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arxiv: 2606.16734 · v2 · pith:AGYDUN3Bnew · submitted 2026-06-15 · 🌌 astro-ph.GA

The Edge-on Galaxies in the DESI survey (EGIDE): sample building and photometry

Alexander A. Marchuk , Sergey S. Savchenko , Dmitry I. Makarov , Vladimir P. Reshetnikov , Ilia V. Chugunov , Matvey D. Kozlov , Aleksandra V. Antipova , Anastasia M. Sypkova
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Evgenii V. Rubtsov Dmitry V. Bizyaev
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Pith reviewed 2026-06-27 03:21 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords edge-on galaxiesDESI Legacy Surveygalaxy photometrystellar massgalaxy morphologyblue sequencered cloud
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The pith

A catalogue of 149215 edge-on galaxy candidates from DESI data shows the flattening ratio increases with stellar mass only for redder galaxies.

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

The paper constructs the EGIDE catalogue of 149215 edge-on galaxy candidates from DESI Legacy Imaging Survey DR10 using a Zoobot model fine-tuned on Galaxy Zoo annotations and followed by manual supervision. It supplies uniform SExtractor photometry in griz bands along with stellar masses and redshifts for most objects. Preliminary analysis compares blue sequence and red cloud populations and finds that redder galaxies drop in number faster with rising a/b ratio, are thicker overall, and show a significant increase in flattening ratio q with total stellar mass M_star that is absent in bluer galaxies. The same q-M_star trend at the high-mass end appears independently in statistical models of figures of revolution and in the direct EGIDE observations. The catalogue is ten times larger than earlier efforts and spans more than half the sky.

Core claim

The EGIDE project delivers a public catalogue of 149215 edge-on galaxy candidates with homogeneous griz photometry and stellar masses, and reports that galaxy thickness varies with colour while the flattening ratio q increases with total stellar mass M_star significantly only for redder cloud galaxies, a trend recovered both from statistical models of figures of revolution and from direct observations of the edge-on sample.

What carries the argument

The Zoobot neural model fine-tuned specifically to identify edge-on galaxies from Galaxy Zoo volunteer annotations, followed by manual supervision and SExtractor photometry in griz bands.

If this is right

  • The number of redder galaxies falls with increasing a/b ratio faster than the number of bluer galaxies.
  • Red sequence galaxies are thicker than blue cloud galaxies at fixed mass.
  • The rise in flattening ratio q at the high-mass end is recovered independently by statistical figures-of-revolution models and by direct EGIDE measurements.
  • The full validity of the q-M_star relation for red galaxies requires explicit removal of bulge and PSF contributions.

Where Pith is reading between the lines

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

  • Larger samples like EGIDE could be cross-matched with HI or molecular gas surveys to test whether the mass-dependent thickness in red galaxies correlates with gas depletion.
  • The colour split in thickness trends offers a possible observable for distinguishing merger-driven versus secular growth channels in simulations.
  • Once bulge and PSF corrections are applied, the same catalogue could be used to calibrate thickness measurements for statistical studies of non-edge-on galaxies.

Load-bearing premise

The combination of the fine-tuned Zoobot model and subsequent manual supervision produces a sample whose measured a/b ratios are sufficiently free of contamination and selection bias to support the reported color and mass trends, prior to any correction for bulge light or PSF effects.

What would settle it

An independent visual classification or retraining of the model on the same images that yields no statistically significant difference in the q versus M_star slope between red and blue subsamples would falsify the reported mass-dependent trend.

Figures

Figures reproduced from arXiv: 2606.16734 by Aleksandra V. Antipova, Alexander A. Marchuk, Anastasia M. Sypkova, Dmitry I. Makarov, Dmitry V. Bizyaev, Evgenii V. Rubtsov, Ilia V. Chugunov, Matvey D. Kozlov, Sergey S. Savchenko, Vladimir P. Reshetnikov.

