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arxiv: 2604.03503 · v1 · submitted 2026-04-03 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

The morphologies of present-day galaxies in the COLIBRE simulations

Victor J. Forouhar Moreno , Joop Schaye , Matthieu Schaller , Aaron Ludlow , Robert J. McGibbon , Alejandro Ben\'itez-Llambay , Evgenii Chaikin , Carlos S. Frenk
show 4 more authors
Filip Hu\v{s}ko Sylvia Ploeckinger Alexander J. Richings James W. Trayford
Authors on Pith no claims yet

Pith reviewed 2026-05-13 17:47 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy morphologykinematic morphologycosmological simulationsstellar massgalaxy formationdisk galaxiesrotation supporthalo properties
0
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The pith

COLIBRE simulations find that galaxy rotational support peaks at stellar masses of 1-2 times 10^10 solar masses and links more strongly to internal properties than to host halos.

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

The COLIBRE simulations improve modeling of the interstellar medium and stellar-dark matter interactions to overcome prior limitations in cosmological runs. They quantify present-day galaxy shapes with four metrics, three based on kinematics and one on spatial structure, and show these shapes converge across resolution levels. Kinematic morphology tracks stellar mass and color closely, with the strongest rotational dominance appearing at intermediate masses. At fixed mass, central galaxy shapes show only weak ties to halo properties but stronger connections to gas richness, star formation rate, stellar age, and size.

Core claim

COLIBRE predicts that kinematic morphology correlates strongly with stellar mass and colour, and that galaxies with stellar masses of ≈(1-2)×10^{10} M_⊙ tend to be the most rotationally-dominated. At fixed stellar mass, the morphology of central galaxies correlates weakly with the properties of their host halo. Morphology correlates more strongly with internal galaxy properties, with more disky galaxies being more gas-rich, having higher star formation rates and exhibiting younger and more extended stellar populations. Other properties, like the mass of the most massive black hole, the fraction of stars that are accreted and stellar metallicity, also correlate with morphology, but with the 0

What carries the argument

Four strongly correlated morphology metrics—three kinematic measures of rotational support versus random motions and one spatial shape indicator—applied to galaxies in the COLIBRE runs that resolve interstellar medium pressure and reduce spurious stellar-dark matter scattering.

If this is right

  • Galaxies near 1-2×10^{10} solar masses reach the highest fraction of ordered rotation.
  • Disk-dominated systems are systematically gas-richer, form stars faster, and host younger stellar populations.
  • Central galaxies show only weak morphology links to halo mass or concentration once stellar mass is fixed.
  • Black-hole mass, accreted-star fraction, and metallicity track morphology, but the strength of those links varies with galaxy mass and central versus satellite status.

Where Pith is reading between the lines

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

  • Internal feedback and gas processes appear to set galaxy shape more than the external merger or accretion history encoded in the halo.
  • Rotation-curve surveys targeting the 10^{10} solar-mass range could directly test the predicted peak in disk dominance.
  • The resolution convergence reported here suggests that similar morphology trends should appear in future higher-resolution runs or in semi-analytic models tuned to the same internal physics.
  • Extending the same metrics to earlier cosmic times could show when the mass-dependent morphology trends first appear.

Load-bearing premise

The new interstellar medium and stellar-dark matter interaction treatments in COLIBRE are assumed to remove the main prior biases so that the reported mass and internal-property correlations reflect actual galaxy formation.

What would settle it

Large observational samples showing no peak in rotational support near 1-2×10^{10} solar masses or a strong morphology-halo correlation at fixed stellar mass would falsify the central predictions.

Figures

Figures reproduced from arXiv: 2604.03503 by Aaron Ludlow, Alejandro Ben\'itez-Llambay, Alexander J. Richings, Carlos S. Frenk, Evgenii Chaikin, Filip Hu\v{s}ko, James W. Trayford, Joop Schaye, Matthieu Schaller, Robert J. McGibbon, Sylvia Ploeckinger, Victor J. Forouhar Moreno.

