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arxiv: 2607.00953 · v1 · pith:TGXLVB5Inew · submitted 2026-07-01 · 🌌 astro-ph.GA

Projection-Enhanced Disk Breaks: Evidence from Deep Photometric Decomposition

Sergey S. Savchenko , Ilia V. Chugunov , Alexander A. Marchuk , Vladimir P. Reshetnikov , Matvey D. Kozlov , Dmitry I. Makarov , Aleksandra V. Antipova , Anastasia M. Sypkova This is my paper

Pith reviewed 2026-07-02 08:50 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords disk breaksType II breaksedge-on galaxiesphotometric decompositionprojection effectssurface brightness profilesgalaxy morphologyDESI Legacy Survey
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The pith

Projection effects in edge-on galaxies produce Type II breaks in about 90 percent of disks.

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

The paper decomposes the radial brightness profiles of 375 edge-on disk galaxies drawn from DESI Legacy DR10 imaging. It reports that roughly 90 percent show downbending Type II breaks, a much higher share than the 50 percent typical in earlier samples that mixed galaxy orientations. The authors attribute the difference to projection, which increases the apparent surface-brightness contrast of breaks when disks are viewed exactly edge-on. They state that they tested whether flaring or two-disk superpositions could explain the breaks instead.

Core claim

Photometric decomposition of 375 edge-on galaxies shows Type II breaks in approximately 90 percent of the disks. This rate is substantially higher than the fractions reported in previous studies of galaxies at mixed inclinations. The difference is explained by projection, which enhances the observed surface brightness at the break radius in edge-on systems. The authors report that tests rule out flaring and two-disk composition as the main cause of the observed breaks.

What carries the argument

Photometric decomposition applied to deep images of edge-on galaxies to locate and classify radial breaks in surface-brightness profiles, with projection as the mechanism that increases break contrast.

If this is right

  • The intrinsic fraction of Type II breaks across all disk orientations is lower than the rate measured in edge-on samples alone.
  • Break detection efficiency depends on the inclination of the galaxy to the line of sight.
  • Studies that average over random orientations will report lower Type II fractions unless they correct for projection.
  • Edge-on systems give a magnified view of break properties that must be deprojected to compare with face-on disks.

Where Pith is reading between the lines

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

  • Models that tie breaks to star-formation thresholds or bar-driven redistribution may need to predict how the observed break strength varies with viewing angle.
  • Future wide-field surveys could select subsamples by inclination to test whether the Type II fraction drops smoothly as galaxies become more face-on.
  • If projection enhances break visibility, then the physical scale lengths measured at the break in edge-on galaxies may require an inclination-dependent correction before they are used in scaling relations.

Load-bearing premise

The breaks detected in the edge-on sample reflect intrinsic disk structure rather than being produced mainly by disk flaring or the superposition of two separate disks.

What would settle it

A large sample of face-on galaxies analyzed with the same decomposition method showing a Type II fraction near 50 percent rather than 90 percent would indicate that projection is not the dominant driver of the high edge-on rate.

Figures

Figures reproduced from arXiv: 2607.00953 by Aleksandra V. Antipova, Alexander A. Marchuk, Anastasia M. Sypkova, Dmitry I. Makarov, Ilia V. Chugunov, Matvey D. Kozlov, Sergey S. Savchenko, Vladimir P. Reshetnikov.

