyond the current few-kiloparsec coverage. If the outer rotation curves turn over or flatten so that the fitted halo mass drops by the roughly 1 dex needed to reach the abundance-matching track, the BDD population dissolves into ordinary scatter; if the high circular speeds persist out to radii where the halo is directly probed, the population is confirmed.

Watch

Extended reading notes

Core claim

The paper's central claim is that the galaxy-halo connection in nearby disc galaxies is not a single efficiency curve but a broad, partly stochastic band. At fixed halo mass $M_{200}$, the stellar retention fraction $\tilde{f}_\ast = M_\ast / (f_{\rm bar,cosmic} M_{200})$ ranges from massive spirals that approach or exceed the cosmic baryon fraction down to five baryon-deficient dwarfs (DDO 190, LVHIS 017, LVHIS 072, LVHIS 080, UGC 8508) whose stellar masses sit $\sim$1–1.5 orders of magnitude below the abundance-matching expectation at $\log(M_{200}/M_\odot) \sim 10.5$–$11.7$. The gas channel is far more regular: $M_{\rm gas}$ tracks $M_{200}$ with a median of about 4 per cent of the cosmic baryon fraction, constant across four orders of magnitude in halo mass. The authors argue the BDDs are not modelling artefacts: the same deficit appears when halo mass is replaced by the directly measured maximum circular speed of the halo, and weak-lensing measurements land nearby; even so, they call the evidence tentative because the relevant $M_{200}$ values carry large uncertainties. None of the comparison models — abundance matching, DarkLight, TNG50, or Simba — reproduces the BDDs or the observed diversity of baryon fractions, which the paper reads as a need for more stochastic baryon retention and more diverse feedback implementations.

Load-bearing premise

The halo masses of the dwarfs, including the five baryon-deficient ones, are inferred by fitting a coreNFW profile to rotation curves that extend only a few kiloparsecs and extrapolating that profile out to R200, tens to hundreds of kiloparsecs away; if the true outer halo is less massive than assumed, the BDDs would relax back toward the normal relation.

Editorial extensions

If this is right

If the BDDs hold up, abundance matching misses a real population: a halo of $M_{200} \sim 10^{11}\,M_\odot$ can host a galaxy 20–60 times poorer in stars than the mean relation predicts, so the scatter in stellar mass at fixed halo mass is a physical signal, not noise.
The gas-to-halo mass relation being a constant 4 per cent of the cosmic baryon fraction across four decades in halo mass is a sharp empirical target that any galaxy formation model should reproduce before its stellar feedback is tuned.
Baryon retention spans the full range from baryon-poor dwarfs to spirals with essentially no missing baryons, so models that produce a single baryon retention efficiency curve cannot match the data.
Below $M_{200} \sim 10^{11}\,M_\odot$ the observed halo concentrations lie systematically below dark-matter-only predictions, and TNG50's concentrations are too high, indicating over-efficient adiabatic contraction in that simulation.
Baryon-rich systems appear at both low and high halo mass, meaning some dwarfs retain a substantial share of the cosmic baryon budget, extending the 'no missing baryons' result down from the massive spiral regime.

Reading between the lines

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

An extension the paper only gestures at: if the five BDDs really sit in overdense haloes, they should betray it through independent tracers such as unusually low globular-cluster counts or sparse satellite systems, giving a non-kinematic test of the classification.
The paper leaves the origin of the concentration deficit open; a testable next step is to compare $c_{200}$ for field dwarfs and group dwarfs at fixed $M_{200}$, which would separate the low-density-environment explanation from the feedback-driven core formation explanation.
If the BDD population is real, abundance-matching-based stellar mass functions need a much wider scatter in the stellar-mass–halo-mass relation at $M_{200} \sim 10^{10.5}$–$10^{11.7}\,M_\odot$ than currently assumed, with consequences for inferred galaxy formation efficiencies.
The tightness of the gas relation combined with the wide stellar scatter suggests cold gas accretion is the regulated channel while star formation is the stochastic one; a concrete test is whether the scatter in $\tilde{f}_\ast$ at fixed $M_{200}$ tracks star-formation main-sequence offset or accretion history proxies in the same galaxies.

