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REVIEW 3 major objections 7 minor 281 references

Searching in HI for Massive Low Surface Brightness Galaxies: II. Completing the UGC Sample

T0 review · 3 major / 7 minor · reviewed 2026-07-31 · grok-4.5

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Pith's one-line read GBT 21-cm observations of the last 35 reachable UGC low-surface-brightness galaxies detect 19, adding one new massive gas-rich LSB.

desk verdict Solid GBT HI catalog completing the remaining UGC late-type LSB targets: real new spectra, one secure massive object, confusion flags already disclosed, science framing thin but honest. read the letter →

arxiv 2607.28180 v1 pith:JEMWR6N4 submitted 2026-07-30 astro-ph.GA

Karen O'Neil , Wim van Driel , Stephan Schneider This is my paper · ORCID
classification astro-ph.GA
keywords lowsurfacebrightnessgalaxiesHIlineGreenBankTelescopeUGCsamplegalaxymasses21-cmspectroscopyspiralredshifts
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 finishes a Green Bank Telescope HI survey of the remaining Uppsala General Catalogue late-type low-surface-brightness galaxies that still lacked measured atomic hydrogen. Of 35 targets, 19 were detected, and five more previously unpublished HI sources turned up by accident in the beam or at other velocities. Only one new object exceeds 10 billion solar masses in HI; the rest sit in the same gas-mass and optical-color ranges already seen in the authors’ earlier 350-galaxy LSB sample and in ALFALFA. Completing the UGC slice shows that these extreme disks are not systematically outliers once their gas is measured, giving a cleaner observational baseline for tests of how galaxies form and evolve at low surface brightness.

What carries the argument

Green Bank Telescope L-band 21-cm spectroscopy with position switching, which supplies integrated HI flux, observed line widths W20 and W50, and derived HI masses for every detection in the completed UGC LSB subsample.

What would settle it

Interferometric or higher-resolution HI maps that spatially separate the confused beams would show whether the wide or velocity-offset profiles (especially those flagged for UGC 07553, UGC 05983, UGC 06395 and the two unidentified sources) truly belong to the catalogued LSB targets.

Watch

Extended reading notes

Core claim

Completing 21-cm HI observations of the final 35 readily observable UGC low-surface-brightness galaxies yields 19 detections plus five previously unpublished serendipitous sources. The new material adds one massive LSB galaxy with HI mass above 10^10 solar masses and four very small dwarfs; overall the objects follow the same HI-mass and color distributions as the authors’ prior LSB set and ALFALFA, with no clear distinction between galaxies that were and were not detected in HI.

Load-bearing premise

Several reported HI profiles may actually come from neighboring galaxies or groups inside the large telescope beam rather than from the named target, so the detection tally and mass values for those objects rest on uncertain associations.

Editorial extensions

If this is right

  • The UGC late-type LSB sample that the GBT can readily observe is now complete in HI.
  • Only one additional massive gas-rich LSB is added to the catalog from this final batch.
  • HI-detected and non-detected LSBs in the sample show no strong optical-color separation.
  • Two serendipitous HI detections still lack clear optical counterparts and need identification.
  • The broader LSB HI-mass distribution remains consistent with earlier work rather than revealing a new extreme population.

Reading between the lines

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

  • Single-dish beam confusion may systematically misassign HI masses for a non-negligible fraction of LSB ‘detections,’ so claims about the massive-LSB tail need interferometric vetting before they are used as formation-theory constraints.
  • The two unidentified HI sources are natural targets for deep optical and infrared imaging as possible gas-dominated or optically dark systems.
  • The lack of color difference between detections and non-detections suggests many non-detections are simply more gas-poor stages of the same LSB sequence rather than a separate class.
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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

3 major / 7 minor

Summary. This paper reports GBT 21-cm HI observations of the final 35 readily observable UGC low-surface-brightness (LSB) galaxies from the authors’ ongoing program, completing that subsample. Of the 35 targets, 19 are detected; two had prior HI measurements that are broadly consistent with the new data. The paper also tabulates five serendipitous HI detections (off-source or at alternate velocities), none previously published in HI. Integrated fluxes, W20/W50 widths, and HI masses are given in Table 1, with notes flagging several confused or unreliable associations. The discussion states that the new objects largely follow the HI-mass and color distributions of the authors’ prior LSB sample and of ALFALFA, adding one secure massive LSB (UGC 11977, M_HI > 10^10 M_⊙). Spectra are deposited on Zenodo.

