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REVIEW 2 major objections 4 minor 135 references

HI asymmetries in spatially resolved SIMBA galaxies

T0 review · 2 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read In simulated galaxies, a merger or interaction within the last ~2 Gyr leaves a measurable disturbance in the projected neutral hydrogen distribution that the morphological asymmetry $A_{\mathrm{mod}}$ detects more reliably than the…

desk verdict A solid methodological paper on HI asymmetry measurements; the resolution-standardization result is convincing, but the category comparison needs a validated merger classification before it can be trusted. read the letter →

arxiv 2506.15827 v1 pith:WZVZGQO6 submitted 2025-06-18 astro-ph.GA

Nadine A. N. Hank , Marc A. W. Verheijen , Sarah-L. Blyth , Romeel Davé , Kyle A. Oman , Nathan Deg , Marcin Glowacki This is my paper · ORCID
classification astro-ph.GA
keywords galaxies:evolutioninteractionsISMradiolines:galaxiesHIasymmetriesmorphologicalasymmetryspectralSIMBAcosmologicalsimulations
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

This paper asks whether a galaxy's recent dynamical history leaves a measurable imprint in its neutral hydrogen (H I) gas, and whether the integrated spectrum or the projected gas map is the better tracer. Using about 1,100 simulated galaxies with mock observations matched to a medium-deep H I survey, it classifies each galaxy as isolated, interacted, or merged over the preceding ~2 Gyr and compares two asymmetry measures: the spectral flux asymmetry $A_{\mathrm{flux}}$ and the modified morphological asymmetry $A_{\mathrm{mod}}$. The paper's central claim is that galaxies that merged or interacted are more asymmetric than isolated galaxies, that this difference is clearer in $A_{\mathrm{mod}}$ than in $A_{\mathrm{flux}}$, and that $A_{\mathrm{mod}}$ decreases with baryonic mass for the disturbed categories while $A_{\mathrm{flux}}$ shows no such trend. A sympathetic reader would care because upcoming wide-field H I surveys will deliver many spatially unresolved detections, and the results warn that relying on spectral asymmetry alone will underestimate how disturbed the H I discs of those galaxies are.

What carries the argument

The load-bearing tools are two asymmetry statistics and a resolution standardization. $A_{\mathrm{flux}}$ is the difference between the integrated flux in the two halves of the global H I profile divided by the total flux. $A_{\mathrm{mod}}$ is the mean over pixels of $|I - I_{180}| / |I + I_{180}|$, which up-weights faint outer-disc asymmetries such as tidal features. Because more massive H I discs contain more resolution elements at a fixed beam size, the paper smooths each moment-0 map to the resolution at which the galaxy is resolved by about 10 beams in area ($N_{\mathrm{beams}} \approx 10$), which removes a spurious mass-asymmetry trend. The dynamical classification is carried by fractional stellar and baryonic mass jumps ($R_{\star}$ and $R_{\mathrm{baryon}} \geq 5$ per cent), a star-formation correction, and neighbour separations of $\leq 50$ kpc for mergers and $\leq 100$ kpc for interactions with mass ratio $\geq 5$ per cent.

What would settle it

Re-classify the same simulated galaxies using a merger tree that identifies genuine merger events by shared stellar or dark-matter particles rather than by fractional mass jumps, then recompute the $A_{\mathrm{mod}}$ and $A_{\mathrm{flux}}$ distributions of the three categories; if the merged-isolated separation in $A_{\mathrm{mod}}$ shrinks to the level seen in $A_{\mathrm{flux}}$, the central claim is undercut.

