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REVIEW 4 major objections 5 minor 276 references

Kinematically misaligned gas accretion can sustain main-sequence star formation only in galaxies with stellar mass below about 10^10 solar masses; in more massive galaxies the fresh gas is diluted by the pre-existing stellar population.

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2026-08-02 00:56 UTC pith:3SQZDEKR

load-bearing objection A careful MaNGA study with a real mass-dependent result; abstract overstates it, and the kinematic classification deserves a robustness test. the 4 major comments →

arxiv 2607.14823 v1 pith:3SQZDEKR submitted 2026-07-16 astro-ph.GA

Fuelling the central region of galaxies with misaligned gas accretion

J. L. Tous , S. I. Raimundo , R. Riffel , A. Puglisi , F. Shankar , M. Vestergaard This is my paper
classification astro-ph.GA
keywords galaxy evolutionstar formationgalaxy kinematicsmisaligned gas accretionspecific star formation rateionized gasactive galactic nucleigalaxy quenching
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.

This paper argues that the external accretion of gas whose rotation is misaligned with a galaxy's stars is a real but mass-limited channel for fuelling galaxy centres. Using 201 misaligned and 3,689 aligned galaxies from the MaNGA survey, the authors show that misaligned galaxies keep the central regions of low-mass systems on the star-forming main sequence, but above roughly 10^10 solar masses newly accreted gas is swamped by the compact stellar core, so global star formation stays low. The paper also finds that the central ionized gas reservoir is enhanced exactly in the intermediate-mass range (10^10 to 10^10.6 solar masses), and that active and inactive misaligned galaxies hold similar amounts of central gas, implying a persistent fuel supply for supermassive black holes. If correct, this connects gas accretion geometry to the quenching-rejuvenation cycle and to black hole fuelling timescales.

Core claim

The paper's central claim is that kinematically misaligned gas accretion is a viable channel for nuclear star formation, but only up to a stellar mass of about 10^10 solar masses. In low-mass misaligned galaxies, the specific star formation rate in the centre reaches main-sequence levels; at intermediate masses (10^10-10^10.6 solar masses) the central density of ionized gas peaks, and above about 10^10.6 solar masses misaligned galaxies largely avoid the star-forming main sequence. The authors attribute this mass dependence to compactness: massive misaligned galaxies have central stellar surface densities above about 10^9.2 solar masses per square kiloparsec, so the stellar mass already pres

What carries the argument

The central measurement is the kinematic misalignment angle ΔPA, the difference between the position angle of the stellar velocity field and the H-alpha gas velocity field, computed from maps that maximize the velocity gradient; ΔPA ≥ 45° defines the misaligned sample. The analysis then compares misaligned and aligned galaxies in three stellar mass bins, using radial profiles of specific star formation rate and ionized gas mass surface density, with the central stellar mass surface density within 0.25 R_e serving as a proxy for compactness. The mass-dependence argument hinges on a distinctive 'knee' in the SSFR-versus-compactness plane for misaligned galaxies, where SSFR drops sharply once c

Load-bearing premise

The classification of every galaxy as misaligned or aligned rests on the assumption that the measured gas velocity-field position angle traces pure rotation of a settled gas disk; if AGN outflows, non-circular motions, or low signal-to-noise bias the gas position angle, the split between the two samples is contaminated and every mass-dependent conclusion in the paper is affected.

What would settle it

A spatially resolved integral-field survey that re-derives ΔPA for the same galaxies using a second kinematic tracer, such as CO emission, would settle whether the misaligned/aligned split is robust; a large population of massive (above 10^10.6 solar masses) misaligned galaxies with main-sequence-level specific star formation rates would directly contradict the paper's central claim.

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

If this is right

  • Misaligned accretion is a viable rejuvenation mechanism only below roughly 10^10 solar masses; above that, external gas cannot push a galaxy back onto the main sequence.
  • The intermediate-mass range (10^10-10^10.6 solar masses) is where misaligned gas most effectively builds a central reservoir, coinciding with the halo mass above which supernova feedback ceases to be effective at quenching.
  • Misaligned galaxies, whether or not they host an AGN, carry comparable central ionized gas reservoirs, implying that most have the fuel to power a supermassive black hole; the absence of AGN in many such systems likely reflects duty cycles far shorter than the misalignment lifetime.
  • The low specific star formation rates of massive misaligned galaxies stem from central stellar compactness rather than an absence of star formation.
  • At low stellar masses, kinematic misalignment itself drives the enhanced central gas concentration; at higher masses, the host galaxy's gravitational potential becomes the dominant factor.

