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arxiv: 2606.26703 · v1 · pith:ECJOWTWFnew · submitted 2026-06-25 · 🌌 astro-ph.GA

Extended Structure in E+A Galaxies Via Image Stacking

Kieran Broadbelt , Kevin Pimbblet , Daniel Farrow , Sugata Kaviraj This is my paper

Pith reviewed 2026-06-26 04:48 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords E+A galaxiespost-starburst galaxiesimage stackingtidal featuresgalaxy interactionssurface brightness profilesGAMA surveySDSS
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The pith

E+A post-starburst galaxies display brighter extended surface brightness profiles than matched non-post-starburst galaxies, revealing faint tidal features from small-scale interactions.

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

The paper stacks 57 SDSS images of E+A galaxies in g, r, and i bands to produce averaged radial surface brightness profiles and compares them to non-PSB galaxies. It reports excess light at large radii in the E+A stacks, which the authors attribute to faint tidal features likely produced by minor mergers, flybys, or harassment. The same excess appears independently in deeper DESI Legacy Survey imaging. A reader would care because the result supplies statistical evidence that small-scale interactions help shape the post-starburst phase without requiring detection of features in single galaxies.

Core claim

Stacking SDSS images of E+A galaxies produces averaged radial surface brightness profiles that are brighter at extended radii than profiles from comparison samples of non-PSB galaxies matched in stellar mass, redshift, and environment. Sersic fits to the stacked profiles, together with independent confirmation from deeper DESI Legacy Survey data, indicate the presence of faint tidal features attributable to small-scale interactions.

What carries the argument

Image stacking to derive averaged radial surface brightness profiles of E+A galaxies, followed by Sersic fitting and comparison to matched non-PSB samples.

If this is right

  • Small-scale interactions are common drivers that can initiate and quench star formation in post-starburst galaxies.
  • Faint tidal features are statistically detectable in E+A populations once individual images are stacked.
  • Deeper wide-field surveys such as LSST will strengthen constraints on the frequency and strength of these extended structures.

Where Pith is reading between the lines

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

  • The stacking approach could be applied to other transitional galaxy classes to uncover similarly subtle morphological signatures.
  • Excess extended light might serve as a statistical proxy for recent interaction history across large galaxy samples.
  • The result suggests that the post-starburst phase is frequently accompanied by low-surface-brightness merger remnants that are missed in single-object studies.

Load-bearing premise

The non-PSB comparison galaxies are matched closely enough in stellar mass, redshift, and environment that differences in extended light arise from the post-starburst property rather than selection or observational biases.

What would settle it

Repeating the stacking analysis on samples re-matched more stringently or on mock images that include only selection effects without tidal features would eliminate the reported excess light at large radii.

Figures

Figures reproduced from arXiv: 2606.26703 by Daniel Farrow, Kevin Pimbblet, Kieran Broadbelt, Sugata Kaviraj.