Figure 2
Figure 2. Figure 2: The effect of varying the aperture size on kinematic morphology metrics as a function of stellar mass. The lines show the median shift of a given morphology metric relative to our fiducial aperture of 3𝑅1/2, and the shaded regions indicate the 16th to 84th percentiles of the distributions. We only use central galaxies from the L200m6 simulation. Using an aperture that is too small underestimates the kinema… view at source ↗
Figure 1
Figure 1. Figure 1: Distribution of axis ratios for L200m6 central galaxies with 𝑀∗ ≥ 109 M⊙. The dotted lines delineate regions of approximately simi￾lar morphological types (van der Wel et al. 2014b), as indicated in the top right panel. The panels in the left column use the iterative method to mea￾sure the inertia tensor, whereas those on the right employ the non-iterative approach. The initial aperture used to select stel… view at source ↗
Figure 3
Figure 3. Figure 3: Misalignment between the mass- and luminosity-weighted stellar angular momentum within 3𝑅1/2 as a function of stellar mass. The median misalignment when using the u and K GAMA photometric bands are shown using the dotted and solid lines, respectively. The shaded regions indicate the 16th to 84th percentiles of the distributions. Galaxies are split into spheroid- (top panel) and disc-dominated (bottom panel… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of mass- and luminosity-weighted morphology met￾rics measured within 3𝑅1/2. The lines indicate the median shift of a given morphology metric relative to its mass-weighted definition at a fixed stellar mass, when using the u (dotted) and K (solid) GAMA photometric bands. The shaded regions indicate the 16th to 84th percentiles of the distributions. We only use central galaxies from the L200m6 sim… view at source ↗
Figure 5
Figure 5. Figure 5: HST-like images of representative galaxies from the L025m5, L200m6 and L400m7 simulations, which are used for different stellar mass ranges, as indicated at the top of the figure. The images use all particles in the region regardless of whether they are bound or not to the galaxy of interest, meaning that nearby companion galaxies may also be imaged. Since we compute morphology metrics using only bound ste… view at source ↗
Figure 7
Figure 7. Figure 7: Convergence of the median values of four morphology indicators with the numerical resolution of the simulation. The tests are done using all galaxies from the largest available volume (253 Mpc3 ) at 𝑧 = 0 common to the m5, m6 and m7 models. The dotted lines at the high mass end indicate stellar mass bins that contain fewer than 10 galaxies. The stellar mass bins in which galaxies are poorly sampled (≲ 50 p… view at source ↗
Figure 9
Figure 9. Figure 9: Correlations between four different indicators of morphology for all galaxies with 𝑀∗ ≥ 5.4 × 107 M⊙ in the L200m6 simulation (at least 50 stellar particles). The intensity of the map reflects the logarithm of the number of galaxies in a given pixel. The different contours enclose 50 per cent of the galaxy population within the three stellar mass bins indicated in the legend, which clearly differ in their … view at source ↗
Figure 10
Figure 10. Figure 10: shows the median value of the four morphology metrics as a function of galaxy stellar mass. We show the trend with stellar mass for the whole galaxy population (solid), and for galaxies that are centrals (dashed) or satellites (dotted). To sample the distribution over a wide range of stellar mass, we use each of the three different resolution simulations for a distinct range in stellar mass.We motivate co… view at source ↗
Figure 11
Figure 11. Figure 11: Top panel: Distribution of galaxies in the space of intrinsic (u-r) colour and stellar mass, and the correlation with the spheroid-to-total mass ratio. We combine central and satellite galaxies of the L025m5, L200m6 and L400m7 simulations in the same manner as in [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Spearman rank correlation coefficients for the relations between the morphology of central galaxies and their host halo properties. The proper￾ties of the halo in the first five panels are measured using all particles enclosed by its virial radius (𝑅200c). We show the correlations with halo properties measured in the hydrodynamical (solid) and DMO (dashed) versions of the simulation. The shaded region ind… view at source ↗
Figure 13
Figure 13. Figure 13: Spearman rank correlation coefficient for the relations between galaxy morphology and various internal properties. The galaxy properties are measured using bound particles within 50 kpc. We show the correlation strength of the central (solid line) and satellite (dashed line) galaxy populations separately. The correlation strengths between morphology and internal galaxy properties are generally strong, mas… view at source ↗
read the original abstract

