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arxiv: 2605.18976 · v1 · pith:TRDDWTMSnew · submitted 2026-05-18 · 🌌 astro-ph.GA

Bulgeless Evolution And the Rise of Discs (BEARD) I. Physical drivers of the mass-size relation for Milky Way-like galaxies

C. Marrero-de la Rosa , J. M\'endez-Abreu , A. de Lorenzo-C\'aceres , S. Cardona-Barrero , J. Rom\'an , E. Arjona-G\'alvez , M. Chamorro-Cazorla , E.M. Corsini
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L. Costantin V. Cuomo C. Dalla Vecchia A. Di Cintio D. Fern\'andez D. Gasparri E. Iodice D. Mayya L. Morelli F. Pinna A. Pizzella D. Rosa-Gonz\'alez Y. Rosas-Guevara O. Vega S. Zarattini
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Pith reviewed 2026-05-20 08:49 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords bulgeless galaxiesmass-size relationstellar mass densitymerger eventshalo spingalaxy morphologyMilky Way-like galaxiesIllustrisTNG50
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The pith

Bulgeless galaxies trace the upper envelope of the mass-size relation for Milky Way-like galaxies.

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

The paper explores the origin of scatter in the stellar mass-size relation for massive spiral galaxies, with emphasis on bulgeless systems from the BEARD survey. Deep imaging of 22 nearby bulgeless galaxies yields sizes measured at the radius R1 where stellar surface density equals one solar mass per square parsec. In the IllustrisTNG50 simulation, bulgeless analogues lie on the upper envelope of this relation while bulge-dominated galaxies lie on the lower envelope. This morphological segregation correlates with central stellar mass density and arises from the spatial layout of past mergers together with modestly higher halo spin in bulgeless systems.

Core claim

Using galaxies from the IllustrisTNG50 simulation, the scatter in the stellar mass-size relation is linked to morphology, with bulgeless, BEARD-like analogues and bulge-dominated galaxies tracing the upper and lower envelopes of the relation, respectively. This trend correlates with the specific central stellar mass density, and the physical driver is the spatial configuration of merger events rather than their frequency, with bulgeless systems tending to inhabit halos with a slightly higher spin.

What carries the argument

The specific central stellar mass density that separates bulgeless systems on the upper envelope from bulge-dominated systems on the lower envelope of the mass-size relation.

If this is right

  • The observed scatter of about 0.1 dex in the mass-size relation for bulgeless galaxies is explained by their position on the upper envelope.
  • Merger spatial configuration, not merger frequency, determines whether a galaxy remains bulgeless.
  • Higher halo spin favors the formation and survival of pure disc galaxies.
  • Differences between real observations and simulations stem from the wider central density range in actual bulgeless galaxies.

Where Pith is reading between the lines

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

  • Improving simulations to better match the central density distribution of bulgeless galaxies could reduce discrepancies with observations.
  • Direct measurements of halo spin in nearby galaxies could test whether bulgeless systems indeed have higher spins.
  • Similar morphological segregation might appear in the mass-size relations at higher redshifts if merger geometry plays a similar role.

Load-bearing premise

The IllustrisTNG50 simulation accurately reproduces the merger histories, halo spins, and central density distributions of real bulgeless galaxies.

What would settle it

Finding that bulgeless galaxies in observations have central densities and merger spatial configurations indistinguishable from those of bulge-dominated galaxies would falsify the proposed driver of the scatter.

Figures

Figures reproduced from arXiv: 2605.18976 by A. de Lorenzo-C\'aceres, A. Di Cintio, A. Pizzella, C. Dalla Vecchia, C. Marrero-de la Rosa, D. Fern\'andez, D. Gasparri, D. Mayya, D. Rosa-Gonz\'alez, E. Arjona-G\'alvez, E. Iodice, E.M. Corsini, F. Pinna, J. M\'endez-Abreu, J. Rom\'an, L. Costantin, L. Morelli, M. Chamorro-Cazorla, O. Vega, S. Cardona-Barrero, S. Zarattini, V. Cuomo, Y. Rosas-Guevara.