Significance. As a sample-completion and data-release paper, the work is useful rather than transformative. It finishes the GBT-accessible UGC late-type LSB subset begun in O’Neil et al. (2023), supplies previously unpublished HI parameters for 19+5 sources, and makes the spectra public. That is a solid incremental contribution for LSB demographics, gas-mass functions, and follow-up targeting. Strengths include standard, well-documented GBT position-switched methods, flux checks against calibrators, explicit uncertainty estimates, comparison to the two literature detections, and the Zenodo archive. The scientific interpretation is brief; the lasting value is the catalog and the transparent confusion notes.

major comments (3)
  1. [Table 1; §2] Table 1, unexpected detection J050022.3+305003: the listed Vel_HI = 106096 km s−1 lies far outside the stated spectrometer coverage (−2000 to 30 250 km s−1, later restricted to ≤25 000 km s−1). The source name implies RA 05h, yet the Beam Center column gives 15:00:22.3,+30:50:03. These inconsistencies cannot both be correct and must be resolved (typo in velocity, name, and/or beam coordinates) before the entry can be used; if the line is real, the observing setup description also needs updating.
  2. [§4] §4 Discussion contains an incomplete placeholder (“Himass ?? distribution”) and only qualitative statements that the new sources “fit within the distributions” of ALFALFA and O’Neil et al. (2023), with “no particular distinction” in SDSS colors between detections and non-detections. For a completion paper this need not be lengthy, but the comparison should be made quantitative (e.g., a simple M_HI or color histogram or cumulative distribution against the parent samples) and the placeholder removed so the “unremarkable / one new massive LSB” claim is documented rather than asserted.
  3. [Table 1; Abstract; §5] Table 1 and notes 1–6: six of the nineteen “LSB galaxy” rows are asterisked as unreliable or likely confused (UGC 00134→UGC 00132; UGC 05944 group; UGC 05983/NGC 3432; UGC 06395→IC 2776/2779; UGC 07553 width/velocity offset and neighbors; UGC 07942/AGC 226177). The abstract and §5 still state “19 were detected” and “adding one new massive LSB” without a clear secure-vs-confused census. Please give an explicit count of clean target detections versus reassigned/confused profiles and ensure M_HI and sample statistics used in the discussion refer only to the secure subset (or are shown both ways).
minor comments (7)
  1. [Abstract] Abstract: “oresent” → “present”; “LBG galaxies” → “LSB galaxies”.
  2. [§2] Section heading “2.OBSER V ATIONS AND DATA REDUCTION” has spurious spaces; several run-on word breaks appear elsewhere (e.g., “Hiproperties”, “Higas”, “Hiline”).
  3. [§3.1] §3.1: “only two of which have previously published data” in the abstract/intro is fine, but the body should cite the exact prior profile parameters (flux, W50, V) side-by-side with the new GBT values for NGC 5944 and UGC 11977 so the “compatible within uncertainties, except widths of NGC 5944” statement can be checked.
  4. [Table 1, note 5] UGC 07553: W20,obs = 932 km s−1 with a ~200 km s−1 velocity offset from the optical redshift is extreme; even with the confusion note, a sentence on whether the profile is double-horned, multi-component, or noise-limited at the 20% level would help.
  5. [§1] §1: “All except 5 have previously reported optical redshifts, ranging from 40 to 30,400 km s−1” — identify the five without redshifts (or point to Table 1) for reproducibility.
  6. Keywords and text mix “Hi”, “HI”, and “H i”; adopt one journal style throughout.
  7. [§5] Data availability DOI is given; please confirm the Zenodo record will be public and linked to the final table columns (including which spectra are asterisked) at acceptance.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: pure observational HI catalog; measurements do not reduce to inputs by construction