Figure 1
Figure 1. Figure 1: Restframe 𝑔 − 𝑟 colour vs Petrosian absolute 𝑟-band magnitude diagram used to select for blue star-formers and red quiescents. We use the same delimiting line as in Farrow et al. (2015) and is shown here as a red dashed line. The plot shows the magnitude limited GAMA survey where 𝑟petro < 19.4. From the quiescent and star-forming samples, we create a selection of similar galaxies to our E+A galaxies, match… view at source ↗
Figure 2
Figure 2. Figure 2: Feature spread of the comparison star-forming and quiescent galaxies.The coloured circles represent the star-forming and quiescent galaxies and the solid black squares, the E+A galaxies. Top plot displays the star-forming galaxies, bottom the quiescent galaxies, left displays the spread of 𝑀∗ vs 𝑧 and right 𝑟𝑝 vs 𝑧. 5 COMPARISON STACKS 5.1 SDSS Images The surface brightness profiles in the low S/N stacks a… view at source ↗
Figure 3
Figure 3. Figure 3: Surface brightness profile of the SDSS low S/N E+A stack (left) and the stacked image plot (right). The dashed blue line is the radial profile of the surface brightness fitted by circular bins about the central pixel. The solid orange line indicates the fitted Sérsic profile with the 𝐼𝑒, 𝑟𝑒 and 𝑛 values extracted via pysersic. Top; 𝑔 band, middle; 𝑟 band , and bottom; 𝑖 band [PITH_FULL_IMAGE:figures/full_… view at source ↗
Figure 5
Figure 5. Figure 5: Surface brightness profiles of the low S/N E+A stacks compared to the profiles of the quiescent (left) and star-forming (right) stacks. The solid black line shows the E+A surface brightness profile, with the coloured dashed line representing the comparison mean and the shaded regions representing the comparison spread. Almost all of the E+A stacks show brighter profiles across all radii, with a dip in the … view at source ↗
Figure 6
Figure 6. Figure 6: Surface brightness profiles of the high S/N E+A stacks compared to the profiles of the quiescent (left) and star-forming (right) stacks. The key is the same as in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Difference between the surface brightness profiles of the SDSS low S/N E+A stacks and the comparison quiescent and star-forming stacks. The plots from top to bottom are 𝑔 band data (top), 𝑟 band data (middle), and 𝑖 band data (bottom). The red circles represent the quiescent stacks and the blue triangles represent the star-forming stacks, with the dashed line between points showing the average profile diff… view at source ↗
Figure 9
Figure 9. Figure 9: Surface brightness profiles of the Legacy Survey low S/N E+A stacks compared to the profiles of the quiescent (left) and star-forming (right) stacks. The key is the same as in [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Surface brightness profiles of the Legacy Survey high S/N E+A stacks compared to the profiles of the quiescent (left) and star-forming (right) stacks. The key is the same as in [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Difference between the surface brightness profiles of the Legacy Survey low S/N E+A stacks and the comparison quiescent and star-forming stacks. The plots and key are the same as in [PITH_FULL_IMAGE:figures/full_fig_p014_11.png] view at source ↗
Figure 13
Figure 13. Figure 13: SDSS low S/N E+A radial profiles compared to the PSF kernel used to convolve them. The PSF is shown by the solid black line and the 𝑔𝑟 𝑖 bands are shown by the coloured dashed, dash-dot, and dotted lines respectively. The PSF decreases steeply with radius and as such the PSF wings should not be affecting the E+A surface brightness profiles. in both the E+A samples, likely due to the greater depth revealin… view at source ↗
Figure 14
Figure 14. Figure 14: Difference plot of the SDSS low S/N E+A stack - E+A companion stack. The solid blue line is the 𝑔 band difference, orange dashed line the 𝑟 band difference, and the green dot-dash line the 𝑖 band difference. A positive difference indicates that the standard E+A stack has a brighter central region than that of the companion E+A stack. We find that the companion stack has a brighter extended region but both… view at source ↗
read the original abstract

Small-scale interactions such as minor mergers, flybys and harassment are considered common driving mechanisms that can both initiate and quench star-forming processes within post-starburst (PSB) galaxies. PSBs have been linked to disturbed morphologies and faint tidal features in numerous works. We aim to independently study these features in E+A galaxies found in the Galaxy and Mass Assembly Fourth Data Release (GAMA DR4). Using image stacking techniques, we derive the averaged radial surface brightness profiles of E+A image stacks alongside the S\'ersic parameters that best fit these profiles. These E+A stacks consist of 57 images extracted from the Sloan Digital Sky Survey (SDSS) in g, r & i bands. The E+A stacks are shown to have brighter extended regions than similar non-PSB galaxies, which is indicative of faint tidal features that could be caused by small-scale interactions. Additionally, we make use of Dark Energy Spectroscopic Instrument (DESI) Legacy Survey imaging, which is deeper than SDSS, to further support our conclusions and find that the Legacy Survey images independently strengthen the evidence for excess light at extended radii relative to the comparison samples. We discuss these findings in the context of future surveys such as the Vera C. Rubin Legacy Survey of Space and Time (LSST) survey.