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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

Know this: read this paper for the sample and the scaling relations, not for the headline claims as stated. The compilation of 49 gas-rich discs with homogeneous kinematics, 22 new dwarf models, and publicly released data products is a real contribution. The self-consistent treatment of gas flaring and the care with beam smearing and distances are above average for this literature.

What is actually new: the homogeneous multi-decade sample, the new 3DBarolo kinematic models, and the demonstration that the scatter in stellar and baryonic fractions at fixed halo mass is wider than TNG50, Simba, or DarkLight produce. The Mgas-M200 relation sitting at roughly 4% of the cosmic baryon fraction is a clean result that should be useful for a while.

The soft spots are concentrated in the two abstract-level claims. First, the c200-M200 'systematic deviation' below 1e11 is derived from posteriors that use the DJ19 relation as a Gaussian prior; all points sit within 2 sigma of that prior, and no group significance is computed. That is not enough to call it a systematic deviation. Second, the baryon-deficient dwarfs rest on M200 values extrapolated from inner rotation curves out to R200. Appendix F's VDM,max check is not independent for these systems because their Vmax radius lies beyond the Hi extent, so it inherits the same outer-profile assumption. The weak-lensing comparisons are suggestive but not individually constraining. The paper does label the BDDs tentative in the conclusions, which is the right tone; the abstract is too confident.

Minor things: the sample is not volume-complete and the BDD threshold is post hoc. Both are acknowledged and neither is fatal, but they should be kept in mind when quoting the number of BDDs. The math and data handling are solid, and the citation pattern is appropriate—self-citations appear where the pipeline is genuinely reused.

Bottom line: a careful, honest paper that deserves a serious referee and would benefit from softened abstract claims and a robustness test with a steeper outer halo profile. I would cite it for the data and the scaling relations.

Referee Report

2 major / 5 minor

Summary. This paper assembles a curated sample of 49 nearby gas-rich disc galaxies with high-resolution Hi kinematics, NIR photometry, and standard-candle distances, and derives mass models via 3DBarolo kinematic modelling, galpynamics rotation curve decomposition, and nested-sampling Bayesian fits with self-consistently computed gas flaring. The dark matter haloes are modelled as coreNFW profiles with free mass-to-light ratios, halo mass, concentration, and core-size parameter. From these models the paper constructs the stellar, gas, and baryonic mass relations with halo mass, computes baryon retention fractions, and compares them with abundance matching, DarkLight, TNG50, and Simba. It reports two headline results: a population of five baryon-deficient dwarfs (BDDs) with stellar masses 20-60 times below abundance-matching expectations, and a c200-M200 relation with systematically low concentrations below M200 ~ 10^11 Msun and at the highest masses.

Significance. If the BDD population is real, it would substantially widen the observed scatter in baryon retention efficiency at fixed halo mass and would challenge current galaxy formation models and abundance-matching assumptions. The paper's strengths are its homogeneous and high-quality data treatment: beam smearing is handled with 3DBarolo, gas disc flaring is solved self-consistently in vertical hydrostatic equilibrium, distances are checked with TRGB/Cepheid measurements, and the kinematic profiles are made public. The comparison with independent weak-lensing measurements of the SHMR is a valuable cross-check. However, both headline claims depend on halo parameters inferred from a specific assumed dark matter profile, and the concentration claim is made with the DJ19 relation imposed as a Gaussian prior; these dependencies need to be explicitly tested before the conclusions can be fully accepted.

major comments (2)

