pith. sign in

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
show 15 more authors
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
This is my paper

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
0
0 comments X

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

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

104 extracted references · 104 canonical work pages · 45 internal anchors

  1. [1]

    , keywords =

    Baryonic imprints on DM haloes: population statistics from dwarf galaxies to galaxy clusters. , keywords =. doi:10.1093/mnras/stab3177 , archivePrefix =. 2109.02713 , primaryClass =

    work page doi:10.1093/mnras/stab3177

  2. [2]

    Research Notes of the American Astronomical Society , keywords =

    Gnuastro: Visualizing the Full Dynamic Range in Color Images. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/ad1aae , archivePrefix =. 2401.03814 , primaryClass =

    work page doi:10.3847/2515-5172/ad1aae

  3. [3]

    M. A. Stephens , journal =. EDF Statistics for Goodness of Fit and Some Comparisons , urldate =

    work page

  4. [4]

    , keywords =

    A multidimensional version of the Kolmogorov-Smirnov test. , keywords =. doi:10.1093/mnras/225.1.155 , adsurl =

    work page doi:10.1093/mnras/225.1.155

  5. [5]

    Planck 2015 results. XXVII. The second Planck catalogue of Sunyaev-Zeldovich sources. , keywords =. doi:10.1051/0004-6361/201525823 , archivePrefix =. 1502.01598 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525823 2015

  6. [6]

    MNRAS , eprint =

    The inner structure of CDM haloes - I. A numerical convergence study. , keywords =. doi:10.1046/j.1365-8711.2003.05925.x , archivePrefix =. astro-ph/0201544 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.05925.x 2003

  7. [7]

    , keywords =

    ERGO-ML I: inferring the assembly histories of IllustrisTNG galaxies from integral observable properties via invertible neural networks. , keywords =. doi:10.1093/mnras/stac3295 , archivePrefix =. 2202.06967 , primaryClass =

    work page doi:10.1093/mnras/stac3295

  8. [8]

    The role of mergers and halo spin in shaping galaxy morphology

    The role of mergers and halo spin in shaping galaxy morphology. , keywords =. doi:10.1093/mnras/stx305 , archivePrefix =. 1609.09498 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx305

  9. [9]

    , keywords =

    Dynamical Structure of Small Bulges Reveals Their Early Formation in CDM Paradigm. , keywords =. doi:10.3847/2041-8213/ab6459 , archivePrefix =. 2001.04984 , primaryClass =

    work page doi:10.3847/2041-8213/ab6459 2041

  10. [10]

    , keywords =

    Expectations of the Size Evolution of Massive Galaxies at 3 z 6 from the TNG50 Simulation: The CEERS/JWST View. , keywords =. doi:10.3847/1538-4357/acb926 , archivePrefix =. 2208.00007 , primaryClass =

    work page doi:10.3847/1538-4357/acb926

  11. [11]

    Stellar masses of SDSS-III BOSS galaxies at z~0.5 and constraints to galaxy formation models

    Stellar masses of SDSS-III/BOSS galaxies at z 0.5 and constraints to galaxy formation models. , keywords =. doi:10.1093/mnras/stt1424 , archivePrefix =. 1207.6114 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1424

  12. [12]

    The influence of diffuse scattered light. I. The PSF and its role in observations of the edge-on galaxy NGC 5907. , keywords =. doi:10.1051/0004-6361/201423429 , archivePrefix =. 1406.5508 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423429

  13. [13]

    , keywords =

    Galactic cirri in deep optical imaging. , keywords =. doi:10.1051/0004-6361/201936111 , archivePrefix =. 1907.00978 , primaryClass =

    work page doi:10.1051/0004-6361/201936111 1907

  14. [14]

    NIHAO XXI: The emergence of Low Surface Brightness galaxies

    NIHAO XXI: the emergence of low surface brightness galaxies. , keywords =. doi:10.1093/mnras/stz985 , archivePrefix =. 1901.08559 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz985 1901