Watch

Extended reading notes

Core claim

In the SIMBA cosmological hydrodynamical simulations, the paper builds synthetic H I data cubes at the resolution of a medium-deep imaging survey and measures, for each of 1,157 galaxies, the integrated spectral asymmetry $A_{\mathrm{flux}}$ and the modified morphological asymmetry $A_{\mathrm{mod}}$ (the pixel-wise normalized difference between the moment-0 map, the velocity-integrated H I intensity map, and its 180-degree rotation). Using galaxy tracking over roughly 2.2 Gyr, it assigns galaxies to isolated, interacted, or merged categories by fractional stellar and baryonic mass jumps, star-formation corrections, and neighbour separations. The paper finds that the merged and interacted categories have higher mean $A_{\mathrm{flux}}$ and $A_{\mathrm{mod}}$ than the isolated category, that the separation between category distributions is larger for $A_{\mathrm{mod}}$ than for $A_{\mathrm{flux}}$, and that the interacted category differs from isolated only in $A_{\mathrm{mod}}$, not in $A_{\mathrm{flux}}$. It also finds an inverse correlation between baryonic mass and $A_{\mathrm{mod}}$ for the interacted and merged categories, absent for $A_{\mathrm{flux}}$, and only a weak correlation between $A_{\mathrm{flux}}$ and $A_{\mathrm{mod}}$ overall. Taken together, these results imply that a recent merger or interaction leaves a detectable, ordered disturbance in the projected H I distribution, and that this disturbance is better captured by the morphology-based measure than by the flux-ratio measure.

Load-bearing premise

The load-bearing premise is that the fractional mass-jump thresholds, star-formation correction, neighbour separation cutoffs, and mass-ratio cut used to classify galaxies as isolated, interacted, or merged actually recover true merger and interaction events; the paper does not validate these thresholds, and if they mislabel many galaxies, every category comparison inherits the error.

Editorial extensions

If this is right

  • Galaxies with a merged or interacted dynamical history within the last ~2 Gyr should, on average, show higher $A_{\mathrm{mod}}$ than isolated galaxies, making morphological asymmetry a candidate indicator of recent disturbance.
  • Spectral asymmetry $A_{\mathrm{flux}}$ should be treated as a lower limit on intrinsic H I disturbance: a symmetric global profile does not imply an undisturbed H I disc.
  • Surveys spanning a wide range of H I masses must match the relative spatial resolution (roughly equal numbers of beams across the galaxy area) before comparing $A_{\mathrm{mod}}$ values, or they will measure a spurious mass dependence.
  • For interacted and merged galaxies, lower baryonic mass should be associated with higher morphological asymmetry, consistent with shallow potential wells being more easily distorted.
  • The weak correlation between $A_{\mathrm{flux}}$ and $A_{\mathrm{mod}}$ limits what can be inferred about unresolved H I distributions from integrated profiles alone.

Reading between the lines

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

  • Extension: applying the same resolution-matching procedure to existing resolved H I samples would test whether previously reported mass and environment trends in morphological asymmetry are partly resolution artefacts.
  • Going beyond the paper, the weak $A_{\mathrm{flux}}$–$A_{\mathrm{mod}}$ correlation implies that unresolved H I surveys will systematically undercount recently disturbed galaxies, because $A_{\mathrm{flux}}$ misses the low-surface-brightness features $A_{\mathrm{mod}}$ is designed to catch.
  • An unstated corollary: if low-mass galaxies are the most morphologically asymmetric after interactions, resolved H I surveys that reach lower H I masses should find a rising asymmetry fraction toward the faint end, a prediction the paper's sample cuts do not fully test.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. This paper uses the SIMBA cosmological simulations to generate synthetic HI data cubes that mimic Apertif Medium-Deep Survey observations, and measures spectral (A_flux) and morphological (A_mod) asymmetries for ~1150 galaxies. The authors find that SIMBA broadly reproduces the observed HI size-mass relation, albeit with slightly small discs at high HI mass. They quantify how A_mod measured at a fixed physical resolution correlates with HI mass, and show that this correlation largely disappears when the resolution is standardized to approximately 10 beams across the galaxy. They classify galaxies into isolated, interacted, and merged categories based on fractional stellar and baryonic mass jumps and neighbour separations over the preceding ~2 Gyr, and report that the interacted and merged categories have higher asymmetries than the isolated category, with a larger separation between categories in A_mod than in A_flux. For interacted and merged galaxies they find an inverse correlation between baryonic mass and A_mod, and they report a weak but significant correlation between A_flux and A_mod. The paper concludes that A_flux alone underestimates the degree of morphological disturbance in HI discs.