[Appendix F and Sec. 6.1] The VDM,max check in Appendix F does not break the outer-profile degeneracy on which the BDD classification rests. For the five BDDs, the observed rotation curves extend only a few kiloparsecs while R200 is tens to hundreds of kiloparsecs away, and VDM,max is computed from the same fitted coreNFW haloes; for these systems the radius at which VDM,max occurs (~2.16 rs) lies beyond the observed Hi extent, so VDM,max inherits the same extrapolation as M200. If the true outer profile is steeper than NFW (e.g., a gNFW with beta > 3 or a truncated halo), the inferred M200 could be biased upward by more than the quoted uncertainties, moving these galaxies back toward the abundance-matching relation. I request an explicit test with an alternative outer profile family, or an equivalent analysis that does not assume the same coreNFW extrapolation, and a demonstration of whether the five BDDs survive that test.
[Sec. 6.4 and Sec. 4.3] The conclusion that c200 is systematically lower than the DJ19 relation at 10^10 < M200/Msun < 10^11 is drawn from posteriors obtained with a Gaussian prior centred exactly on the DJ19 c200-M200 relation with sigma = 0.16 dex. The paper itself states in Sec. 4.3 that for some galaxies the concentration remains unconstrained with a flat prior, which is the stated motivation for imposing this prior. With such a narrow prior, the low-concentration values are pulled toward the prior mean, so the 'substructure' in Fig. 10 is a residual from that pull rather than an independent measurement. Please re-fit the low-mass subsample with a flat or substantially wider c200 prior and report how many galaxies remain below the DJ19 relation by more than 1 sigma; this is necessary to support the claim of systematically low concentrations.

minor comments (5)

[Sec. 2.1] The text says the selection cuts result in 16 massive spiral galaxies, but only 15 galaxies are listed (NGC 0253 through NGC 5055); please correct the number or add the missing galaxy.
[Appendix F] In the paragraph on adiabatic contraction, 'the gap galaxies do not have high c200 values' appears to be a typo for 'these galaxies'; as written, the phrase is unclear.
[Fig. 6] The label 'Moster + 10' in the bottom panels is ambiguous; it should read 'Moster et al. (2010)' to match the reference style used elsewhere.
[Eq. (C.1) and surrounding text] The base of the logarithm in the luminosity-mass-to-light relation is not stated; given the use of log(Mstar/Msun) elsewhere, base 10 is presumably intended and should be stated explicitly.
[Sec. 6.1 and abstract] The abstract describes BDDs as having stellar masses ~1-1.5 orders of magnitude lower than expected, while Sec. 6.1 quotes a factor of 20-60 (i.e., 1.3-1.8 dex); these statements should be harmonised.

Circularity Check

0 steps flagged · score 2.0 of 10

No load-bearing circularity: scaling relations and the baryon-deficient dwarf classification rest on independent rotation-curve, photometric, and weak-lensing data; the c200 result is tested against an imposed external prior, and the VDM,max check is a secondary consistency test rather than the derivation.

full rationale

The central scaling relations are derived from independent inputs: Mstar and Mgas come from NIR and Hi photometry (Sec. 4.1), while M200 and c200 come from rotation-curve decomposition under a coreNFW halo (Secs. 4.2-4.3). The BDD population is identified in Sec. 6.1 by comparing fitted M200 values against independently measured stellar masses and against the external abundance-matching reference of Moster et al. (2010), with an additional external weak-lensing comparison in Sec. 6.1 and Fig. 7. The concentration-mass result is not circular even though the DJ19 c200-M200 relation is used as a Gaussian prior: the prior is an external theoretical benchmark, and the reported low concentrations lie away from the prior centre, so any prior bias would push the posteriors toward, not away from, the comparison relation. The only point approaching circularity is Appendix F's VDM,max robustness check: 'we sample the posterior distributions of our best-fitting mass models and extract the maximum circular speed of the halo.' For several BDDs, the inferred Vmax radius can lie beyond the few-kpc Hi extent, so this check inherits the same outer-profile extrapolation as M200. However, this is a secondary consistency argument, not the basis of the BDD claim, which is also supported by independent weak-lensing measurements and by the direct SHMR comparison. Self-citations to Mancera Piña et al. (2022a) and Kim et al. (2024a) are methodological or comparative, not load-bearing uniqueness claims. No circular step reduces a prediction to a fitted input.