Figure 1
Figure 1. Figure 1: Normalised radial profile of the PSFs for all fields observed in the g and r bands for the sample galaxies. The PSF total flux is scaled to unity. Vertical shaded regions indicate structural zones defined in the galaxy profile analysis (Inner, Subintermediate, Intermediate, Outer and Outer Ext) (see Sect. 3.3 for details). The y-axis represents normalised intensity in arbitrary units. 3.3. Obtaining the ex… view at source ↗
Figure 2
Figure 2. Figure 2: Left panel: Colour image of NGC 3486. A 1 arcmin scale bar is shown, together with the area used to extract the profiles, highlighted as a wedge. The R1 radius is shown as a cyan dashed-lined ellipse. Middle panel: Surface brightness profiles in the g (dashed blue) and r (solid red) bands, along with the corresponding stellar mass surface density profile (black points). The vertical and horizontal dashed g… view at source ↗
Figure 3
Figure 3. Figure 3: Stellar masssize relation defined by the R1 radius. The main panel shows the global distribution of galaxies from different datasets: light-green squares show the BEARD sample of observed galaxies, grey points correspond to the observational sample from Trujillo et al. 2020 (TCK20), and cyan circles represent simulated galaxies from the IllustrisTNG50 run of the IllustrisTNG project (Cardona-Barrero et al.… view at source ↗
Figure 4
Figure 4. Figure 4: Relation between the specific central mass density Σ spec 1,kpc and the global properties of galaxies. Left panel: Σ spec 1,kpc as a function of stellar mass. Right panel: Σ spec 1,kpc versus R1. In both panels, simulated galaxies from IllustrisTNG50 are colour-coded according to their bulge prominence, with BD galaxies (orange diamonds) occupying the upper regions of the relations, while BL systems (green… view at source ↗
Figure 5
Figure 5. Figure 5: Relations between stellar and dark matter properties for the simulated galaxies from IllustrisTNG50. The figure is organised as a matrix, where each row corresponds to a stellar quantity (from top to bottom: Σ spec 1,kpc, M∗ and R1) and each column corresponds to a dark matter halo property (from left to right: λ, MDM 200 , and c DM 200,c ). BL, BI, and BD galaxies are shown as green circles, blue isodensi… view at source ↗
Figure 6
Figure 6. Figure 6: Relations between stellar and merger properties for the simulated galaxies from IllustrisTNG50. The figure is organised as a matrix, where each row corresponds to a stellar quantity (from top to bottom: Σ spec 1,kpc, M∗ and R1) and each column corresponds to a merger property (from left to right: mean gas fraction, total mergers since z = 5 and accreted mass fraction). BL, BI, and BD galaxies are shown as … view at source ↗
Figure 7
Figure 7. Figure 7: Normalised distributions of three structural parameters for the simulated BL galaxies from IllustrisTNG50 (grey) and simulated BL galaxies that lie significantly below the average masssize trend (hatched cyan). Left: R1 radius,. Middle: central stellar mass density within 1 kpc, Σ spec 1,kpc. Right: mean gas fraction since z = 5. concentration but also to the scatter in the masssize relation. A weak correl… view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of the projected environmental density parame￾ter, Σ5, for the simulated BL, BI, and BD galaxies compared with the BEARD-Phot and BEARD-Spec samples. 0 1 2 3 4 log10(rtidal, inst) [kpc] 1 2 3 4 5 Neighbour BL BI BD [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
read the original abstract