The diversity of galaxy morphologies and their relations with galaxy and halo properties is fundamental to understanding galaxy formation. Cosmological simulations of representative volumes can help disentangle the origin of observed correlations, but most suffer from two main limitations that affect morphologies: an over-pressurised interstellar medium and spurious interactions between stellar and dark matter particles. We present an overview of galaxy morphologies in the COLIBRE simulations, which address these limitations and reproduce many observed galaxy scaling relations. To quantify galaxy morphology, we use four (strongly-correlated) theory-space metrics, three kinematic and one spatial. We explore how different choices and limitations affect these indicators, including luminosity- versus mass-weighting, aperture size and shot noise. Overall, we find good convergence in present-day morphologies across two orders of magnitude in mass resolution. COLIBRE predicts that kinematic morphology correlates strongly with stellar mass and colour, and that galaxies with stellar masses of $\approx(1-2)\times 10^{10}\,\mathrm{M}_{\odot}$ tend to be the most rotationally-dominated. At fixed stellar mass, the morphology of central galaxies correlates weakly with the properties of their host halo. Morphology correlates more strongly with internal galaxy properties, with more disky galaxies being more gas-rich, having higher star formation rates and exhibiting younger and more extended stellar populations. Other properties, like the mass of the most massive black hole, the fraction of stars that are accreted and stellar metallicity, also correlate with morphology, but with correlation strengths sensitive to the stellar mass of the galaxy and whether it is a central or satellite.

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.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract supplies no enumerated free parameters, axioms, or invented entities; the work rests on standard cosmological initial conditions and unspecified subgrid physics models for gas and feedback.

pith-pipeline@v0.9.0 · 5645 in / 1196 out tokens · 78131 ms · 2026-05-13T17:47:17.605725+00:00 · methodology

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Reference graph

Works this paper leans on

153 extracted references · 153 canonical work pages · 4 internal anchors

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

    work page

  2. [2]

    G., Navarro J

    Abadi M. G., Navarro J. F., Steinmetz M., Eke V. R., 2003, @doi [ ] 10.1086/378316 , https://ui.adsabs.harvard.edu/abs/2003ApJ...597...21A 597, 21

    work page doi:10.1086/378316 2003

  3. [3]

    Abbott T. M. C., et al., 2022, @doi [ ] 10.1103/PhysRevD.105.023520 , https://ui.adsabs.harvard.edu/abs/2022PhRvD.105b3520A 105, 023520

    work page doi:10.1103/physrevd.105.023520 2022

  4. [4]

    G., Navarro J

    Algorry D. G., Navarro J. F., Abadi M. G., Sales L. V., Steinmetz M., Piontek F., 2014, @doi [ ] 10.1093/mnras/stt2154 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.437.3596A 437, 3596

    work page doi:10.1093/mnras/stt2154 2014

  5. [5]

    K., Glazebrook K., Brinkmann J., Ivezi \'c Z ., Lupton R

    Baldry I. K., Glazebrook K., Brinkmann J., Ivezi \'c Z ., Lupton R. H., Nichol R. C., Szalay A. S., 2004, @doi [ ] 10.1086/380092 , https://ui.adsabs.harvard.edu/abs/2004ApJ...600..681B 600, 681

    work page doi:10.1086/380092 2004

  6. [6]

    F., et al., 2012, @doi [ ] 10.1088/0004-637X/753/2/167 , http://adsabs.harvard.edu/abs/2012ApJ...753..167B 753, 167

    Bell E. F., et al., 2012, @doi [ ] 10.1088/0004-637X/753/2/167 , https://ui.adsabs.harvard.edu/abs/2012ApJ...753..167B 753, 167

    work page doi:10.1088/0004-637x/753/2/167 2012

  7. [7]

    The abundance of thin dwarf galaxies: a challenge for cosmological simulations

    Benavides J. A., Sales L. V., Navarro J. F., White S. D. M., Frenk C. S., Oman K. A., Cole S., 2025a, @doi [arXiv e-prints] 10.48550/arXiv.2512.11035 , https://ui.adsabs.harvard.edu/abs/2025arXiv251211035B p. arXiv:2512.11035

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2512.11035

  8. [8]

    A., et al., 2025b, @doi [ ] 10.1093/mnras/staf1847 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544.4651B 544, 4651