Figure 1
Figure 1. Figure 1: A schematic face-on view of a galaxy, with three parallel lines of sight piercing it at three distinct points: LOS1 lies inside the break radius, LOS2 passes exactly through the break radius, and LOS3 lies outside of the break radius. It is easy to see that the surface brightness at the locations of LOS2 and LOS3 is governed only by the outer disk density distribution. First, in the edge-on orientation the… view at source ↗
Figure 2
Figure 2. Figure 2: Radial surface brightness for an edge-on and a face-on disk with the same parameters (surface brightness of a model scaled such that for a face-on disk, µ(0) = 21.7 mag/sq.arcsec). The second point is that, due to projection effects, disks in edge-on orientation should have higher values of surface brightness at the same galactocentric distances than the same disks viewed face-on (at least if one considers… view at source ↗
Figure 3
Figure 3. Figure 3: The difference in surface brightness at the break point between an inclined disk and the same disk in the face-on orientation. Different lines correspond disks with different intrinsic thicknesses (see legend). In the conclusion of this section we would like to note that the approach described above, along with the decomposition method (Section 4), treats a galaxy only within the framework of the observed … view at source ↗
Figure 4
Figure 4. Figure 4: demonstrates the results of the decomposition for three galaxies: PGC 90713, PGC 16144, and PGC 49296. The figure shows horizontal slices taken along major axes: blue—the observed bright￾ness distribution, green—the Sérsic function (bulge), red—the BrokenExponentialDisk3D function (disk), and orange—the total model. To exclude dust-contaminated regions (which were masked out), the figure shows the average … view at source ↗
Figure 5
Figure 5. Figure 5: Decomposition results for the same three galaxies as in [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of sample galaxies by absolute magnitude in the r-band (left), radius of 27th-magnitude isophote in the r-band (middle), and stellar mass (right). Numbers of galaxies for which the corresponding parameter was obtained are shown in the top right corners. 0.2 0.3 0.4 0.5 0.6 0.7 0.8 Rb/R27 0 20 40 60 80 N 20 21 22 23 24 25 µedge(Rb) 0 20 40 60 80 N [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Left: Distribution of the sample break radii normalized by the disk’s 27-th magnitude isophote in the r-band. Right: Distribution of breaks by the surface brightnesses at the break point in the r-band. Error bars show Poisson √ N uncertainty. discrepancy: impact of the photometric depth, possible disk flaring and an interplay between two disks (thin and thick) with different radial scales. 5.1.1. Impact of… view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of surface brightness at the break point obtained in this work and recomputed to a face-on orientation (filled blue), compared with measurements from [10,24] (unfilled black). Another interesting result from [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Results of the numerical experiment on the decomposition of a flaring disk by a broken disk model, highlighting how the measured break strength depends on the true value of the flare strength. Solid line: analytical prediction from Equation (9); asterisks: result of one-dimensional decomposition; dots: results of two-dimensional decomposition. sample are stronger than this limit (see Section 5.3). Therefor… view at source ↗
Figure 10
Figure 10. Figure 10: A comparison between our original model containing a single disk with a break (left column) and a model with two disks, one thick and one thin (right column). From top to bottom: image, model, and residual image. Disk parameters are listed at the corresponding model images. Again, this analysis does not imply that galaxies in our sample lack thick disk components, but rather it shows that Type II profile … view at source ↗
Figure 11
Figure 11. Figure 11: Results of the experiment on brightness projection onto a disk plane are shown for four galaxies with Type II breaks. In each panel, the blue line shows a photometric cut along the disk plane, and the red line shows radial brightness distribution of the projection. Both brightness distributions are shifted vertically such that their peaks match. Vertical axes show brightness fading in stellar magnitudes r… view at source ↗
Figure 12
Figure 12. Figure 12: Radial exponential-scale length of an outer disk (normalized by the 27th magnitude isophote radius) vs. surface brightness at the break point (all values in r-band). Left-panel: observed values, right panel: recalculated to the face-on orientation. −2 −1 0 log10 (h2/h1) 22 23 24 25 26 27 µf (Rb) −2 −1 0 log10 (h2/h1) −0.25 0.00 0.25 0.50 0.75 1.00 1.25 1.50 (g − r)b [PITH_FULL_IMAGE:figures/full_fig_p016… view at source ↗
Figure 13
Figure 13. Figure 13: Left panel: face-on surface brightness for break point vs. break strength. Right panel: (g − r) color for break point vs. break strength. Red dots mark disks with strength < −2.0, and blue dots mark those with strength > −2.0. The black dot is a sole galaxy with a Type III break (PGC 731, see Appendix C for details about this object). Crosses mark galaxies that host apparent X-structures. In all cases, th… view at source ↗
Figure 14
Figure 14. Figure 14: Decomposition results for three galaxies with very strong breaks. All markings are the same as in [PITH_FULL_IMAGE:figures/full_fig_p017_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Decomposition results for the same three galaxies as in [PITH_FULL_IMAGE:figures/full_fig_p018_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Results of a test for the degeneracy between bulge parameters and the break strength (see text). Left panel: photometric cuts along the disk plane in the “image-model” residual map for a set of decompositions with different values of bulge-to-total ratio. The solid black line shows the results of the best decomposition, dotted lines represent B/T fixed to larger values, and dot-dashed lines represent B/T … view at source ↗
Figure 17
Figure 17. Figure 17: shows the relation between the integrated disk (g − r) color and the break strength. As in the previous subsection, we divided all the breaks into two subsamples: strong ones (with break strength < −2) and weak ones (with strength > −2). As can be seen from the figure, both groups of breaks exhibit significant correlations. For weak breaks, Pearson’s correlation coefficient is 0.337 (p-value 1.06 · 10−9 )… view at source ↗
Figure 18
Figure 18. Figure 18: Distribution if differences between breaks strengths measured in g and i-bands. For Type II breaks, lower values mean stronger breaks in the g-band. As in [26], we found that the main source of the dependence of break strength on wavelength is related to the changes in the inner disk radial scale rather than the outer one. We computed the normalized average differences between the radial scales of inner a… view at source ↗
Figure 19
Figure 19. Figure 19: Break radius in r-band (left) and stellar mass (right) vs. maximum rotation velocity. 6. Conclusions In this work, we performed two-dimensional photometric decomposition of a sample of 375 disk galaxies viewed in the edge-on orientation. To perform the decomposition, we utilized g-, r- and i-band images from the DESI Legacy DR10 survey, which is considerably more in-depth than many older wide-field survey… view at source ↗
read the original abstract