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 / 2 minor

Summary. The manuscript analyzes stacked radial surface-brightness profiles of 57 E+A (post-starburst) galaxies selected from GAMA DR4 using SDSS g, r, and i imaging. Sersic fits to the stacks are compared against control samples of non-PSB galaxies, with the E+A stacks reported to show excess light at large radii. Deeper DESI Legacy Survey imaging is used to corroborate the result, which is interpreted as evidence for faint tidal features driven by small-scale interactions. The work discusses implications for future surveys such as LSST.

Significance. If the control-sample matching holds, the result would provide empirical support for a morphological signature associated with the post-starburst phase at low surface brightness, complementing existing studies of disturbed morphologies in PSBs. The stacking approach and cross-survey comparison are standard techniques that can detect faint extended structure when sample sizes permit.

major comments (1)
  1. [Abstract] Abstract and implied methods: The central claim that E+A stacks exhibit brighter extended regions than 'similar' non-PSB galaxies requires that the comparison samples are matched sufficiently closely in stellar mass, redshift, and environment. No quantitative matching tolerances, tables of median/mean properties, or post-matching statistical tests (e.g., KS tests on mass or local density) are described. Residual differences in these quantities could produce the observed excess light via known correlations with merger-driven structure, independent of the post-starburst selection.
minor comments (2)
  1. [Abstract] Abstract: The E+A sample size (57 galaxies) and exact selection criteria from GAMA DR4 are stated without further detail on redshift range, spectral classification thresholds, or contaminant rejection; adding these would improve reproducibility.
  2. The manuscript does not discuss the impact of sample variance or bootstrap uncertainties on the stacked profiles at large radii, which would help assess the robustness of the reported excess light.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and recommendation for major revision. We address the single major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract and implied methods: The central claim that E+A stacks exhibit brighter extended regions than 'similar' non-PSB galaxies requires that the comparison samples are matched sufficiently closely in stellar mass, redshift, and environment. No quantitative matching tolerances, tables of median/mean properties, or post-matching statistical tests (e.g., KS tests on mass or local density) are described. Residual differences in these quantities could produce the observed excess light via known correlations with merger-driven structure, independent of the post-starburst selection.

    Authors: We agree that explicit documentation of the control-sample matching is required to substantiate the central claim. The manuscript refers to 'similar' non-PSB galaxies but does not provide the quantitative tolerances, summary statistics, or post-matching tests mentioned by the referee. In the revised version we will add a table of median and mean stellar mass, redshift, and local density for the E+A and control samples, state the matching tolerances used, and report Kolmogorov-Smirnov test results on these quantities. These additions will allow readers to evaluate whether residual differences could account for the excess light. revision: yes

Circularity Check

0 steps flagged

No circularity: purely empirical stacking and profile comparison

full rationale

The paper conducts image stacking of SDSS and DESI observations of E+A galaxies, derives averaged radial surface-brightness profiles, fits Sersic models, and compares the extended light to non-PSB control samples matched in mass, redshift and environment. No equations, model predictions, or derivations are present that reduce to fitted parameters or self-citations by construction. All steps (stacking, profile extraction, Sersic fitting) are standard observational procedures applied to external survey data; the central claim is a direct empirical difference, not a self-referential result. The matching of controls is an assumption about sample construction, not a circular reduction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The paper is observational and relies on standard assumptions about image stacking and profile fitting rather than new postulates. No free parameters are introduced to derive a result; the Sersic fits are descriptive.

axioms (2)
  • domain assumption Stacked images faithfully represent the average radial light distribution of the parent population without significant bias from alignment or selection effects.
    Invoked when deriving averaged radial surface brightness profiles from the 57-image stack.
  • standard math Sersic profile is an adequate parametric description of the stacked light distribution for comparison purposes.
    Used to extract parameters that best fit the profiles.

pith-pipeline@v0.9.1-grok · 5766 in / 1428 out tokens · 30336 ms · 2026-06-26T04:48:28.150065+00:00 · methodology

discussion (0)

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Reference graph

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