Assumptions & free parameters 6 free parameters · 8 assumptions · 0 invented entities

No fundamentally new physical entity is introduced. The analysis rests on LambdaCDM, dynamical equilibrium, hydrostatic balance, the coreNFW halo family, external priors for M*/L and c200, and an external abundance-matching benchmark. The main cost is the assumed halo profile and priors, which are acknowledged in the text but not always quantified.

free parameters (6)

Stellar disc mass-to-light ratio Y_d (per galaxy) = log Y_d medians in Table G.1, roughly -0.7 to -0.1 dex
Fitted in the mass models with a Gaussian prior from empirical luminosity-Y_d relations (Appendix C). Directly sets M* and therefore the SHMR and baryon fractions.
Stellar bulge mass-to-light ratio Y_b (per galaxy) = log Y_b medians in Table G.1 for 12 bulge galaxies
Fitted with a flat prior Y_d < Y_b < 2 Y_d; affects Mstar for massive spirals.
Halo mass M200 (per galaxy) = log M200 medians in Table G.1, about 9.0 to 13.1
Central inferred quantity from rotation curve decomposition, with a flat prior 6 < log M200 < 14.
Halo concentration c200 (per galaxy) = log c200 medians in Table G.1, about 0.55 to 1.41
Fitted with a Gaussian prior centered on the DJ19 c200-M200 relation with sigma 0.16 dex. The low-mass concentration claim depends on this prior.
Core-size parameter eta (per galaxy) = log eta medians in Table G.1, often at prior boundaries
Controls the dark matter core radius via rc = eta Re. Flat prior log 0.1 to log 3.75; for about one fifth of dwarfs the posterior hits the upper bound.
Surface density profile coefficients (galpynamics fits) = Per-galaxy values in the electronic profiles
Coefficients such as Sigma0, R1, R2, alpha, Sersic n and Re, or poly-exponential c_i, fitted to observed H I, CO, and NIR profiles. These are integrated to obtain Mstar and Mgas.

assumptions (8)

domain assumption LambdaCDM cosmology with Omega_m=0.3, Omega_Lambda=0.7, H0=70 km/s/Mpc and fbar,cosmic=0.16.
Stated at the end of Sec. 1 and used for M200 and baryon fraction definitions. Different cosmology would shift absolute normalizations.
domain assumption Galaxies are in dynamical equilibrium and rotation curves trace the gravitational potential (Eq. 1).
Standard mass modeling assumption. Non-equilibrium gas or strong non-circular motions would bias M200 and c200.
domain assumption Gas disks are in vertical hydrostatic equilibrium with a Gaussian vertical profile (Eq. 8).
Used to compute gas flaring and gas potentials. The flaring affects halo parameters, especially for low-mass galaxies.
ad hoc to paper Dark matter halos follow the coreNFW family with fixed n=1 and core radius rc=eta Re.
Necessary to parametrize M200 and c200 from rotation curves. If real halos deviate from this family, inferred M200 and especially c200 could be biased.
domain assumption The Diemer and Joyce 2019 concentration-mass relation is the correct Gaussian prior for c200.
Imposed with sigma 0.16 dex. The low-concentration result is partly conditional on this external benchmark.
domain assumption Empirical luminosity-Yd relations from Marasco et al. 2025, fit in Appendix C, set the stellar mass scale.
Used as priors for Yd. For dwarfs the kinematics have limited constraining power on Yd, so Mstar depends significantly on this prior.
domain assumption The Moster et al. 2010 abundance-matching relation is a valid benchmark for defining BDDs.
Used to label baryon-deficient dwarfs. The relation is extrapolated below its calibration range, although weak lensing comparisons provide independent support.
domain assumption The curated sample is representative of gas-rich, regularly rotating disc galaxies despite a complex selection function.
Needed to compare observed scatter and BDD incidence with simulated galaxy populations. Non-representativeness would bias the diversity conclusions.