    Benavides J. A., et al., 2025b, @doi [ ] 10.1093/mnras/staf1847 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544.4651B 544, 4651

    work page doi:10.1093/mnras/staf1847

  9. [9]

    F., Frenk C

    Ben \' tez-Llambay A., Navarro J. F., Frenk C. S., Ludlow A. D., 2018, @doi [ ] 10.1093/mnras/stx2420 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.1019B 473, 1019

    work page doi:10.1093/mnras/stx2420 2018

  10. [10]

    Ben \' tez-Llambay A., et al., 2026, @doi [ ] 10.1093/mnras/stag268 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.546ag268B 546, stag268

    work page doi:10.1093/mnras/stag268 2026

  11. [11]

    Bevacqua D., Cappellari M., Pellegrini S., 2022, @doi [ ] 10.1093/mnras/stab3732 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511..139B 511, 139

    work page doi:10.1093/mnras/stab3732 2022

  12. [12]

    A., Pedrosa S

    Bignone L. A., Pedrosa S. E., Trayford J. W., Tissera P. B., Pellizza L. J., 2020, @doi [ ] 10.1093/mnras/stz3014 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.3624B 491, 3624

    work page doi:10.1093/mnras/stz3014 2020

  13. [13]

    Binney J., 1978, @doi [ ] 10.1093/mnras/183.3.501 , https://ui.adsabs.harvard.edu/abs/1978MNRAS.183..501B 183, 501

    work page doi:10.1093/mnras/183.3.501 1978

  14. [14]

    Binney J., Tremaine S., 2008, Galactic Dynamics: Second Edition

    work page 2008

  15. [15]

    Bizyaev D., Mitronova S., 2009, @doi [ ] 10.1088/0004-637X/702/2/1567 , https://ui.adsabs.harvard.edu/abs/2009ApJ...702.1567B 702, 1567

    work page doi:10.1088/0004-637x/702/2/1567 2009

  16. [16]

    R., et al., 2003, @doi [ ] 10.1086/375528 , https://ui.adsabs.harvard.edu/abs/2003ApJ...594..186B 594, 186

    Blanton M. R., et al., 2003, @doi [ ] 10.1086/375528 , https://ui.adsabs.harvard.edu/abs/2003ApJ...594..186B 594, 186

    work page doi:10.1086/375528 2003

  17. [17]

    Bonamigo M., Despali G., Limousin M., Angulo R., Giocoli C., Soucail G., 2015, @doi [ ] 10.1093/mnras/stv417 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.449.3171B 449, 3171

    work page doi:10.1093/mnras/stv417 2015

  18. [18]

    F., Capozziello, S., & Dainotti, M

    Booth C. M., Schaye J., 2009, @doi [ ] 10.1111/j.1365-2966.2009.15043.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.398...53B 398, 53

    work page doi:10.1111/j.1365-2966.2009.15043.x 2009

  19. [19]

    doi:10.1093/mnras/stab3166 , archiveprefix =

    Borrow J., Schaller M., Bower R. G., Schaye J., 2022, @doi [ ] 10.1093/mnras/stab3166 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511.2367B 511, 2367

    work page doi:10.1093/mnras/stab3166 2022

  20. [20]

    L., 2017, @doi [ ] 10.1093/mnras/stx276 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.467.2879B 467, 2879

    Bottrell C., Torrey P., Simard L., Ellison S. L., 2017, @doi [ ] 10.1093/mnras/stx276 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.467.2879B 467, 2879

    work page doi:10.1093/mnras/stx276 2017

  21. [21]

    Bruzual G., Charlot S., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06897.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.344.1000B 344, 1000

    work page doi:10.1046/j.1365-8711.2003.06897.x 2003

  22. [22]

    E., Kay S

    Bryan S. E., Kay S. T., Duffy A. R., Schaye J., Dalla Vecchia C., Booth C. M., 2013, @doi [ ] 10.1093/mnras/sts587 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.429.3316B 429, 3316

    work page doi:10.1093/mnras/sts587 2013

  23. [23]

    S., Dekel A., Kolatt T

    Bullock J. S., Dekel A., Kolatt T. S., Kravtsov A. V., Klypin A. A., Porciani C., Primack J. R., 2001, @doi [ ] 10.1086/321477 , https://ui.adsabs.harvard.edu/abs/2001ApJ...555..240B 555, 240

    work page doi:10.1086/321477 2001

  24. [24]