Significance. If the dynamical classification is trustworthy, the paper provides a valuable large-sample benchmark for interpreting resolved and unresolved HI asymmetries in upcoming surveys. The resolution-standardization procedure is a genuinely useful methodological advance, and the claim that A_mod is more sensitive than A_flux to recent interactions is a testable prediction for Apertif, WALLABY, and other HI surveys. The paper also benefits from using a simulation suite (SIMBA) that was not calibrated to asymmetry observables, so there is no direct circularity. The use of public simulation data and the martini package supports reproducibility, with data products available on reasonable request. However, the central classification step is not validated against a known-truth merger history, and the combined-sample analysis does not fully control for the different volume mixtures, so the scientific claims are not yet secured.

major comments (2)
  1. [Section 4, Eq. (11)] The merger and interaction classification is not validated against a known-truth merger history. The thresholds (R_star and R_baryon >= 5 per cent, R_star - R_SF >= 5 per cent, r_sep <= 50 or 100 kpc, baryonic mass ratio >= 5 per cent) are adopted from the literature, but no confusion matrix, visual verification of the merged/interacted classes, or comparison with the simulation's own merger trees is provided. The refined-isolated check only guards against false negatives in the isolated class; it says nothing about false positives in the merged and interacted classes, which can arise from smooth gas accretion, flybys, or satellite confusion. Because the central claims of Section 4.1 (higher mean A_flux and A_mod, larger A_mod separation between categories) and Section 4.3 (inverse A_mod-baryonic mass trend) depend entirely on this categorization, I request an explicit validation step, for example using true halo/galaxy merger histories from the SIMBA snapshots to compute contamination rates, or a threshold-robustness analysis varying R from 1-10 per cent, r_sep from 30-100 kpc, and the mass ratio from 1-10 per cent, demonstrating that the KS-test separations and median differences persist.
  2. [Section 4.1 and Figs. 5-6] The combined-sample analysis in Section 4.1 may be driven in part by the differing volume mixtures. SIMBA-25 contributes 78/513 (15 per cent) merged galaxies versus 58/644 (9 per cent) for SIMBA-100, while Figs. 5 and 6 show systematically different A_mod behaviour between the two volumes, including different regions of the A_mod-HI mass plane being populated. At face value, the merged category's higher A_mod could reflect the larger SIMBA-25 fraction in that category rather than the dynamical history itself. I request that the KS tests and median comparisons shown in Fig. 7 and Table 1 be repeated separately for SIMBA-25 and SIMBA-100, and ideally within overlapping baryonic-mass or HI-mass ranges. If the category separations persist in both volumes, the volume-mixing concern is resolved.
minor comments (4)
  1. [Section 4.1 and Table 1] The text in Section 4.1 repeatedly describes the categories as having 'higher mean asymmetry' and 'mean asymmetry', but Table 1 reports only medians and interquartile ranges, not means. The abstract also uses 'mean asymmetries'. Please either report both the mean and median for each category, or consistently use one statistic and state explicitly which one is used in the comparisons and in the abstract.
  2. [Section 2.4] The 3-sigma-MAD cut that removes 181 galaxies based on the discrepancy between cube-measured and catalogue HI masses may preferentially exclude satellites with HI bridges or interacting systems, which could in turn affect the category fractions and the asymmetry distributions. Please briefly discuss the potential selection bias and, if feasible, report the category fractions after excluding the 181 galaxies versus the full starting sample.
  3. [Section 3.2] The procedure for identifying the resolution at which N_beams is approximately 10 is described as smoothing to fixed beam sizes of 30, 45, 60, 90, and 120 arcseconds. Since 'approximately 10' suggests interpolation, please clarify how the exact resolution and the corresponding A_mod value are obtained between these discrete beam sizes.
  4. [Section 4.3 and Fig. 9] The 'clear inverse trend' between A_mod and baryonic mass for the interacted and merged categories is supported only by binned medians in Fig. 9; no Spearman correlation coefficients or significance levels are reported for these categories separately. Please provide these statistics for each category to support the statement in the abstract and conclusions.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the dynamical-history categories are defined from mass-growth histories independent of the asymmetry measurements, and the size-mass benchmark and resolution test are self-contained.