  15. [15]

    C., Glover, S

    Hierarchical formation of bulgeless galaxies: why outflows have low angular momentum. , keywords =. doi:10.1111/j.1365-2966.2011.18545.x , archivePrefix =. 1010.1004 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18545.x 2011

  16. [16]

    2010, MNRAS, 401, 791, doi:10.1111/j.1365-2966.2009

    Forming a large disc galaxy from a z < 1 major merger. , keywords =. doi:10.1111/j.1365-2966.2009.15143.x , archivePrefix =. 0812.0379 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15143.x 2009

  17. [17]

    At the heart of the matter: the origin of bulgeless dwarf galaxies and Dark Matter cores

    Bulgeless dwarf galaxies and dark matter cores from supernova-driven outflows. , keywords =. doi:10.1038/nature08640 , archivePrefix =. 0911.2237 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature08640

  18. [18]

    Discovery of disc truncations above the galaxies' mid-plane in Milky Way-like galaxies

    Discovery of disc truncations above the galaxies' mid-plane in Milky Way-like galaxies. , keywords =. doi:10.1093/mnras/sty2886 , archivePrefix =. 1804.01546 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2886

  19. [19]

    , keywords =

    Are ultra-diffuse galaxies Milky Way-sized?. , keywords =. doi:10.1051/0004-6361/201936821 , archivePrefix =. 2001.02691 , primaryClass =

    work page doi:10.1051/0004-6361/201936821 2001

  20. [20]

    Star formation thresholds and galaxy edges: why and where

    Star Formation Thresholds and Galaxy Edges: Why and Where. , keywords =. doi:10.1086/421232 , archivePrefix =. astro-ph/0205125 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/421232

  21. [21]

    The Gaia mission

    The Gaia mission. , keywords =. doi:10.1051/0004-6361/201629272 , archivePrefix =. 1609.04153 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629272

  22. [22]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.1051/0004-6361/202243940

  23. [23]

    Total Galaxy Magnitudes and Effective Radii from Petrosian Magnitudes and Radii

    Total Galaxy Magnitudes and Effective Radii from Petrosian Magnitudes and Radii. , keywords =. 2005a , month = oct, volume =. doi:10.1086/444475 , archivePrefix =. astro-ph/0504287 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/444475

  24. [24]

    Color Separation of Galaxy Types in the Sloan Digital Sky Survey Imaging Data

    Color Separation of Galaxy Types in the Sloan Digital Sky Survey Imaging Data. , keywords =. doi:10.1086/323301 , archivePrefix =. astro-ph/0107201 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/323301

  25. [25]

    The Thirteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey MApping Nearby Galaxies at Apache Point Observatory

    The 13th Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey Mapping Nearby Galaxies at Apache Point Observatory. , keywords =. doi:10.3847/1538-4365/aa8992 , archivePrefix =. 1608.02013 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aa8992

  26. [26]

    HyperLEDA. III. The catalogue of extragalactic distances. , keywords =. doi:10.1051/0004-6361/201423496 , archivePrefix =. 1408.3476 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423496

  27. [27]

    , archivePrefix = "arXiv", eprint =

    Frequency and properties of bars in cluster and field galaxies at intermediate redshifts. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/200810352 , adsurl =

    work page doi:10.1051/0004-6361/200810352

  28. [28]

    Theoretical Challenges in Galaxy Formation

    Theoretical Challenges in Galaxy Formation. , keywords =. doi:10.1146/annurev-astro-081913-040019 , archivePrefix =. 1612.06891 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081913-040019

  29. [29]

    Edge-on disk galaxies in the SDSS DR6: Fractions of bulgeless and other disk galaxies

    Edge-on disk galaxies in the SDSS DR6: Fractions of bulgeless and other disk galaxies. Astronomische Nachrichten , keywords =. doi:10.1002/asna.200811132 , archivePrefix =. 0901.1894 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/asna.200811132

  30. [30]

    How Do Disks Survive Mergers?