    Bundy K., et al., 2010, @doi [ ] 10.1088/0004-637X/719/2/1969 , https://ui.adsabs.harvard.edu/abs/2010ApJ...719.1969B 719, 1969

    work page doi:10.1088/0004-637x/719/2/1969 2010

  25. [25]

    Cappellari M., 2008, @doi [ ] 10.1111/j.1365-2966.2008.13754.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.390...71C 390, 71

    work page doi:10.1111/j.1365-2966.2008.13754.x 2008

  26. [26]

    M., Navarro J

    Celiz B. M., Navarro J. F., Abadi M. G., Springel V., 2025, @doi [ ] 10.1051/0004-6361/202554847 , https://ui.adsabs.harvard.edu/abs/2025A&A...699A..12C 699, A12

    work page doi:10.1051/0004-6361/202554847 2025

  27. [27]

    Chaikin E., Schaye J., Schaller M., Ben \' tez-Llambay A., Nobels F. S. J., Ploeckinger S., 2023, @doi [ ] 10.1093/mnras/stad1626 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3709C 523, 3709

    work page doi:10.1093/mnras/stad1626 2023

  28. [28]

    COLIBRE: calibrating subgrid feedback in cosmological simulations that include a cold gas phase

    Chaikin E., et al., 2025a, @doi [arXiv e-prints] 10.48550/arXiv.2509.04067 , https://ui.adsabs.harvard.edu/abs/2025arXiv250904067C p. arXiv:2509.04067

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.04067

  29. [29]

    The evolution of the galaxy stellar mass function and star formation rates in the COLIBRE simulations from redshift 17 to 0

    Chaikin E., et al., 2025b, @doi [arXiv e-prints] 10.48550/arXiv.2509.07960 , https://ui.adsabs.harvard.edu/abs/2025arXiv250907960C p. arXiv:2509.07960

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.07960

  30. [30]

    Chandro-G \'o mez \'A ., et al., 2025, @doi [ ] 10.1093/mnras/staf519 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.539..776C 539, 776

    work page doi:10.1093/mnras/staf519 2025

  31. [31]

    Chua K. T. E., Pillepich A., Rodriguez-Gomez V., Vogelsberger M., Bird S., Hernquist L., 2017, @doi [ ] 10.1093/mnras/stx2238 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.472.4343C 472, 4343

    work page doi:10.1093/mnras/stx2238 2017

  32. [32]

    Chua K. T. E., Pillepich A., Vogelsberger M., Hernquist L., 2019, @doi [ ] 10.1093/mnras/sty3531 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484..476C 484, 476

    work page doi:10.1093/mnras/sty3531 2019

  33. [33]

    G., 2018, @doi [ ] 10.1093/mnras/sty1229 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.3994C 478, 3994

    Clauwens B., Schaye J., Franx M., Bower R. G., 2018, @doi [ ] 10.1093/mnras/sty1229 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.3994C 478, 3994

    work page doi:10.1093/mnras/sty1229 2018

  34. [34]

    A., Schaye J., Clauwens B., Bower R

    Correa C. A., Schaye J., Clauwens B., Bower R. G., Crain R. A., Schaller M., Theuns T., Thob A. C. R., 2017, @doi [ ] 10.1093/mnrasl/slx133 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.472L..45C 472, L45

    work page doi:10.1093/mnrasl/slx133 2017

  35. [35]

    A., Schaye J., Trayford J

    Correa C. A., Schaye J., Trayford J. W., 2019, @doi [ ] 10.1093/mnras/stz295 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.4401C 484, 4401

    work page doi:10.1093/mnras/stz295 2019

  36. [36]

    A., et al., 2026, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2026arXiv260400980C p

    Correa C. A., et al., 2026, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2026arXiv260400980C p. arXiv:2604.00980

    work page arXiv 2026

  37. [37]

    A., van de Voort F., 2023, @doi [ ] 10.1146/annurev-astro-041923-043618 , https://ui.adsabs.harvard.edu/abs/2023ARA&A..61..473C 61, 473