full rationale

This paper reports GBT 21-cm detections and non-detections for the remaining readily observable UGC LSB targets, plus five serendipitous sources. HI velocities, widths, fluxes, and masses are measured directly from spectra (Table 1) and compared empirically to ALFALFA and the authors' prior LSB sample (O'Neil et al. 2023). The self-citation defines the parent program and supplies a comparison distribution; it does not force the new detection census, the single secure massive object (UGC 11977), or the stated unremarkable character of the additions. No fitted parameter is relabeled as a prediction, no uniqueness theorem is imported, and no quantity is defined in terms of the claimed result. Confusion notes on asterisked profiles are disclosed observational caveats, not circular reasoning. The derivation chain is simply: observe → reduce spectra → tabulate parameters. Score 0 is appropriate.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

Load-bearing content is empirical HI spectroscopy under standard extragalactic radio assumptions. No new physical entities. The few numerical conventions (H0, beam, optical velocity frame) and domain practices (position switching, noise-diode calibration, association of HI with optical counterparts) are inherited from the field; several target-to-profile associations are themselves uncertain as noted in Table 1.

free parameters (2)
  • Hubble constant H0 = 70 km s^{-1} Mpc^{-1}
    Fixed to 70 km s^{-1} Mpc^{-1} to convert velocity to distance and thus HI mass; choice scales all log(M_HI) values.
  • Spectral smoothing resolutions = 5 and 15 km s^{-1}
    Native 0.15 km s^{-1} data smoothed to 5 and 15 km s^{-1}; tabulated values use 5 km s^{-1}, which affects reported widths and S/N of weak lines.
assumptions (4)
  • domain assumption Integrated 21-cm line flux and adopted distance yield total HI mass under standard optically thin conversion.
    Used throughout Table 1 log(M_HI) column; standard in extragalactic HI work but not re-derived here.
  • domain assumption GBT L-band engineering noise diode plus session calibrators provide absolute flux scale.
    Stated in §2 as the calibration path for all fluxes.
  • domain assumption Optical morphological LSB/late-type selection from UGC/HyperLeda traces the intended nearby LSB population.
    Sample definition in §1 inherits Schneider et al. 1990 and O'Neil et al. 2023 selection without new surface-brightness re-measurement in this text.
  • ad hoc to paper An HI line at the pointing is attributable to the named optical galaxy unless notes say otherwise.
    Required to populate Table 1 IDs; contradicted or caveated for multiple asterisked rows in the table notes.

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Cite this review

Pith. "Pith review of Searching in HI for Massive Low Surface Brightness Galaxies: II. Completing the UGC Sample." pith.science (2026). https://pith.science/paper/JEMWR6N4

@misc{pith2026260728180,
  author       = {Pith},
  title        = {Pith review of: Searching in HI for Massive Low Surface Brightness Galaxies: II. Completing the UGC Sample},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JEMWR6N4}},
  note         = {Machine review of arXiv:2607.28180}
}
read the original abstract

Although Low Surface Brightness (LSB) galaxies are increasingly well studied, considerable uncertainty still exists as to both their range in properties and their evolutionary history. LSB galaxies provide a fascinating extreme in galaxy formation and evolution, allowing excellent tests of galaxy formation and evolution theories. Previously, our group successfully measured the HI gas and dynamical mass properties of 350 LSB galaxies, significantly increasing the number of known extreme LSB galaxies (massive, gas rich, etc.) in the process. Here we oresent 100-m Robert C. Byrd Green Bank Telescope 21-cm HI line observations of a further 35 LBG galaxies, only two of which have previously published data. Of the 35, 19 were detected. This paper also includes the HI information for five additional galaxies detected accidentally (in the blank sky region or at alternative velocities), none of which has previously published HI results.

Discussion (0). Continue with ORCID to comment.

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