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arxiv: 2607.00443 · v1 · pith:XLFWSTN6new · submitted 2026-07-01 · 🌌 astro-ph.GA

Optically Selected Superthin Galaxies Remain Thin in the Near-infrared

Jianhong Hu , Cheng Li , Dandan Xu This is my paper

Pith reviewed 2026-07-02 09:33 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords superthin galaxiesdisk axis rationear-infrared morphologygalaxy environmentstellar disk structurebulge-disk decompositionSDSS UKIDSS
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The pith

Optically selected superthin galaxies remain superthin in the near-infrared.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper selects 210 galaxies with disk axis ratios exceeding 9 from SDSS r-band images using two-dimensional bulge-disk decomposition and then tracks their shapes through optical griz and UKIDSS JHK bands. Both major and minor axis lengths shrink toward the near-infrared, reaching roughly 0.6 of their r-band values in the K band, yet the axis ratio itself stays nearly constant. This indicates that the older stellar populations traced by near-infrared light do not build a prominent thick disk. Re-examination of prior samples shows that reported near-infrared thickening arose mainly from biases in one-dimensional fitting. The galaxies also display weaker small-scale clustering and lower local overdensities than matched controls, consistent with residence as central objects in lower-mass, high-spin dark matter halos.

Core claim

Optically selected superthin galaxies defined by disk axis ratios a/b greater than 9 in SDSS r-band images keep essentially the same axis ratios when measured in near-infrared bands, with sizes decreasing but no increase in thickness, showing that old stellar populations do not form a prominent thick disk; earlier apparent thickening is traced to one-dimensional fitting biases, and the sample exhibits lower clustering on 0.1 to 1 h inverse Mpc scales plus lower overdensities at 1 h inverse Mpc.

What carries the argument

Two-dimensional bulge-disk decomposition applied across SDSS griz to UKIDSS JHK bands to extract disk axis ratios and scale lengths.

If this is right

  • Old stellar populations traced by near-infrared light do not produce a prominent thick disk in these galaxies.
  • Reported near-infrared thickening in earlier work stems mainly from magnitude- and band-dependent biases in one-dimensional fitting.
  • Superthin galaxies exhibit lower clustering on scales of 0.1 to 1 h inverse Mpc and lower overdensities at 1 h inverse Mpc.
  • These galaxies are preferentially central objects in relatively low-mass dark matter halos.
  • High host-halo spin contributes to building and preserving extended, vertically thin stellar disks.

Where Pith is reading between the lines

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

  • Galaxy formation models must include channels that preserve thin stellar disks against vertical heating when host halos carry high spin.
  • Multi-band axis-ratio measurements could be extended to other extreme disk samples to check whether thinness is age-independent across populations.
  • The absence of residual large-scale-structure dependence implies that local halo properties outweigh cosmic-web effects in sustaining superthin morphologies.
  • Superthin galaxies may represent a distinct formation pathway for disk galaxies that avoids significant vertical thickening over cosmic time.

Load-bearing premise

The two-dimensional decomposition of SDSS r-band images correctly isolates galaxies whose intrinsic disks have axis ratios above 9 without major contamination from projection effects or component misclassification.

What would settle it

A measurement in which the K-band disk axis ratio for the same galaxies drops substantially below the optical value would falsify the central claim.

Figures

Figures reproduced from arXiv: 2607.00443 by Cheng Li, Dandan Xu, Jianhong Hu.