Figure 1
Figure 1. Figure 1: Final distribution of edge-on galaxies from the EGIDE, found in the DESI DR10 footprint, over the sky in the equatorial coordinate system. The grey line symbolically represents the plane of our Galaxy [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Examples of objects classified as truly edge-on galaxies. Ellipses of different colours show segmentation by SEXTRACTOR in different bands. More images can be found in the EGIDE project site https://www.sao. ru/edgeon/catalogs.php?cat=EGIDE. More images can be found in Appendix D and in the EGIDE project site https://www.sao.ru/edgeon/catalogs.php?cat=EGIDE. Rubin, Roman, and Euclid will clearly benefit fr… view at source ↗
Figure 3
Figure 3. Figure 3: Distribution of q versus Kron radius ar in the r-band. In each plot, black contours show the density of EGIDE points (blue). The data are presented before PSF correction (a) and after correction (b, c, d). The horizontal line shows the boundary at q = 0.1; points shown in magenta are filtered out. In panels (c) and (d), coloured isolines show contours of constant relative error of the q = b/a after PSF cor… view at source ↗
Figure 4
Figure 4. Figure 4: Distributions of the photometric properties of galaxies in EGIDE (red hatched), EGIPS (blue), and the volume-limited subsample of EGIDE (green, for 5000 km/s < cz < 15000 km/s, see Section 5). Presented values are the Kron radius in the r band (upper left, panel a), apparent Petrosian magnitude in the r band (upper right, panel b), colour (g − r) (lower left, panel c), and b/a (q-value) in the r band (lowe… view at source ↗
Figure 5
Figure 5. Figure 5: The redshift distribution of edge-on galaxies for the EGIS (green), EGIPS (blue), and EGIDE (red hatched for the whole dataset and magenta for the smaller subsample with information from other surveys) samples. The median cz values for EGIPS and EGIDE are indicated by the vertical dashed lines. Each bin size is 500 km/s. For illustration purposes, we limit the figure to an 80000 km/s range, which contains … view at source ↗
Figure 6
Figure 6. Figure 6: Left: Completeness function in the form of log N versus log ar for EGIDE galaxies. Different colours show the whole sample (black), galaxies with colour 0.7 < (g − r) < 1.2 (red), and galaxies with colour 0.2 < (g − r) < 0.6 (blue). The line marks the linear fit to the whole distribution. Right: Cumulative distribution of apparent magnitude. Individual black lines correspond to the g, r, i, and z bands, an… view at source ↗
Figure 7
Figure 7. Figure 7: Upper: Total stellar mass versus redshift for EGIPS (blue) and EGIDE (red). Isocontours show the density distribution for the EGIDE sample. The blue and black dashed lines schematically show the observational limitations for each mass. In the right subplot, we show histograms of M⋆/M⊙ for both surveys. Lower: Total SFR versus stellar mass relation for galaxies in the intersection of EGIDE with DESI DR1. Is… view at source ↗
Figure 8
Figure 8. Figure 8: The galaxy colour (g − r) versus absolute magnitude in the g-band diagram. The density distribution of the EGIDE galaxies is shown in reddish colours and cyan contours. We show subsamples in three cz-limited bins, marked at the top of each panel. The black solid isocontours illustrate the distribution of a general sample of galaxies from the SDSS DR7 survey, converted into the same photometric system. Earl… view at source ↗
Figure 9
Figure 9. Figure 9: The colour (g − i) versus inverse thickness (a/b) in the r-band for the EGIDE galaxies. In each panel, for comparison, the dashed brown line shows the running median over vertical bins for the EGIPS galaxies. Colours show the density distribution for the whole sample (upper left), for galaxies with a Kron radius larger than 15 arcsec (upper right), and for the mass-limited (lower left) and volume-limited (… view at source ↗
Figure 10
Figure 10. Figure 10: Left: Black points and the latte-colored line of arbitrary width show the flattening b/a of galaxies measured for EGIDE in different stellar mass bins. Blue points represent the b/a peak value for statistical oblate models in [26] (obtained via private communication for most of the bins). The green line and points show b/a measured in DESI DR1 for ∼ 20% of the EGIDE galaxies. Right: Same values as in the … view at source ↗
Figure 11
Figure 11. Figure 11: Left: distribution of the EGIDE galaxies by the a/b axis ratio in the g band. Distributions for different (g − r)-selected subsamples are also shown. Lines represent the linear fits in the given coordinates. Right: points show the dependence of the decline rate of the distribution function of the axis ratios for a given colour bin. Vertical error bars represent 1-σ uncertainties of the fit. Lines with tra… view at source ↗
read the original abstract

We present the EGIDE (The Edge-on Galaxies in the DESI survey) project - a catalogue of 149,215 edge-on galaxy candidates created using the data of the DESI Legacy Imaging Survey DR10 images. The catalogue size is ten times bigger than its predecessor and covers more than half of the sky. It is constructed in an automatic way utilizing the full power of manual annotations from the GalaxyZoo volunteers, implemented in the Zoobot neural model, which was fine-tuned to search for edge-on galaxies specifically. To ensure the credibility of the dataset, subsequent manual supervision was done. The EGIDE catalogue provides homogeneous SExtractor photometry in $griz$ bands, total stellar mass estimation, redshift values for 98% of the sample, star formation rates and other information. All of this is publicly available at The Edge-on Galaxy Database site. The preliminary analysis focused on differences between edge-on galaxies in the so-called blue sequence and red cloud populations. These galaxies demonstrate distinct properties: the number of redder galaxies drops with increasing $a/b$ ratio faster than for the bluer galaxies; galaxy thickness varies with galaxy colour: red sequence galaxies are thicker than blue cloud galaxies; the flattening ratio $q=b/a$ increases with total stellar mass $M_{\star}$ significantly only for redder cloud galaxies. It is an intriguing result, that the same trend of $q$ increasing for the high-mass end is detected from both the statistical models of figures of revolution and direct observations of edge-on galaxies in EGIDE independently. The full extent of the validity of this relationship can only be determined after correctly accounting for the contributions of the bulge and the PSF.