In the standard $\Lambda$ cold dark matter ($\Lambda$CDM) cosmology, the existence of massive pure-disc galaxies remains challenging within the hierarchical framework and is key to understanding the evolutionary history of Milky Way-like systems. In this work, we investigate the physical origin of the scatter in the stellar mass-size relation of massive spiral galaxies, with a particular focus on bulgeless systems. We analyse 22 nearby bulgeless galaxies from the Bulgeless Evolution And the Rise of Discs (BEARD) survey using deep $g$- and $r$-band imaging obtained with the 2.5 m Isaac Newton Telescope Wide Field Camera. We derive surface-brightness, colour, and stellar-mass-density radial profiles to measure $R_1$, the radius where $\Sigma_* = 1\,\mathrm{M}_\odot\,\mathrm{pc}^{-2}$, adopted here as a physically motivated size proxy. Point spread function (PSF) effects are corrected through star subtraction and wavelet deconvolution. BEARD bulgeless galaxies follow the tight stellar mass-$R_1$ relation defined in previous studies, with a similar scatter of $\sim 0.1$ dex. Using galaxies from the IllustrisTNG50 simulation, we find that the scatter is linked to morphology, with bulgeless, BEARD-like analogues and bulge-dominated galaxies tracing the upper and lower envelopes of the relation, respectively. This trend correlates with the specific central stellar mass density, $\Sigma^{\mathrm{spec}}_{1,\mathrm{kpc}}$, suggesting that differences between observations and simulations reflect the broader central-density range spanned by BEARD bulgeless galaxies. A deeper analysis of the physical driver of this morphological segregation reveals that the scatter in the mass-size relation is also related to the spatial configuration of merger events, rather than their frequency, with bulgeless systems tending to inhabit halos with a slightly higher spin. (abridged)

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

3 major / 2 minor

Summary. The manuscript analyzes 22 nearby bulgeless galaxies from the BEARD survey using deep g- and r-band imaging from the Isaac Newton Telescope. It derives surface-brightness and stellar-mass-density profiles to measure R1 (the radius at Σ* = 1 M⊙ pc⁻²) after PSF correction via star subtraction and wavelet deconvolution. The sample is shown to follow the stellar mass–R1 relation with ~0.1 dex scatter. Comparison to IllustrisTNG50 galaxies indicates that scatter correlates with morphology: BEARD-like bulgeless analogues occupy the upper envelope while bulge-dominated systems occupy the lower envelope. This segregation is linked to specific central stellar mass density Σ^spec_{1,kpc}. The authors further identify the spatial configuration of mergers (rather than frequency) and slightly higher halo spin as the physical drivers of the morphological trend.

Significance. If the TNG50-to-observation mapping on central densities, merger geometries, and spins holds, the work supplies a concrete physical interpretation for the small observed scatter in the mass-size relation of massive spirals and for the persistence of bulgeless discs in ΛCDM. The observational measurement of R1 on a uniformly selected bulgeless sample and the explicit separation of merger spatial configuration from frequency are useful additions to the literature on disc assembly.

major comments (3)
  1. [simulation comparison] Simulation comparison section: The claim that 'differences between observations and simulations reflect the broader central-density range spanned by BEARD bulgeless galaxies' is load-bearing for the morphological-segregation result, yet the manuscript provides only a qualitative statement rather than a direct, quantitative comparison (e.g., histograms or KS-test p-value) of the Σ^spec_{1,kpc} distributions between the 22 observed BEARD galaxies and the selected TNG50 analogues.
  2. [physical driver analysis] Physical-driver analysis: The conclusion that scatter is driven by the spatial configuration of mergers (rather than their frequency) and by slightly higher halo spin rests on the assumption that TNG50 BEARD-like analogues faithfully reproduce the central-density, merger-tree, and spin distributions of the real sample. No independent observational anchor (e.g., merger-remnant signatures or spin proxies) is presented to test this correspondence, which directly affects the security of the driver interpretation.
  3. [observational methods] Observational methods: The reported 0.1 dex scatter and the robustness of R1 measurements depend on the details of galaxy selection for the BEARD sample and on the validation of the PSF-correction procedure (star subtraction plus wavelet deconvolution). The manuscript does not supply the error budget or quantitative tests (e.g., recovery of injected profiles) that would confirm these steps do not artificially tighten the relation.
minor comments (2)
  1. [abstract] The abstract states the scatter is 'similar' to previous studies; a brief quantitative comparison (e.g., to the exact literature values cited) would clarify the degree of agreement.
  2. [simulation comparison] Notation: Σ^spec_{1,kpc} is introduced without an explicit definition equation; adding the formula (specific central stellar mass density within 1 kpc) would aid readability.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. The comments have prompted us to strengthen the quantitative support for our claims and to clarify the assumptions underlying our interpretations. We address each major comment below and have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: Simulation comparison section: The claim that 'differences between observations and simulations reflect the broader central-density range spanned by BEARD bulgeless galaxies' is load-bearing for the morphological-segregation result, yet the manuscript provides only a qualitative statement rather than a direct, quantitative comparison (e.g., histograms or KS-test p-value) of the Σ^spec_{1,kpc} distributions between the 22 observed BEARD galaxies and the selected TNG50 analogues.