    Crain R. A., van de Voort F., 2023, @doi [ ] 10.1146/annurev-astro-041923-043618 , https://ui.adsabs.harvard.edu/abs/2023ARA&A..61..473C 61, 473

    work page doi:10.1146/annurev-astro-041923-043618 2023

  38. [38]

    A., Schaye, J., Bower, R

    Crain R. A., et al., 2015, @doi [ ] 10.1093/mnras/stv725 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.450.1937C 450, 1937

    work page doi:10.1093/mnras/stv725 2015

  39. [39]

    Cui J., Gu Q., Shi Y., 2024, @doi [ ] 10.1093/mnras/stae156 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.528.2391C 528, 2391

    work page doi:10.1093/mnras/stae156 2024

  40. [40]

    Dekel A., Ginzburg O., Jiang F., Freundlich J., Lapiner S., Ceverino D., Primack J., 2020, @doi [ ] 10.1093/mnras/staa470 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.4126D 493, 4126

    work page doi:10.1093/mnras/staa470 2020

  41. [41]

    Dickinson H., et al., 2018, @doi [ ] 10.3847/1538-4357/aaa250 , https://ui.adsabs.harvard.edu/abs/2018ApJ...853..194D 853, 194

    work page doi:10.3847/1538-4357/aaa250 2018

  42. [42]

    G., 1970, Astrofizika, https://ui.adsabs.harvard.edu/abs/1970Afz.....6..581D 6, 581

    Doroshkevich A. G., 1970, Astrofizika, https://ui.adsabs.harvard.edu/abs/1970Afz.....6..581D 6, 581

    work page 1970

  43. [43]

    Dressler A., 1980, @doi [ ] 10.1086/157753 , https://ui.adsabs.harvard.edu/abs/1980ApJ...236..351D 236, 351

    work page doi:10.1086/157753 1980

  44. [44]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Driver S. P., et al., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10126.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.368..414D 368, 414

    work page doi:10.1111/j.1365-2966.2006.10126.x 2006

  45. [45]

    P., Norberg, P., Baldry, I

    Driver S. P., et al., 2009, @doi [Astronomy and Geophysics] 10.1111/j.1468-4004.2009.50512.x , https://ui.adsabs.harvard.edu/abs/2009A&G....50e..12D 50, 5.12

    work page doi:10.1111/j.1468-4004.2009.50512.x 2009

  46. [46]

    , keywords =

    Driver S. P., et al., 2022, @doi [ ] 10.1093/mnras/stac472 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.513..439D 513, 439

    work page doi:10.1093/mnras/stac472 2022

  47. [47]

    G., 1991, @doi [ ] 10.1086/170451 , https://ui.adsabs.harvard.edu/abs/1991ApJ...378..496D 378, 496

    Dubinski J., Carlberg R. G., 1991, @doi [ ] 10.1086/170451 , https://ui.adsabs.harvard.edu/abs/1991ApJ...378..496D 378, 496

    work page doi:10.1086/170451 1991

  48. [48]

    Dubois Y., Gavazzi R., Peirani S., Silk J., 2013, @doi [ ] 10.1093/mnras/stt997 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.433.3297D 433, 3297

    work page doi:10.1093/mnras/stt997 2013

  49. [49]

    Dubois Y., et al., 2021, @doi [ ] 10.1051/0004-6361/202039429 , https://ui.adsabs.harvard.edu/abs/2021A&A...651A.109D 651, A109

    work page doi:10.1051/0004-6361/202039429 2021

  50. [50]

    L., Eli \'a s ek J., 2021, @doi [ ] 10.1051/0004-6361/202039562 , https://ui.adsabs.harvard.edu/abs/2021A&A...647A.103E 647, A103

    Ebrov \'a I., okas E. L., Eli \'a s ek J., 2021, @doi [ ] 10.1051/0004-6361/202039562 , https://ui.adsabs.harvard.edu/abs/2021A&A...647A.103E 647, A103

    work page doi:10.1051/0004-6361/202039562 2021

  51. [51]

    F., Kere s D., Chan T

    El-Badry K., Wetzel A., Geha M., Hopkins P. F., Kere s D., Chan T. K., Faucher-Gigu \`e re C.-A., 2016, @doi [ ] 10.3847/0004-637X/820/2/131 , https://ui.adsabs.harvard.edu/abs/2016ApJ...820..131E 820, 131

    work page doi:10.3847/0004-637x/820/2/131 2016

  52. [52]