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 / 1 minor

Summary. The paper presents the EGIDE catalogue of 149215 edge-on galaxy candidates selected from DESI Legacy Imaging Survey DR10 using a fine-tuned Zoobot model trained on Galaxy Zoo annotations followed by manual supervision. It supplies homogeneous SExtractor photometry in griz, stellar masses, redshifts (for 98% of objects), star-formation rates and ancillary data, all released publicly. Preliminary analysis compares blue-cloud and red-sequence subsamples and reports that the number of red galaxies declines faster with increasing a/b, that red galaxies are thicker, and that the flattening ratio q = b/a rises with stellar mass M_star significantly only among redder galaxies; the same mass trend appears independently in statistical figures-of-revolution models.

Significance. A tenfold increase in sample size over prior edge-on catalogues, combined with uniform photometry and public release, would constitute a useful resource for statistical studies of disk structure if the selection and photometric measurements are shown to be sufficiently free of bias. The independent detection of the q-M_star trend in both direct observations and statistical models is a positive feature, but its robustness hinges on the unaddressed bulge/PSF corrections explicitly flagged in the abstract.

major comments (2)
  1. [Abstract] Abstract: the reported trend that q = b/a increases with M_star significantly only for redder galaxies is presented as a key result, yet the text states that 'the full extent of the validity of this relationship can only be determined after correctly accounting for the contributions of the bulge and the PSF.' Higher-mass red galaxies are expected to host larger bulges; an uncorrected central excess would systematically raise apparent b/a preferentially in the red sequence, directly threatening the claimed color-dependent mass trend.
  2. [Abstract / sample construction] Sample construction section (implied by abstract description): no quantitative purity, completeness, or contamination estimates are supplied for the Zoobot-selected sample after manual supervision. Because the central scientific claims rest on measured a/b ratios, the absence of these metrics leaves the weakest assumption (that the sample is free of selection bias and contamination sufficient to support the color and mass trends) untested.
minor comments (1)
  1. [Abstract] The abstract states that the catalogue 'covers more than half of the sky' but does not specify the exact sky area or footprint overlap with DESI; adding this would improve reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review and recommendations. We address the major comments point by point below, indicating planned revisions where appropriate.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the reported trend that q = b/a increases with M_star significantly only for redder galaxies is presented as a key result, yet the text states that 'the full extent of the validity of this relationship can only be determined after correctly accounting for the contributions of the bulge and the PSF.' Higher-mass red galaxies are expected to host larger bulges; an uncorrected central excess would systematically raise apparent b/a preferentially in the red sequence, directly threatening the claimed color-dependent mass trend.

    Authors: We appreciate the referee highlighting this potential bias. The abstract already qualifies the result by noting that bulge and PSF corrections are required to determine the full validity of the q-M_star relationship. The same mass-dependent trend is independently recovered from statistical figures-of-revolution models, which are less sensitive to individual bulge contributions. We agree that a more explicit discussion of differential bulge effects between red and blue populations is needed. In revision we will expand the discussion section with a dedicated paragraph on this caveat and its possible impact on the color-dependent trend, while retaining the abstract qualification. revision: partial

  2. Referee: [Abstract / sample construction] Sample construction section (implied by abstract description): no quantitative purity, completeness, or contamination estimates are supplied for the Zoobot-selected sample after manual supervision. Because the central scientific claims rest on measured a/b ratios, the absence of these metrics leaves the weakest assumption (that the sample is free of selection bias and contamination sufficient to support the color and mass trends) untested.

    Authors: We acknowledge that the manuscript does not currently provide quantitative purity, completeness or contamination estimates after the manual supervision stage. The supervision was performed on a representative subset to vet the Zoobot output, but we agree that formal metrics would strengthen confidence in the reported trends. In the revised manuscript we will add a new subsection to the sample construction section that describes the supervision protocol and reports quantitative estimates (e.g., contamination fraction and completeness indicators) derived from the supervised subsample. revision: yes

Circularity Check

0 steps flagged

No circularity: trends derived from independent catalogue photometry and external models

full rationale

The paper constructs the EGIDE sample via Zoobot fine-tuning on Galaxy Zoo annotations plus manual checks, applies SExtractor photometry, estimates M_star, and reports observed q vs M_star trends split by color. The central claim states the same high-mass q increase appears independently in both the EGIDE direct measurements and separate statistical figures-of-revolution models. No equations, fitted parameters, or self-citations are shown that reduce any reported prediction to its own inputs by construction. The derivation chain remains observational and externally benchmarked.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the domain assumption that the Zoobot fine-tuning plus manual supervision yields a sufficiently clean edge-on sample and that SExtractor photometry remains reliable for highly inclined systems.

axioms (1)
  • domain assumption The Zoobot neural model fine-tuned on GalaxyZoo annotations, followed by manual supervision, produces a reliable sample of edge-on galaxies suitable for statistical analysis of a/b ratios.
    Invoked in the sample-building description in the abstract.

pith-pipeline@v0.9.1-grok · 5900 in / 1360 out tokens · 61391 ms · 2026-06-27T03:21:28.121980+00:00 · methodology

discussion (0)

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Reference graph

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