    How do Disks Survive Mergers?. , keywords =. doi:10.1088/0004-637X/691/2/1168 , archivePrefix =. 0806.1739 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/691/2/1168

  31. [31]

    Annales d'Astrophysique , year = 1948, month = jan, volume =

    Recherches sur les Nebuleuses Extragalactiques. Annales d'Astrophysique , year = 1948, month = jan, volume =

    work page 1948

  32. [32]

    , keywords =

    Evolutionary pathways of disk galaxies with different sizes. , keywords =. doi:10.1051/0004-6361/202450397 , archivePrefix =. 2404.10432 , primaryClass =

    work page doi:10.1051/0004-6361/202450397

  33. [33]

    Bulgeless Giant Galaxies Challenge our Picture of Galaxy Formation by Hierarchical Clustering

    Bulgeless Giant Galaxies Challenge Our Picture of Galaxy Formation by Hierarchical Clustering. , keywords =. doi:10.1088/0004-637X/723/1/54 , archivePrefix =. 1009.3015 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/723/1/54

  34. [34]

    Our Milky Way as a Pure-Disk Galaxy -- A Challenge for Galaxy Formation

    Our Milky Way as a Pure-disk Galaxy A Challenge for Galaxy Formation. , keywords =. doi:10.1088/2041-8205/720/1/L72 , archivePrefix =. 1005.0385 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/720/1/l72 2041

  35. [35]

    Luminosity distribution in galaxies. II. A study of accidental and systematic errors with application to NGC 3379. , keywords =. doi:10.1086/190879 , adsurl =

    work page doi:10.1086/190879

  36. [36]

    A concise reference to (projected) Sersic R^{1/n} quantities, including Concentration, Profile Slopes, Petrosian indices, and Kron Magnitudes

    A Concise Reference to (Projected) S \'e rsic R ^ 1/n Quantities, Including Concentration, Profile Slopes, Petrosian Indices, and Kron Magnitudes. , keywords =. 2005b , month = jan, volume =. doi:10.1071/AS05001 , archivePrefix =. astro-ph/0503176 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1071/as05001

  37. [37]

    On The Robustness of z=0-1 Galaxy Size Measurements Through Model and Non-Parametric Fits

    On the Robustness of z = 0-1 Galaxy Size Measurements through Model and Non-parametric Fits. , keywords =. doi:10.1088/0004-637X/777/2/117 , archivePrefix =. 1302.6240 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/777/2/117

  38. [38]

    The ATLAS$^{\rm{3D}}$ project - XXV: Two-dimensional kinematic analysis of simulated galaxies and the cosmological origin of fast and slow rotators

    The ATLAS ^ 3D project - XXV. Two-dimensional kinematic analysis of simulated galaxies and the cosmological origin of fast and slow rotators. , keywords =. doi:10.1093/mnras/stt1919 , archivePrefix =. 1311.0284 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1919

  39. [39]

    3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since $z=3$

    3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since z = 3. , keywords =. doi:10.1088/0004-637X/788/1/28 , archivePrefix =. 1404.2844 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/788/1/28

  40. [40]

    Readdressing galaxy growth using a physically motivated size indicator

    Strong size evolution of disc galaxies since z = 1. Readdressing galaxy growth using a physically motivated size indicator. , keywords =. doi:10.1051/0004-6361/202346133 , archivePrefix =. 2311.07656 , primaryClass =

    work page doi:10.1051/0004-6361/202346133

  41. [41]

    The Sloan Digital Sky Survey: Technical Summary

    The Sloan Digital Sky Survey: Technical Summary. , keywords =. doi:10.1086/301513 , archivePrefix =. astro-ph/0006396 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301513

  42. [42]