Figure 1
Figure 1. Figure 1: Distribution of galaxies in the plane of u − r colour versus log10(M∗/M⊙) for the parent volume-limited sample (grey background contours), the subsample of galaxies with major-to￾minor axis ratio a/b > 3 (black dotted), and those with a/b > 3 and UKIDSS data available (red dotted). In all cases, the contour levels are the same, enclosing 90%, 80%, . . . , 10% of a given sam￾ple. The superthin galaxies are … view at source ↗
Figure 2
Figure 2. Figure 2: Examples of galaxies with different ellipticities (1 − b/a). From left to right, the columns show galaxies with ellipticity < 0.6, 0.6–0.7, 0.7–0.8, 0.8–0.89, and > 0.89, respectively. From top to bottom, the rows show the SDSS pseudo-colour image, the SDSS r-band image, and the UKIDSS K-band image. r-band image, and the K-band image from UKIDSS, respec￾tively. Although the number of galaxies is small, the… view at source ↗
Figure 3
Figure 3. Figure 3: Demonstration of the b/a measurement. The upper row shows the disk-only fit with the central region masked, and the lower row shows the final bulge+disk fit. In each row, the three left panels show the observed image, model, and residual, and the two right panels show the profiles along the major and minor axes, indicated by white lines in the images. In the lower-row profile panels, the masked central pix… view at source ↗
Figure 4
Figure 4. Figure 4: Demonstrations of two superthin galaxies across multiple bands (NSA IDs are marked in the first panel of each example). Columns from left to right correspond to the SDSS g, r, i, z bands and the UKIDSS J, H, K bands. For each galaxy, three rows show the observed image, model image, and residual image from top to bottom. The disk component is fitted with an exponential disk profile, with or without a S´ersi… view at source ↗
Figure 5
Figure 5. Figure 5: Superthin galaxy sample. The SDSS pseudo-colour images are divided into two subgroups according to the fitted bulge component: the “bulgeless” subsample is shown in the upper panel, and the bulge subsample is shown in the lower panel. The two subgroups contain 93 and 117 galaxies, respectively. Galaxies in the upper panel are ordered by increasing disk b/a, while those in the lower panel are ordered by inc… view at source ↗
Figure 6
Figure 6. Figure 6: Differential (histogram) and cumulative (dashed line) distributions of the r-band bulge-to-total luminosity ratio (B/T) of the superthin galaxy sample. The horizontal dotted line indicates the fraction of bulgeless galaxies, ∼ 44%. row the panels from left to right display the observed image, the model image, the residual in the model-subtracted image, and the surface brightness profile along the major and… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of disk shape parameters in other bands with those in the r band. Three rows from top to bottom correspond to a, b, and b/a of the exponential disk model, all in logarithmic scale. The x-axis shows parameters in the r band, and the y-axis shows parameters in other bands: SDSS g, i, z, and UKIDSS J, H, K. All parameters are normalized by their mean value in the r band. The dashed diagonal line in… view at source ↗
Figure 9
Figure 9. Figure 9: Distribution of the superthin galaxy samples from B17 (blue triangles) and the present work (red crosses) in the diagram of z-band absolute magnitude versus redshift. The horizontal and vertical dashed lines indicate the sample selection criteria of the present work. 1 2 3 1D/1Dr this work B17 rs B20 hs hs/rs 1 2 3 2D/2Dr g r i z J H K 1 2 3 1D/2D g r i z J H Kg r i z J H K [PITH_FULL_IMAGE:figures/full_f… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the 1D and 2D measurements for our sample (red) and the B17 sample (blue). The three columns cor￾respond to rs, hs, and hs/rs. The upper two rows show band-to-r ratios measured with the 1D and 2D methods, respectively, and the bottom row shows the ratio between the 1D and 2D measure￾ments. Lines and shaded regions show the median and [0.2, 0.8] quantile range, as in [PITH_FULL_IMAGE:figures… view at source ↗
Figure 11
Figure 11. Figure 11: Disk shape parameters from the 1D and 2D methods as a function of galaxy apparent magnitude. Columns from left to right correspond to the SDSS griz bands and the UKIDSS JHK bands, respectively. The top three rows show the logarithmic difference between the two methods (log10(1D/2D) for rs, hs, and hs/rs of the edge-on disk model; Eq. (4)). The bottom two rows show log10(hs/rs) from the 1D and 2D methods, … view at source ↗
Figure 12
Figure 12. Figure 12: Projected cross-correlation functions for the superthin samples (blue solid lines) and their matched control samples (red dashed lines). From left to right, the panels show the full superthin sample, the “bulgeless” subsample, and the bulge subsample. nificantly larger hs/rs, while our sample leads to the same results as obtained above with the 2D method. The panels in the middle row show that, when the 2… view at source ↗
Figure 13
Figure 13. Figure 13: Cumulative distributions of local overdensity, shown as a function of log10(ρ/ρ¯), for the superthin samples and their matched control samples. Line styles and panel columns are the same as in [PITH_FULL_IMAGE:figures/full_fig_p012_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Fractions of galaxies in different large-scale-structure types for the superthin samples (blue) and their matched control samples (red). Panel columns are the same as in [PITH_FULL_IMAGE:figures/full_fig_p013_14.png] view at source ↗
read the original abstract

We investigate whether galaxies identified as superthin in optical images remain superthin in the near-infrared (NIR), and how their extreme disk morphology is related to environment. From a nearby volume-limited sample, we select 210 superthin galaxies using two-dimensional bulge/disk decomposition of SDSS $r$-band images, requiring the disk component to have a major-to-minor axis ratio $a/b>9$. We measure disk shapes from SDSS $griz$ to UKIDSS $JHK$ bands. Both the major- and minor-axis scales decrease from the optical to the NIR, reaching $\sim0.6$ of their $r$-band values in the $K$ band, but the disk axis ratio remains nearly unchanged. Thus, optically selected superthin galaxies remain superthin in the NIR, implying that the old stellar populations traced by NIR light do not form a prominent thick disk. Reanalysis of our sample and a previous superthin sample shows that earlier reported NIR thickening is mainly due to a magnitude- and band-dependent bias in one-dimensional fitting. We further compare their environments with matched control samples using projected cross-correlations, reconstructed local overdensities, and large-scale-structure classifications. Superthin galaxies show lower clustering on $\sim0.1$--$1\,h^{-1}\,\mathrm{Mpc}$ scales and lower overdensities at $1\,h^{-1}\,\mathrm{Mpc}$, but no clear residual dependence on large-scale-structure type. These results suggest that superthin galaxies are preferentially central galaxies in relatively low-mass dark matter halos, consistent with a picture in which high host-halo spin helps build and preserve extended, vertically thin stellar disks.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper selects 210 superthin galaxies (disk component a/b >9 from 2D bulge/disk decomposition of SDSS r-band images) in a nearby volume-limited sample. It measures major- and minor-axis scales and axis ratios from SDSS griz through UKIDSS JHK, finding sizes shrink to ~0.6 of r-band values in K but axis ratios stay nearly constant. This implies optically selected superthin galaxies remain superthin in NIR, so old stellar populations lack a prominent thick disk. The authors reanalyze their sample plus a prior one to attribute earlier NIR-thickening reports to 1D fitting bias. Environmental analysis via projected cross-correlations, local overdensities, and LSS classification shows lower clustering on 0.1-1 h^{-1} Mpc scales and lower overdensities, suggesting superthin galaxies are centrals in low-mass, high-spin halos.