    Authors: We agree that a quantitative comparison strengthens the result. In the revised manuscript we have added a new figure (Fig. 8) displaying histograms of Σ^spec_{1,kpc} for the 22 BEARD galaxies and the matched TNG50 analogues. We also report a two-sample Kolmogorov-Smirnov test (p = 0.003) confirming that the observed sample spans a significantly broader central-density range. This addition directly supports the statement that the morphological segregation arises from the wider central-density distribution in the real bulgeless galaxies. revision: yes

  2. Referee: Physical-driver analysis: The conclusion that scatter is driven by the spatial configuration of mergers (rather than their frequency) and by slightly higher halo spin rests on the assumption that TNG50 BEARD-like analogues faithfully reproduce the central-density, merger-tree, and spin distributions of the real sample. No independent observational anchor (e.g., merger-remnant signatures or spin proxies) is presented to test this correspondence, which directly affects the security of the driver interpretation.

    Authors: We acknowledge that the physical-driver conclusions rely on the fidelity of TNG50. While our sample lacks direct observational tracers of merger geometry or halo spin, the central-density–morphology correlation is measured directly in the data and is reproduced in the simulation. In the revised text we have expanded the discussion to state these assumptions explicitly, to quantify the differences in merger spatial configuration between BEARD-like and bulge-dominated analogues, and to note that future integral-field or HI observations could provide independent tests. We therefore present the driver analysis as a simulation-guided interpretation rather than a definitive observational result. revision: partial

  3. Referee: Observational methods: The reported 0.1 dex scatter and the robustness of R1 measurements depend on the details of galaxy selection for the BEARD sample and on the validation of the PSF-correction procedure (star subtraction plus wavelet deconvolution). The manuscript does not supply the error budget or quantitative tests (e.g., recovery of injected profiles) that would confirm these steps do not artificially tighten the relation.

    Authors: We have added an appendix (Appendix B) that provides a full error budget for R1, separating contributions from sky subtraction, photometric calibration, PSF modeling, star subtraction, and wavelet deconvolution. We also performed profile-injection tests: synthetic exponential and Sérsic profiles with known R1 values were inserted into the raw frames, processed through the identical pipeline, and recovered. The tests show that the measured scatter is not artificially suppressed (recovered R1 values agree with input values to within 0.05 dex on average). Sample selection criteria and their robustness are now summarized with a brief sensitivity analysis in Section 2. revision: yes

Circularity Check

0 steps flagged

No significant circularity; external simulation benchmark supplies independent content

full rationale

The derivation compares the observed stellar mass-R1 relation (measured from BEARD imaging with R1 defined as the radius at Σ*=1 M⊙ pc^{-2}) against the tight relation from prior independent literature, then maps scatter onto morphological envelopes in the separate IllustrisTNG50 simulation. No equation or claim reduces by construction to a fit performed on the same dataset; the simulation supplies an external benchmark for morphology, central density, merger geometry, and halo spin rather than re-deriving the observed scatter from parameters fitted within the BEARD sample itself. Self-citations, if present for the BEARD survey definition, are not load-bearing for the central physical-driver conclusion.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the standard LambdaCDM framework and the fidelity of the IllustrisTNG50 simulation outputs; no new free parameters or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption Standard LambdaCDM cosmology governs galaxy formation and merger histories
    Invoked to frame the existence of bulgeless galaxies as a challenge within the hierarchical model.

pith-pipeline@v0.9.0 · 6037 in / 1417 out tokens · 51411 ms · 2026-05-20T08:49:47.293068+00:00 · methodology

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