    , keywords =

    A physically motivated definition for the size of galaxies in an era of ultradeep imaging. , keywords =. doi:10.1093/mnras/staa236 , archivePrefix =. 2001.02689 , primaryClass =

    work page doi:10.1093/mnras/staa236 2001

  43. [43]

    First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback

    First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback. , keywords =. doi:10.1093/mnras/stz2306 , archivePrefix =. 1902.05554 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz2306 1902

  44. [44]

    Monthly Notices of the Royal Astronomical Society , volume =

    Pillepich, Annalisa and Nelson, Dylan and Springel, Volker and Pakmor, Rüdiger and Torrey, Paul and Weinberger, Rainer and Vogelsberger, Mark and Marinacci, Federico and Genel, Shy and van der Wel, Arjen and Hernquist, Lars , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2019 , month =. doi:10.1093/mnras/stz2338 , url =

    work page doi:10.1093/mnras/stz2338 2019

  45. [45]

    Sparse Image and Signal Processing : Wavelets, Curvelets, Morphological Diversity , isbn =

    Starck, Jean-Luc and Murtagh, Fionn and Fadili, Mohamed-Jalal , year =. Sparse Image and Signal Processing : Wavelets, Curvelets, Morphological Diversity , isbn =. Sparse Image and Signal Processing: Wavelets, Curvelets, Morphological Diversity , doi =

    work page

  46. [46]

    Carrillo, R. E. and McEwen, J. D. and Wiaux, Y. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2012 , month =. doi:10.1111/j.1365-2966.2012.21605.x , url =

    work page doi:10.1111/j.1365-2966.2012.21605.x 2012

  47. [47]

    Minor mergers and the size evolution of elliptical galaxies

    Minor Mergers and the Size Evolution of Elliptical Galaxies. , keywords =. doi:10.1088/0004-637X/699/2/L178 , archivePrefix =. 0903.1636 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/699/2/l178

  48. [48]

    , keywords =

    Image restoration with noise suppression using the wavelet transform. , keywords =

    work page

  49. [49]

    , keywords =

    The Sloan Digital Sky Survey extended point spread functions. , keywords =. doi:10.1093/mnras/stz3111 , archivePrefix =. 1911.01430 , primaryClass =

    work page doi:10.1093/mnras/stz3111 1911

  50. [50]

    Sedighi, Nafise and Sharbaf, Zahra and Trujillo, Ignacio and Eskandarlou, Sepideh and Golini, Giulia and Infante-Sainz, Ra. LIGHTS. The Open Journal of Astrophysics , doi =. 2025 , month =

    work page 2025

  51. [51]

    The Fornax Deep Survey with VST. VIII. Connecting the accretion history with the cluster density. , keywords =. doi:10.1051/0004-6361/202038015 , archivePrefix =. 2005.00025 , primaryClass =

    work page doi:10.1051/0004-6361/202038015 2005

  52. [52]

    IC 1101 and the Galaxies of Tomorrow: Toward an Observational Detection of the Splashback Radius , note =

    work page

  53. [53]

    10.1051/0004-6361/202555288

    LIGHTS - A robust technique to identify galaxy edges , DOI= "10.1051/0004-6361/202555288", url= "https://doi.org/10.1051/0004-6361/202555288", journal =

    work page doi:10.1051/0004-6361/202555288

  54. [54]

    10.1051/0004-6361/202557194

    Bulgeless Evolution And the Rise of Discs (BEARD) - III. A numerical simulation view of satellites around Milky-Way analogues , DOI= "10.1051/0004-6361/202557194", url= "https://doi.org/10.1051/0004-6361/202557194", journal =

    work page doi:10.1051/0004-6361/202557194

  55. [55]

    10.1051/0004-6361/202556875

    Bulgeless Evolution And the Rise of Discs (BEARD) - II. The role of mergers in shaping the Milky Way analogues in TNG50 , DOI= "10.1051/0004-6361/202556875", url= "https://doi.org/10.1051/0004-6361/202556875", journal =

    work page doi:10.1051/0004-6361/202556875

  56. [56]