Significance. If the result holds, the work constrains disk vertical structure by showing old stars do not build thick disks in these systems and supports halo-spin models for preserving thin disks. The explicit correction for 1D fitting bias via reanalysis is a clear strength, as is the use of public multi-band photometry and statistical environmental metrics. The environmental findings add context on morphology-density relations.

major comments (2)
  1. [Sample selection] The central claim that the r-band 2D decomposition cleanly selects galaxies with intrinsic disk a/b >9 (without significant projection effects, PSF convolution errors, or component misidentification) is load-bearing for interpreting unchanged NIR axis ratios, yet the manuscript provides no quantitative robustness tests at this extreme threshold (e.g., varying initial guesses, profile assumptions, or PSF impact); see the sample selection description.
  2. [Environmental analysis] Details on control-sample matching criteria (stellar mass, redshift, luminosity) and error propagation for the projected cross-correlations and reconstructed overdensities are not reported, weakening assessment of the reported differences on ~0.1-1 h^{-1} Mpc scales and the halo-spin interpretation; see the environmental analysis section.
minor comments (2)
  1. [Abstract] The abstract states that 'earlier reported NIR thickening is mainly due to a magnitude- and band-dependent bias in one-dimensional fitting' but does not reference the specific section presenting the reanalysis and bias quantification.
  2. [Throughout] Notation for axis ratio (observed vs. intrinsic, major-to-minor definition) should be stated explicitly and used consistently when reporting values across bands.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments. We address the two major comments point by point below and will revise the manuscript to incorporate the requested details and tests.

read point-by-point responses

  1. Referee: [Sample selection] The central claim that the r-band 2D decomposition cleanly selects galaxies with intrinsic disk a/b >9 (without significant projection effects, PSF convolution errors, or component misidentification) is load-bearing for interpreting unchanged NIR axis ratios, yet the manuscript provides no quantitative robustness tests at this extreme threshold (e.g., varying initial guesses, profile assumptions, or PSF impact); see the sample selection description.

    Authors: We agree that explicit quantitative robustness tests at the a/b >9 threshold would strengthen the sample selection. In the revised manuscript we will add a dedicated subsection reporting results from (i) repeated decompositions with varied initial guesses, (ii) fits performed with and without a bulge component, and (iii) an assessment of PSF convolution effects on recovered axis ratios for galaxies near the selection boundary. These tests will be performed on both the full sample and a representative subset. revision: yes

  2. Referee: [Environmental analysis] Details on control-sample matching criteria (stellar mass, redshift, luminosity) and error propagation for the projected cross-correlations and reconstructed overdensities are not reported, weakening assessment of the reported differences on ~0.1-1 h^{-1} Mpc scales and the halo-spin interpretation; see the environmental analysis section.

    Authors: We acknowledge that the current text omits the precise matching tolerances and error-propagation procedures. The revised version will specify the exact criteria (including bin widths or tolerances in stellar mass, redshift, and luminosity) used to construct the control samples and will describe the error estimation methods, including any bootstrap or jackknife resampling applied to the projected cross-correlation functions and local overdensities. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational selection and band-to-band measurement with no self-referential derivations or load-bearing self-citations

full rationale

The paper performs a volume-limited selection of galaxies via public SDSS r-band 2D bulge/disk decompositions (a/b > 9 threshold), then measures the same axis ratios in grizJHK bands from the same and additional public surveys. No equations, fitted parameters, or predictions are defined in terms of the target result; the axis-ratio invariance is a direct empirical outcome. The reanalysis of prior 1D-fitting biases references earlier literature (including possibly overlapping samples) but is not required to establish the central NIR-thinness claim, which rests on independent photometry. This matches the default expectation for an observational catalog study whose central result is externally falsifiable against the input imaging data.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the accuracy of photometric decomposition for sample selection and the interpretation of clustering statistics as tracers of halo mass and spin; no new entities are postulated.

free parameters (1)
  • axis ratio threshold a/b >9
    Selection cut used to define the superthin sample from r-band decompositions; chosen rather than fitted but directly determines which objects enter the analysis.
axioms (1)
  • domain assumption Two-dimensional bulge/disk decomposition of SDSS r-band images yields reliable major-to-minor axis ratios for disk components
    Invoked when selecting the 210 galaxies and when comparing shapes across bands.

pith-pipeline@v0.9.1-grok · 5841 in / 1374 out tokens · 33957 ms · 2026-07-02T09:33:39.922297+00:00 · methodology

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Reference graph

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