Where Pith is reading between the lines

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

  • If misaligned accretion commonly supplies a long-lived fuel reservoir, intermediate-mass misaligned galaxies should host preferentially low-luminosity, accretion-rate-limited AGN; comparing Eddington ratios of aligned and misaligned AGN at fixed mass would test this directly.
  • The sharp SSFR drop at high central stellar density makes misaligned galaxies plausible local analogues of the high-redshift compaction events that precede inside-out quenching; age-gradient measurements of their stellar populations could check that sequence.
  • The ΔPA-based selection may miss counter-rotating gas that projects as aligned; deprojecting the intrinsic misalignment distribution from the observed axis ratios would quantify how much the mass-dependent trends are affected by projection.
  • Ionized gas is only a small fraction of the fuel supply; CO or dust-continuum mapping of a subset of misaligned galaxies would reveal whether the molecular reservoir shows the same central concentration and mass dependence.

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

4 major / 5 minor

Summary. The manuscript uses MaNGA IFS data to compare 201 galaxies with kinematically misaligned gas (ΔPA ≥ 45°, measured from the difference between stellar and Hα velocity-field position angles) with 3689 aligned galaxies. It analyses global stellar mass and specific star formation rate, central Hα concentration, total ionized gas mass, and radial profiles of SSFR and ionized gas surface density, splitting the sample into three stellar-mass bins. The authors report that misaligned galaxies are less massive, have lower SSFRs, and show more centrally concentrated ionized gas, with the central ionized-gas density peaking at intermediate masses (10^10–10^10.6 M☉). They argue that in low-mass systems misaligned accretion can sustain main-sequence-level star formation, while in more massive, compact systems the newly accreted gas is diluted by the pre-existing stellar mass and mainly replenishes the nuclear reservoir, with implications for AGN fuelling. Appendices provide additional controls based on light concentration (C95), SFR surface density, and morphology.

Significance. If the central conclusions hold, this is a valuable population-level constraint on how externally accreted, kinematically misaligned gas fuels nuclear star formation and AGN reservoirs across mass. The paper's strengths include a large homogeneous MaNGA sample, bootstrap-based uncertainties, KS tests, and a thoughtful C95-matched control analysis in Appendix A that attempts to separate kinematic-misalignment effects from the host galaxy's structural concentration. The interpretation in terms of compactness and dilution of the accreted gas is physically plausible. However, the paper's headline claim is phrased more categorically than the data support, the kinematic classification purity is not quantitatively tested, and there are internal inconsistencies in reported sample sizes. These issues are fixable, but they need to be addressed before the paper is accepted.

major comments (4)
  1. [Section 2 / Section 1] The entire sample definition rests on ΔPA, derived from the PA that maximizes the velocity gradient in the Hα velocity field. The paper notes in Section 1 that powerful outflows may affect gas kinematics, but it does not quantify what fraction of the 201 'misaligned' galaxies have non-rotating, disturbed, or outflow-dominated Hα velocity fields. Given that the misaligned subsample has a 21% AGN fraction versus 6% among aligned galaxies, and AGN incidence is mass-dependent, a mass-dependent contamination could produce the central trend (low SSFR and quiescence at high mass) without any causal link to misaligned accretion. I request robustness tests: fit rotating-disc models or use a kinematic asymmetry metric, exclude or separately flag galaxies with clear outflow signatures, and rerun the key analyses on the clean subsample.
  2. [Section 3.2, Figs. 4 and 5] The sample numbers are internally inconsistent. The abstract and Section 2 state 201 misaligned and 3689 aligned galaxies; after excluding 3+37 galaxies with offset maps, Section 3.2 reports 172 misaligned and 4016 aligned galaxies with adequate coverage. The AGN/non-AGN classification then gives 142+30 misaligned and 3798+218 aligned, again implying 4016 aligned galaxies. This exceeds the total aligned sample of 3689. Please reconcile these numbers and verify that the KS tests and fractions are computed with the correct sample sizes.
  3. [Abstract / Section 5, Fig. 3] The phrase 'this specific accretion channel can only sustain main-sequence levels of star formation in galaxies with M* ≲ 1e10 M☉' is too categorical. Figure 3 shows that only ~65% of low-mass misaligned galaxies are on the main sequence, with ~35% in the green valley or quiescent regimes, and that ~30% of intermediate-mass misaligned galaxies are still on the main sequence. The data support a statistical statement like 'typically' or 'on average', not 'can only'. Please rephrase the claim to a distributional statement and include the actual numbers and bootstrap uncertainties, especially for the high-mass bin where the 5.5% main-sequence fraction is based on a small sample.
  4. [Appendix A, Fig. A2 vs abstract] The claim of a 'strongest enhancement at intermediate masses' is not robust to structural matching. After matching on C95, the difference in central Hα concentration between misaligned and aligned galaxies is significant only at low mass (p=0.01); at intermediate and high mass the p-values are 0.40 and 0.49 (Fig. A2, top row). The absolute peak in central ΣHII at intermediate mass (Fig. 7) may therefore reflect the compactness of those hosts rather than an enhanced effect of kinematic misalignment. Please add a formal significance test for the mass dependence of the enhancement, and align the abstract and Section 5 with the matched-control results.
minor comments (5)
  1. [Section 3.1] The definition of the MS/GV/QS regimes is stated as 'if log(SSFR_MS) is...'; this should be the offset 'log SSFR − log SSFR_MS' from the Renzini & Peng main sequence, not the main-sequence value itself. Please clarify the notation.
  2. [Appendices A2/A3 captions] The notation (r_m, n_0) = (279:58, 1) is confusing. As defined, r_m is the average number of controls per misaligned galaxy, but the parenthetical values appear to be a ratio of total controls to misaligned galaxies plus n_0. Please define the notation explicitly and make it consistent.
  3. [Appendix C caption] Typo: 'witin' should be 'within'.
  4. [Section 5] The concluding paragraph cites 'Raimundo et al. 2013' among references supporting misaligned accretion fuelling the centre and nuclear activity. Please check whether 'Raimundo et al. 2023' or another appropriate work is intended.
  5. [Eq. (1)–(3)] The Balmer-decrement correction uses the Cardelli et al. (1989) extinction curve with R_V = 3.1. It would be helpful to note whether a starburst attenuation curve would change any conclusions, though this is unlikely to affect the relative comparisons.