    A universal angular momentum profile for galactic halos

    A Universal Angular Momentum Profile for Galactic Halos. , keywords =. doi:10.1086/321477 , archivePrefix =. astro-ph/0011001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/321477

  57. [57]

    Removing Internal Reflections from Deep Imaging Datasets

    Removing Internal Reflections from Deep Imaging Data Sets. , keywords =. doi:10.1086/648457 , archivePrefix =. 0909.3320 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/648457

  58. [58]

    Beyond 31 mag/arcsec^2: the low surface brightness frontier with the largest optical telescopes

    Beyond 31 mag arcsec ^ -2 : The Frontier of Low Surface Brightness Imaging with the Largest Optical Telescopes. , keywords =. doi:10.3847/0004-637X/823/2/123 , archivePrefix =. 1510.04696 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/823/2/123

  59. [59]

    Noise Based Detection and Segmentation of Nebulous Objects

    Noise-based Detection and Segmentation of Nebulous Objects. , keywords =. doi:10.1088/0067-0049/220/1/1 , archivePrefix =. 1505.01664 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/220/1/1

  60. [60]

    arXiv e-prints , keywords =

    Carving out the low surface brightness universe with NoiseChisel. arXiv e-prints , keywords =. doi:10.48550/arXiv.1909.11230 , archivePrefix =. 1909.11230 , primaryClass =

    work page doi:10.48550/arxiv.1909.11230 1909

  61. [61]

    Mathematical Morphology - Theory and Applications , doi =

    Statistical attribute filtering to detect faint extended astronomical sources , author =. Mathematical Morphology - Theory and Applications , doi =. 2016 , lastchecked =

    work page 2016

  62. [62]

    Observations, reduction and results

    CCD surface photometry of elliptical galaxies - I. Observations, reduction and results. , keywords =. doi:10.1093/mnras/226.4.747 , adsurl =

    work page doi:10.1093/mnras/226.4.747

  63. [63]

    doi:10.5281/zenodo.3478575 , version =

    astropy/photutils: v0.7.1. doi:10.5281/zenodo.3478575 , version =

    work page doi:10.5281/zenodo.3478575

  64. [64]

    On the Uncertainties of Stellar Mass Estimates via Colour Measurements

    On the uncertainties of stellar mass estimates via colour measurements. , keywords =. doi:10.1093/mnras/stv1499 , archivePrefix =. 1507.03016 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1499

  65. [65]

    Color Profiles of Spiral Galaxies: Clues on Outer-Disk Formation Scenarios

    Color Profiles of Spiral Galaxies: Clues on Outer-Disk Formation Scenarios. , keywords =. doi:10.1086/591671 , archivePrefix =. 0807.2776 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591671

  66. [66]

    , keywords =

    The edges of galaxies: Tracing the limits of star formation. , keywords =. doi:10.1051/0004-6361/202243612 , archivePrefix =. 2209.05497 , primaryClass =

    work page doi:10.1051/0004-6361/202243612

  67. [67]

    The Absolute Magnitude of the Sun in Several Filters

    The Absolute Magnitude of the Sun in Several Filters. , keywords =. doi:10.3847/1538-4365/aabfdf , archivePrefix =. 1804.07788 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aabfdf

  68. [68]

    10.1051/0004-6361/202554290

    A physically motivated galaxy size definition across different state-of-the-art hydrodynamical simulations , DOI= "10.1051/0004-6361/202554290", url= "https://doi.org/10.1051/0004-6361/202554290", journal =

    work page doi:10.1051/0004-6361/202554290

  69. [69]

    , keywords =

    Structural and stellar-population properties versus bulge types in Sloan Digital Sky Survey central galaxies. , keywords =. doi:10.1093/mnras/staa328 , archivePrefix =. 1908.08055 , primaryClass =

    work page doi:10.1093/mnras/staa328 1908

  70. [70]