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Cite this review

Pith. "Pith review of The galaxy-halo connection of disc galaxies over six orders of magnitude in stellar mass." pith.science (2026). https://pith.science/paper/DAFKS72N

@misc{pith2026250522727,
  author       = {Pith},
  title        = {Pith review of: The galaxy-halo connection of disc galaxies over six orders of magnitude in stellar mass},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/DAFKS72N}},
  note         = {Machine review of arXiv:2505.22727}
}

abstract

(Abridged) The relations between stellar ($M_\ast$), gas ($M_{\rm gas}$), baryonic ($M_{\rm bar} = M_\ast + M_{\rm gas}$), and dark matter halo mass ($M_{200}$) provide unique constraints on galaxy formation and cosmology. The shape of the relations constrains how galaxies regulate their growth through gas accretion, star formation, and feedback; their scatter probes the stochasticity of galaxy assembly. Here, we assemble a sample of 49 nearby gas-rich dwarf and massive disc galaxies with unmatched ancillary data. We obtain their gas kinematics and derive their dark matter properties through rotation curve decomposition. Our sample allows us to study the galaxy-halo connection across nearly six orders of magnitude in $M_\ast$. We find that the $M_{\rm gas}-M_{200}$ relation rises monotonically, with galaxies having around 4 per cent of the average cosmological baryon fraction in cold gas. Contrastingly, the $M_\ast-M_{200}$ relation shows a more complex behaviour. A particularly interesting finding is that of a population of baryon-deficient' dwarfs (BDDs) with stellar masses $\sim 1-1.5$ orders of magnitude lower than expected from current models. Yet, baryon-rich galaxies also exist, and we find a large spread in the baryon retention fraction across our galaxies. We compare our findings with semi-analytic and hydrodynamical galaxy formation simulations. While the simulations broadly reproduce most observed features, they struggle to match the BDDs and do not capture the diversity in baryon fractions. Understanding these differences will shed new light on how feedback regulates galaxy formation. Finally, we study the dark matter halo concentration-mass relation. We find that below $M_{200} \sim 10^{11}\,M_\odot$, the concentrations are systematically lower than expected. We discuss whether these results stem from the influence of baryonic physics or the environment.

Figures

Figures reproduced from arXiv: 2505.22727 by the authors.

**Figure 2.** Kinematics of four representative galaxies in our sample (see also Fig. [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗

**Figure 3.** Mass models of nine representative galaxies in our sample (similar plots for our full sample and the corresponding posterior [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗

Figures from the paper (7 more)

**Figure 4.** Figure 4: Our Υd (circles) and Υb (triangles) values as a function of disc luminosity (Ld). We distinguish between galaxies with photometry at 1.65 µm and 3.6 µm. The lines and bands represent the Gaussian priors adopted for Υd in our mass modelling (see Sec. 4 and Appendix C). …

**Figure 5.** Figure 5: Scale heights of the H i for our sample. The top panel colour-codes each galaxy depending on its halo mass, while the bottom panel uses the Vrot/σHI ratio. It has been attempted to find a universal profile for the gas flaring (e.g. Patra 2020b,a; Mancera Piña et al. 20…

**Figure 6.** Figure 6: Relations between stellar and halo mass in our galaxy sample. The [PITH_FULL_IMAGE:figures/full_fig_p013_6.png]

**Figure 7.** Figure 7: Zoom-in SHMR for our galaxy sample contrasted against [PITH_FULL_IMAGE:figures/full_fig_p014_7.png]

**Figure 8.** Figure 8: Relations between the cold gas and halo mass in our sample. The [PITH_FULL_IMAGE:figures/full_fig_p015_8.png]

**Figure 9.** Figure 9: Relations between baryonic and halo mass in our sample. The [PITH_FULL_IMAGE:figures/full_fig_p016_9.png]

**Figure 10.** Figure 10: Concentration–mass relation for our galaxy sample [PITH_FULL_IMAGE:figures/full_fig_p017_10.png]

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Forward citations

Cited by 2 Pith papers

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astro-ph.GA 2026-07 conditional novelty 6.0 of 10

No current simulation simultaneously reproduces observed halo hot-gas fractions and local galaxy star-formation/quenching demographics; strong AGN feedback overquenches, weak feedback retains too much gas.
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UDGs and NUDGE galaxies with independent halo masses follow the globular cluster number-halo mass relation but scatter off the stellar mass-halo mass relation in proportion to their GC counts.

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Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.

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