Radial brightness profiles of disk galaxies often exhibit so-called breaks -- locations where their exponential-scale length abruptly changes. Some galaxies have downbending (Type II) breaks, where their brightness decays faster in outer regions, while other have upbending (Type III) breaks, resulting in more extended outer disks or envelopes. Disk radial profiles without any breaks (Type I) appear to constitute a minority. The exact fractions of different break types depend on many galactic parameters -- such as Hubble type, stellar mass, spatial environment, and bar presence -- and vary significantly across different studies. Another source of discrepancy is the orientation of galaxies: projection effects may play an important role in break detectability. In this work, we utilize DESI Legacy DR10 imaging to perform photometric decomposition of a sample of 375 edge-on galaxies and investigate their radial breaks. We find that the vast majority (~90%) of disks in our sample have Type II breaks, which is a considerably higher fraction than in many previous works (~50%). We carefully tested our results to check if observed breaks can be a result of flaring or two-disk composition. We showed that a high fraction of Type II breaks can be attributed to projection effects, which enhance the observed surface brightness of breaks in edge-on galaxies.

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

1 major / 1 minor

Summary. The manuscript reports photometric decomposition of radial brightness profiles for a sample of 375 edge-on galaxies drawn from DESI Legacy DR10 imaging. It finds that ~90% of the disks exhibit Type II (downbending) breaks, a substantially higher fraction than the ~50% reported in many prior studies, and attributes the difference to projection effects that enhance break visibility in edge-on systems. The authors state that they performed careful tests to exclude flaring and two-disk composition as primary causes.

Significance. If the decomposition pipeline is robust and the tests against flaring and two-disk models are quantitatively convincing, the result would demonstrate that orientation and projection are major drivers of apparent break statistics, helping to reconcile discrepancies across samples with differing inclinations.

major comments (1)
  1. [Abstract and tests section] Abstract and the section describing tests for alternatives: the statement that 'careful tests' were performed to check whether observed breaks can result from flaring or two-disk composition supplies no description of the model-construction procedure, no quantitative comparison metrics (e.g., χ^{2}, BIC, or residual profiles), and no tabulated or plotted outcomes showing that these alternatives fail to reproduce the observed break statistics or radial profiles. Because the central claim that projection effects explain the elevated Type II fraction rests on having ruled out these alternatives, the absence of this information is load-bearing.
minor comments (1)
  1. The abstract and methods summary omit any description of the photometric decomposition algorithm, the functional forms adopted for the disk components, the treatment of sky subtraction or PSF convolution, and the criteria used to classify breaks as Type I/II/III.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for highlighting the need for greater detail on our tests. We address the major comment below.

read point-by-point responses

  1. Referee: [Abstract and tests section] Abstract and the section describing tests for alternatives: the statement that 'careful tests' were performed to check whether observed breaks can result from flaring or two-disk composition supplies no description of the model-construction procedure, no quantitative comparison metrics (e.g., χ^{2}, BIC, or residual profiles), and no tabulated or plotted outcomes showing that these alternatives fail to reproduce the observed break statistics or radial profiles. Because the central claim that projection effects explain the elevated Type II fraction rests on having ruled out these alternatives, the absence of this information is load-bearing.

    Authors: We agree that the current description of the tests is insufficient to fully support the central claim. In the revised manuscript we will add a dedicated subsection that (i) describes the construction of the flaring and two-disk models, (ii) reports quantitative metrics (χ², BIC, and AIC) comparing these alternatives to the fiducial single-disk models with breaks, and (iii) presents residual profiles, summary tables, and figures showing that the alternative models do not reproduce the observed break statistics or radial profiles as well as the fiducial models. These additions will make the exclusion of flaring and two-disk explanations explicit and quantitative. revision: yes

Circularity Check

0 steps flagged

No circularity: empirical decomposition of observed profiles

full rationale

The paper performs photometric decomposition on DESI Legacy imaging of 375 edge-on galaxies and reports an observed ~90% Type II break fraction, attributing the excess to projection. This is a direct measurement from data fitting, not a derivation that reduces to its own inputs by construction. No equations, fitted parameters, or uniqueness theorems are invoked that would make the central statistic equivalent to the input sample by definition. The mention of 'careful tests' for flaring or two-disk models is an empirical check, not a self-referential loop. Self-citations are absent from the provided text and not load-bearing. The result remains falsifiable against external samples and is therefore scored 0.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The analysis depends on standard assumptions in photometric decomposition of galaxy images and the interpretation of projection effects in edge-on systems.

free parameters (1)
  • exponential scale lengths
    Fitted parameters in the radial profile decomposition for inner and outer disks.
axioms (1)
  • domain assumption The surface brightness profiles of disk galaxies can be modeled as piecewise exponential functions with breaks.
    This is the standard approach in studies of galactic disk structure as referenced in the abstract.

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discussion (0)

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Reference graph

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