    The Dependence of Quenching upon the Inner Structure of Galaxies at 0.5<z< 0.8 in the DEEP2/AEGIS Survey

    The Dependence of Quenching upon the Inner Structure of Galaxies at 0.5 <= z < 0.8 in the DEEP2/AEGIS Survey. , keywords =. doi:10.1088/0004-637X/760/2/131 , archivePrefix =. 1210.4173 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/760/2/131

  71. [71]

    Dense cores in galaxies out to z=2.5 in SDSS, UltraVISTA, and the five 3D-HST/CANDELS fields

    Dense Cores in Galaxies Out to z = 2.5 in SDSS, UltraVISTA, and the Five 3D-HST/CANDELS Fields. , keywords =. doi:10.1088/0004-637X/791/1/45 , archivePrefix =. 1404.4874 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/791/1/45

  72. [72]

    Evidence for Mature Bulges and an Inside-out Quenching Phase 3 Billion Years After the Big Bang

    Evidence for mature bulges and an inside-out quenching phase 3 billion years after the Big Bang. Science , keywords =. doi:10.1126/science.1261094 , archivePrefix =. 1504.04021 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1261094

  73. [73]

    The intrinsic characteristics of galaxies on the SFR-stellar mass plane at 1.2<z<4: I. the correlation between stellar age, central density and position relative to the main sequence

    The Intrinsic Characteristics of Galaxies on the SFR-M _ * Plane at 1.2 < z < 4: I. The Correlation between Stellar Age, Central Density, and Position Relative to the Main Sequence. , keywords =. doi:10.3847/1538-4357/aaa40f , archivePrefix =. 1706.02311 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaa40f

  74. [74]

    , keywords =

    Evolution of central galaxy alignments in simulations. , keywords =. doi:10.1051/0004-6361/202450597 , archivePrefix =. 2405.02398 , primaryClass =

    work page doi:10.1051/0004-6361/202450597

  75. [75]

    Strong bimodality in the host halo mass of central galaxies from galaxy-galaxy lensing

    Strong bimodality in the host halo mass of central galaxies from galaxy-galaxy lensing. , keywords =. doi:10.1093/mnras/stw188 , archivePrefix =. 1509.06762 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw188

  76. [76]

    MNRAS , archivePrefix = "arXiv", eprint =

    Satellite abundances around bright isolated galaxies. , keywords =. doi:10.1111/j.1365-2966.2012.21256.x , archivePrefix =. 1203.0009 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21256.x 2012

  77. [77]

    , keywords =

    Galaxy disc scaling relations: A tight linear galaxy-halo connection challenges abundance matching. , keywords =. doi:10.1051/0004-6361/201935982 , archivePrefix =. 1909.01344 , primaryClass =

    work page doi:10.1051/0004-6361/201935982 1909

  78. [78]

    Monthly Notices of the Royal Astronomical Society , volume =

    Proctor, Katy L and Ludlow, Aaron D and Lagos, Claudia del P and Robotham, Aaron S G , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2025 , month =. doi:10.1093/mnras/staf1339 , url =

    work page doi:10.1093/mnras/staf1339 2025

  79. [79]

    Galactic Angular Momentum in the Illustris Simulation: Feedback and the Hubble Sequence

    Galactic Angular Momentum in the Illustris Simulation: Feedback and the Hubble Sequence. , keywords =. doi:10.1088/2041-8205/804/2/L40 , archivePrefix =. 1503.01117 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/804/2/l40 2041

  80. [80]

    Morphological quenching of star formation: making early-type galaxies red

    Morphological Quenching of Star Formation: Making Early-Type Galaxies Red. , keywords =. doi:10.1088/0004-637X/707/1/250 , archivePrefix =. 0905.4669 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/707/1/250

Showing first 80 references.