Circularity Check

0 steps flagged

No significant circularity: the analysis is an empirical comparison built on external calibrations, not a derivation that reduces to its inputs.

full rationale

The paper's central claims are observational comparisons, not predictions derived from fitted parameters. Kinematic misalignment is defined in Section 2 via ΔPA = |PA_stars − PA_gas|, and this is an explicit sample-selection criterion, not a quantity predicted from the later star-formation results. Stellar masses and SFRs are taken from Salim et al. (2018), emission-line/SFR maps from Riffel et al. (2023), main-sequence/green-valley/quiescent boundaries from Renzini & Peng (2015) and Tous et al. (2024), and ionized-gas masses from Kim (1989) with electron densities from Sanders et al. (2016). None of these calibrations are adjusted to reproduce the paper's conclusions. The main findings—that misaligned galaxies have more centrally concentrated ionized gas, avoid the high-SSFR region at high stellar mass, and show central gas density peaking at intermediate masses—are obtained by comparing binned distributions with KS tests and bootstrap uncertainties. Self-citations to Raimundo et al. (2023, 2025) provide the ΔPA measurement method and prior AGN-excess context, but the method is described in the text and the conclusions do not rest on an unverified uniqueness theorem or ansatz imported from those papers. The mass bins used in Figs. 3, 6, and 7 are fixed before the profile analysis and are not optimized to produce the reported peak, so the binned 'peak' is a data description rather than a construction-level circularity. Potential measurement concerns, such as outflow contamination of gas PAs, are correctness/robustness risks and are not circularity: the paper does not define its outcome in terms of its input by construction.

Axiom & Free-Parameter Ledger

2 free parameters · 5 axioms · 0 invented entities

The paper's central claim depends on externally calibrated data products (Salim et al. SED masses/SFRs, MEGACUBES emission-line fits) and a set of hand-chosen analysis thresholds (ΔPA≥45°, mass bins). No new physical entities are introduced. The main potential circularity is the mass-bin choice: the 'peak' at intermediate mass is defined by the same binned data used to claim it, and the bin edges are not independently derived.

free parameters (2)
  • Mass bin boundaries = 1e10 and 1e10.6 Msun
    The low/intermediate/high mass bins in Figs 3, 6, 7 are chosen by hand; the abstract's threshold and the intermediate-mass peak depend on these edges.
  • Kinematic misalignment threshold = ΔPA = 45° (with uncertainty <30°)
    Selection threshold for 'highly misaligned'; changing it changes sample composition (201 vs 3689 galaxies).
axioms (5)
  • domain assumption Hα emission traces ionized gas and recent star formation; Balmer decrement correction with intrinsic Hα/Hβ=2.86 and Cardelli extinction curve are valid.
    Section 3.2, Eqs (1)-(3). If dust correction or case B assumptions fail, central gas concentrations and masses are biased.
  • domain assumption The velocity-gradient PA difference ΔPA between Hα gas and stars robustly identifies externally accreted misaligned gas; gas kinematics are dominated by rotation and not by AGN outflows.
    Section 2; the authors note outflows can affect gas kinematics but do not correct for them.
  • domain assumption The Renzini & Peng (2015) main-sequence relation and the adopted MS/GV/QS offsets (-0.5 and -1.1 dex) are applicable to the local MaNGA sample.
    Section 3.1; they check alternative green valley definitions but not the MS relation itself.
  • domain assumption Stellar masses and SFRs from Salim et al. (2018) SED fits are unbiased for both misaligned and aligned galaxies.
    Used for all mass and SSFR classifications; systematic differences between morphologies could change the mass dependence.
  • ad hoc to paper Mass-bin boundaries are physically meaningful / chosen independently of the result.
    The 1e10-1e10.6 Msun range is linked to halo mass ~1e12 Msun in the discussion, but the boundaries are not derived from data or a model.