full rationale

This is a measurement study rather than a derivation chain. The central comparisons (A_flux/A_mod versus dynamical history) use a classification based on caesar mass-growth histories (Eq. 11), star-formation-corrected stellar mass jumps, neighbour separation, and baryonic mass ratio; none of these inputs use the asymmetry measurements, so the category separation is not forced by construction. The HI size-mass relation is benchmarked against the external Wang et al. (2016) relation, and SIMBA is not calibrated to HI scaling relations, so the agreement is an independent check. The resolution-standardization result is obtained by re-measuring A_mod at N_beams approximately 10 and is an empirical outcome, not a self-fulfilling fit. The paper does cite prior work by its own authors (e.g., Dave et al. 2020 for the HI mass function; Bilimogga et al. 2022 for the A_mod column-density threshold; Glowacki et al. 2022 for profile-asymmetry trends), but these citations provide methodological context or prior external benchmarks and are not the load-bearing step that produces the asymmetry-category separation. The unvalidated merger/interaction thresholds are a correctness risk, not a circularity: misclassification would weaken or bias the category comparison, but the comparison itself is not equivalent to the classification by definition. No fitted parameter is renamed as a prediction, and no uniqueness claim is imported from the authors' prior work.

Assumptions & free parameters 3 free parameters · 4 assumptions · 1 invented entities

The central claims rest on the performance of the SIMBA simulation and on hand-chosen classification thresholds. The paper is explicit about the noise-free nature of the cubes and the absence of kinematic analysis, and it carefully describes the mass cuts and completeness limit. The main unvalidated element is the dynamical-history classification, which carries the burden of the category-based results.

free parameters (3)
  • N_beams target of ~10 for A_mod standardization = ~10 beams
    The resolution at which A_mod is measured is chosen by the authors as approximately 10 beams in the galaxy area. This is a hand-chosen threshold, not derived from an objective criterion, and it directly affects the central comparison between A_mod and baryonic mass and between categories.
  • Merger and interaction classification thresholds = R >= 5%, r_sep <= 50 and 100 kpc, mass ratio >= 5%
    The thresholds defining merged, interacted and isolated categories (Section 4) are chosen by hand following related literature. The 5 per cent mass ratio and 50 and 100 kpc separations are adopted as compromises; the paper does not validate that these thresholds correctly separate true merger and interaction events from other processes.
  • Baryonic mass completeness limit = M_baryon = 10^9.5 M_sun
    The completeness limit in Section 5.2 and Appendix B is defined as the mass where the SIMBA-25 baryonic mass function deviates by 0.25 dex from a fitted Schechter function. It is used to restrict the median trends in Figure 9. The 0.25 dex deviation threshold is a hand-chosen convention.
assumptions (4)
  • domain assumption SIMBA's HI content, including the self-shielding prescription and H2 fraction calculation, is a reliable representation of real HI disks.
    The entire study measures asymmetries in SIMBA's HI and interprets them as physical diagnostics. The paper cites Dave et al. (2019, 2020) for the code's success, but the assumption that simulated HI distributions have realistic asymmetric features is not independently validated.
  • domain assumption Galaxies can be traced across the 11 snapshots via shared star particle IDs in caesar catalogues.
    The dynamical-history classification in Section 4 relies on identifying the most massive progenitor as the galaxy that contains the most shared star particle IDs. This is a standard but unproven-by-this-paper assumption about the fidelity of the merger tree.
  • domain assumption The median radial HI profile and size-mass relation of observed galaxies from Wang et al. (2016) are the correct observational benchmark.
    The size-mass validation in Section 2.5 compares SIMBA only to the Wang et al. (2016) relation. Other observational calibrations exist, and the paper later notes that Wang et al. (2024) find a shallower relation, so the benchmark itself is not uniquely fixed.
  • domain assumption Noise-free synthetic data cubes provide HI measurements that are directly comparable to real observations when interpreting asymmetry trends.
    The cubes have no instrumental noise by design. The authors discuss how noise can both inflate and deflate spectral asymmetries (Section 5.1.2), meaning the simulated asymmetry distributions are not exactly what a real survey with the same parameters would measure. This weakens the quantitative comparison with observed asymmetric fractions.
invented entities (1)
  • None
    purpose: No new physical entities are introduced.
    The paper introduces no new particles, forces, or physical objects. The only constructed objects are synthetic data cubes and the N_beams ~ 10 resolution-standardized maps, which are analysis tools rather than physical entities.