    El-Badry K., et al., 2018, @doi [ ] 10.1093/mnras/stx2482 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.1930E 473, 1930

    work page doi:10.1093/mnras/stx2482 2018

  53. [53]

    arXiv:2511.02964

    Euclid Collaboration et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2511.02964 , https://ui.adsabs.harvard.edu/abs/2025arXiv251102964E p. arXiv:2511.02964

    work page doi:10.48550/arxiv.2511.02964 2025

  54. [54]

    Fakhouri O., Ma C.-P., 2009, @doi [ ] 10.1111/j.1365-2966.2009.14480.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.394.1825F 394, 1825

    work page doi:10.1111/j.1365-2966.2009.14480.x 2009

  55. [55]

    Faltenbacher A., White S. D. M., 2010, @doi [ ] 10.1088/0004-637X/708/1/469 , https://ui.adsabs.harvard.edu/abs/2010ApJ...708..469F 708, 469

    work page doi:10.1088/0004-637x/708/1/469 2010

  56. [56]

    Feldmann R., et al., 2023, @doi [ ] 10.1093/mnras/stad1205 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.3831F 522, 3831

    work page doi:10.1093/mnras/stad1205 2023

  57. [57]

    J., Ben \' tez-Llambay A., Cole S., Frenk C., 2022, @doi [ ] 10.1093/mnras/stac3062 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5627F 517, 5627

    Forouhar Moreno V. J., Ben \' tez-Llambay A., Cole S., Frenk C., 2022, @doi [ ] 10.1093/mnras/stac3062 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5627F 517, 5627

    work page doi:10.1093/mnras/stac3062 2022

  58. [58]

    J., Helly J., McGibbon R., Schaye J., Schaller M., Han J., Kugel R., Bah \'e Y

    Forouhar Moreno V. J., Helly J., McGibbon R., Schaye J., Schaller M., Han J., Kugel R., Bah \'e Y. M., 2025, @doi [ ] 10.1093/mnras/staf1478 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.543.1339F 543, 1339

    work page doi:10.1093/mnras/staf1478 2025

  59. [59]

    Frontiere N., Emberson J. D., Buehlmann M., Habib S., Heitmann K., Ramachandra N., Faucher-Gigu \`e re C.-A., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2511.21921 , https://ui.adsabs.harvard.edu/abs/2025arXiv251121921F p. arXiv:2511.21921

    work page doi:10.48550/arxiv.2511.21921 2025

  60. [60]

    Genel S., et al., 2014, @doi [ ] 10.1093/mnras/stu1654 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445..175G 445, 175

    work page doi:10.1093/mnras/stu1654 2014

  61. [61]

    W., Sahu N., 2023, @doi [ ] 10.1093/mnras/stac2019 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2177G 518, 2177

    Graham A. W., Sahu N., 2023, @doi [ ] 10.1093/mnras/stac2019 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2177G 518, 2177

    work page doi:10.1093/mnras/stac2019 2023

  62. [62]

    Hahn O., Rampf C., Uhlemann C., 2021, @doi [ ] 10.1093/mnras/staa3773 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..426H 503, 426

    work page doi:10.1093/mnras/staa3773 2021

  63. [63]

    S., Benitez-Llambay A., Helly J., 2018, @doi [ ] 10.1093/mnras/stx2792 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.474..604H 474, 604

    Han J., Cole S., Frenk C. S., Benitez-Llambay A., Helly J., 2018, @doi [ ] 10.1093/mnras/stx2792 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.474..604H 474, 604

    work page doi:10.1093/mnras/stx2792 2018

  64. [64]

    A., Cortese L., Obreschkow D., Catinella B., Cook R

    Hardwick J. A., Cortese L., Obreschkow D., Catinella B., Cook R. H. W., 2022, @doi [ ] 10.1093/mnras/stab3261 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.3751H 509, 3751

    work page doi:10.1093/mnras/stab3261 2022

  65. [65]