pith-pipeline@v1.3.0-alltime-deepseek · 22654 in / 11647 out tokens · 99134 ms · 2026-08-02T00:56:18.479258+00:00 · methodology

0 comments
read the original abstract

Recent studies have shown that the accretion of kinematically misaligned gas fuels the central reservoir of galaxies, triggering nuclear activity and star formation. In this work, we show that this specific accretion channel can only sustain main-sequence levels of star formation in galaxies with $M_* \lesssim 10^{10} {\rm M_\odot}$. Using a sample of 201 kinematically misaligned galaxies, and a comparison sample of 3689 aligned galaxies, from the Mapping Nearby Galaxies at Apache Point Observatory survey, we investigate the impact of kinematically misaligned gas on star formation across stellar mass. We characterise the global specific star formation rate, central concentration and mass of ionized gas of our samples, and derive radial profiles of specific star formation rate and ionized gas mass surface density. We find that misaligned galaxies exhibit more centrally concentrated ionized gas than their aligned counterparts, with the strongest enhancement occurring at intermediate masses ($10^{10}$-$10^{10.6} {\rm M_\odot}$), where the central ionized gas density peaks. In galaxies less massive than $10^{10} {\rm M_\odot}$, misaligned gas fuels nuclear star formation at rates typical of star-forming systems. At higher masses, however, the impact of this newly accreted gas is diluted by the larger pre-existing stellar mass in the central regions, limiting its ability to rejuvenate the star formation activity in these galaxies. Our results also show that misaligned galaxies with or without nuclear activity exhibit similar central concentrations of ionized gas, suggesting that most have a reservoir capable of fuelling their supermassive black holes over timescales longer than typical nuclear activity episodes.

Figures

Figures reproduced from arXiv: 2607.14823 by A. Puglisi, F. Shankar, J. L. Tous, M. Vestergaard, R. Riffel, S. I. Raimundo.

Figure 1
Figure 1. Figure 1: Distribution of global stellar mass (left) and specific star formation rate (right) of galaxies with high (red) and low (blue) kinematic misalignment. In both panels, the histograms show, for each subset, the fraction of galaxies in a given bin so each distribution is normalized to unity. For both properties, the observed differences are statistically significant according to a two-sample KS test, with 𝑝-v… view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of galaxies with high (red dots) and low (blue contours) kinematic misalignment in the global specific star formation rate vs stellar mass plane. The contour lines are derived from a kernel density estimate of the distribution of aligned galaxies. For reference, the grey-shaded background shows the distribution of SDSS galaxies (at 𝑧 < 0.15) binned into hexagonal cells, where darker tones indi… view at source ↗
Figure 3
Figure 3. Figure 3: Fraction of galaxies with high (top) and low (bottom) kinematic misalignment in three bins of stellar mass: 𝑀∗ ≤ 1010 M⊙ (low), 1010 M⊙ < 𝑀∗ ≤ 1010.6 M⊙ (mid), and 𝑀∗ > 1010.6 M⊙ (high). In both panels, the different tones, from darker to lighter, correspond to galaxies in the main sequence (MS), green valley (green valley), and quiescent (QS) regimes. The error bars show the 1𝜎 uncertainty from 1000 boots… view at source ↗
Figure 4
Figure 4. Figure 4: Enclosed H 𝛼 luminosity as a function of radius, normalized to 𝑅e, of galaxies with high (red dots) and low (blue triangles) kinematic misalign￾ment in the original sample (top panel), with no AGN (middle panel), and with AGN (bottom panel). Data points indicate the median, error bars show the 3𝜎 uncertainty on the population median inferred from 1000 bootstrap resamples, and shaded regions show the interq… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of total ionized gas mass within the 𝑅e of galaxies with high (red) and low (blue) kinematic misalignment. The histograms show, for each subset, the fraction of galaxies in a given bin so each distribution is normalized to unity. The observed differences are statistically significant according to a two-sample KS test, with 𝑝−value ≪ 0.001. latter result to a mismatch between the duration of ki… view at source ↗
Figure 6
Figure 6. Figure 6: Median SSFR radial profiles of galaxies with high (red dots) and low (blue triangles) kinematic misalignment in the same three bins of stellar mass as in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Global specific star formation rate vs stellar mass surface density within the central 0.25 𝑅e as a function of global stellar mass of galaxies with high (left) and low (right) kinematic misalignment. In both panels, the different tones of the markers indicate, from darker to lighter, increasing global stellar mass corresponding to the same mass bins of [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗

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