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Cite this review

Pith. "Pith review of HI asymmetries in spatially resolved SIMBA galaxies." pith.science (2026). https://pith.science/paper/WZVZGQO6

@misc{pith2026250615827,
  author       = {Pith},
  title        = {Pith review of: HI asymmetries in spatially resolved SIMBA galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/WZVZGQO6}},
  note         = {Machine review of arXiv:2506.15827}
}
abstract

We present a study of the neutral atomic hydrogen (HI) content of spatially resolved, low-redshift galaxies in the SIMBA cosmological simulations. We create synthetic HI data cubes designed to match observations from the Apertif Medium-Deep HI imaging survey, and follow an observational approach to derive the HI size-mass relation. The HI size-mass relation for SIMBA is in broad agreement with the observed relation to within 0.1 dex, but SIMBA galaxies are slightly smaller than expected at fixed HI mass. We quantify the HI spectral ($A_{\mathrm{flux}}$) and morphological ($A_{\mathrm{mod}}$) asymmetries of the galaxies and motivate standardizing the relative spatial resolution when comparing values in a sample that spans several orders of magnitude in HI mass. Galaxies are classified into three categories (isolated, interacted, or merged) based on their dynamical histories over the preceding ~2 Gyr to contextualize disturbances in their HI reservoirs. We determine that the interacted and merged categories have higher mean asymmetries than the isolated category, with a larger separation between the categories' $A_{\mathrm{mod}}$ distributions than between their $A_{\mathrm{flux}}$ distributions. For the interacted and merged categories, we find an inverse correlation between baryonic mass and $A_{\mathrm{mod}}$ that is not observed between baryonic mass and $A_{\mathrm{flux}}$. These results, coupled with the weak correlation found between $A_{\mathrm{flux}}$ and $A_{\mathrm{mod}}$, highlight the limitations of only using $A_{\mathrm{flux}}$ to infer the HI distributions of spatially unresolved HI detections.

Figures

Figures reproduced from arXiv: 2506.15827 by the authors.

Figure 1
Figure 1. Comparison between the H i mass measured from the masked mock data cube and the expected H i mass from the caesar catalogue for the simba-25 (red) and simba-100 (blue) galaxies. The black dotted line shows the 1:1 relation, with the grey shaded region representing a 0.15 dex buffer from the relation. Galaxies that deviate from the 1:1 relation by more than 3𝜎MAD are plotted as open circle markers and have been exclu… view at source ↗
Figure 2
Figure 2. Sample properties for the final sample of simba-25 (red) and simba-100 (blue) galaxies. Top row: Distributions of the measured H i mass, stellar mass, and baryonic mass (calculated as 𝑀baryon = 𝑀★ + 1.33𝑀H i). Bottom row: Distributions of the H i gas fraction, H i diameter, and specific star formation rate (sSFR = SFR/𝑀★). In all panels, the black step histogram represents the combined sample. The stellar masses and… view at source ↗
Figure 3
Figure 3. Median azimuthally averaged H i surface density profiles for galax￾ies from simba-25 (red) and simba-100 (blue). The median radial profile of high-H i mass galaxies (𝑀H i ≥ 109.5 M⊙) from simba-25 is shown in pink and has been slightly offset horizontally, along with the median profile of simba-100, for easier viewing. The solid grey line shows the median radial profile for a combined sample of resolved galaxies fro… view at source ↗
Figures from the paper (5 more)
Figure 5
Figure 5. Figure 5: Scatter plot of morphological asymmetry (𝐴mod) as a function of H i mass for simba-25 (left) and simba-100 (right) galaxies. Here, 𝐴mod is calculated using the 15′′ × 15′′ resolution moment-0 maps with an applied column density threshold of 5 × 1019 cm−2 . The colour o…
Figure 6
Figure 6. Figure 6: Same as in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 7
Figure 7. Figure 7: Comparison between the cumulative histograms of the spectral asymmetry (𝐴flux, top) and morphological asymmetry (𝐴mod, bottom) for galaxies that have undergone a merger (mass ratios > 1:20) within the last ∼2.2 Gyr (orange, solid), galaxies that have experienced an int…
Figure 8
Figure 8. Figure 8: Left: Spectral asymmetry (𝐴flux) plotted against morphological asymmetry (𝐴mod) for the isolated (grey circles), interacting (green triangles), and merged (orange squares) galaxies in our sample. The Spearman correlation coefficient and associated 𝑝-value using the ful…
Figure 9
Figure 9. Figure 9: H i spectral asymmetry (𝐴flux, top) and morphological asymmetry (𝐴mod, bottom) as a function of baryonic mass. The left panels show the individual data points from the isolated (grey circles), interacted (green triangles) and merged (orange squares) categories. In the …

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Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.