    E., Hoekstra H., McGibbon R

    Herle A., Chisari N. E., Hoekstra H., McGibbon R. J., Schaye J., Schaller M., Kugel R., 2025, @doi [ ] 10.1051/0004-6361/202554244 , https://ui.adsabs.harvard.edu/abs/2025A&A...699A.192H 699, A192

    work page doi:10.1051/0004-6361/202554244 2025

  66. [66]

    Hetznecker H., Burkert A., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10616.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.370.1905H 370, 1905

    work page doi:10.1111/j.1365-2966.2006.10616.x 2006

  67. [67]

    P., 1926, @doi [ ] 10.1086/143018 , https://ui.adsabs.harvard.edu/abs/1926ApJ....64..321H 64, 321

    Hubble E. P., 1926, @doi [ ] 10.1086/143018 , https://ui.adsabs.harvard.edu/abs/1926ApJ....64..321H 64, 321

    work page doi:10.1086/143018 1926

  68. [68]

    Huertas-Company M., et al., 2019, @doi [ ] 10.1093/mnras/stz2191 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.1859H 489, 1859

    work page doi:10.1093/mnras/stz2191 2019

  69. [69]

    Hu s ko F., et al., 2026, @doi [ ] 10.1093/mnras/stag324 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.547ag324H 547, stag324

    work page doi:10.1093/mnras/stag324 2026

  70. [70]

    , keywords =

    Jeeson-Daniel A., Dalla Vecchia C., Haas M. R., Schaye J., 2011, @doi [ ] 10.1111/j.1745-3933.2011.01081.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.415L..69J 415, L69

    work page doi:10.1111/j.1745-3933.2011.01081.x 2011

  71. [71]

    L., et al., 2022, @doi [ ] 10.1093/mnras/stac1622 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515...22J 515, 22

    Jung S. L., et al., 2022, @doi [ ] 10.1093/mnras/stac1622 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515...22J 515, 22

    work page doi:10.1093/mnras/stac1622 2022

  72. [72]

    Kaiser N., 1984, @doi [ ] 10.1086/184341 , https://ui.adsabs.harvard.edu/abs/1984ApJ...284L...9K 284, L9

    work page doi:10.1086/184341 1984

  73. [73]

    Klein C., et al., 2026, @doi [ ] 10.3847/1538-4357/ae31f4 , https://ui.adsabs.harvard.edu/abs/2026ApJ...998..125K 998, 125

    work page doi:10.3847/1538-4357/ae31f4 2026

  74. [74]

    Kugel R., et al., 2023, @doi [ ] 10.1093/mnras/stad2540 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.6103K 526, 6103

    work page doi:10.1093/mnras/stad2540 2023

  75. [75]

    Lagos C. d. P., Schaye J., Bah \'e Y., van de Sande J., Kay S. T., Barnes D., Davis T. A., Dalla Vecchia C., 2018, @doi [ ] 10.1093/mnras/sty489 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.476.4327L 476, 4327

    work page doi:10.1093/mnras/sty489 2018

  76. [76]

    Lagos C. d. P., et al., 2025, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv251211309L p. arXiv:2512.11309

    work page arXiv 2025

  77. [77]

    Lang P., et al., 2014, @doi [ ] 10.1088/0004-637X/788/1/11 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...11L 788, 11

    work page doi:10.1088/0004-637x/788/1/11 2014

  78. [78]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Li C., Kauffmann G., Jing Y. P., White S. D. M., B \"o rner G., Cheng F. Z., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10066.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.368...21L 368, 21

    work page doi:10.1111/j.1365-2966.2006.10066.x 2006

  79. [79]

    D., Schaye J., Schaller M., Richings J., 2019, @doi [ ] 10.1093/mnrasl/slz110 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.488L.123L 488, L123

    Ludlow A. D., Schaye J., Schaller M., Richings J., 2019, @doi [ ] 10.1093/mnrasl/slz110 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.488L.123L 488, L123

    work page doi:10.1093/mnrasl/slz110 2019

  80. [80]

    D., Schaye J., Schaller M., Bower R., 2020, @doi [ ] 10.1093/mnras/staa316 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.2926L 493, 2926

    Ludlow A. D., Schaye J., Schaller M., Bower R., 2020, @doi [ ] 10.1093/mnras/staa316 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.2926L 493, 2926

    work page doi:10.1093/mnras/staa316 2020

Showing first 80 references.