pith. sign in

arxiv: 2605.16505 · v1 · pith:H2F2JL4Tnew · submitted 2026-05-15 · 🌌 astro-ph.GA

Feedback driven interactions between dark and luminous matter to explain tight galaxy scaling relations

Leen Alrawas , Andrea V. Macci\`o , Carlo Cannarozzo This is my paper

Pith reviewed 2026-05-20 15:48 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy scaling relationsstellar feedbackdark matter haloshydrodynamical simulationsbaryon-dark matter couplingdisk-halo connectioncosmic evolution
0
0 comments X

The pith

Stellar feedback in standard simulations naturally produces the tight observed link between galaxy disk sizes and dark matter halo radii.

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

The paper examines why galaxies show a remarkably tight correlation between the scale length of their stellar disks and the characteristic radius of their dark matter halos. Using cosmological simulations that incorporate only gravity and ordinary baryonic processes, it finds that this relation emerges automatically from the way feedback from stars rearranges the inner structure of halos. Tracking the same galaxies across cosmic time reveals that most systems adjust their disk and halo scales together, keeping the relation tight as they evolve. This outcome suggests the coupling between luminous and dark matter is a consequence of ordinary feedback rather than any new interaction in the dark sector.

Core claim

Hydrodynamical simulations that include only gravitational interactions and stellar feedback reproduce both the normalization and small scatter of the observed relation between stellar disk scale length Rd and dark matter scale radius r0 at the present day. Galaxies follow three evolutionary paths but preferentially move along the relation while their stellar and dark components rebalance, resulting in mild changes to normalization and slope from redshift 2 to 0. Direct comparison to dark-matter-only runs isolates the role of baryons in reshaping the central potential.

What carries the argument

The Rd-r0 scaling relation, whose evolution is isolated by comparing full hydrodynamical runs to their dark-matter-only counterparts to reveal the structural impact of stellar feedback.

If this is right

  • Galaxies evolve along the relation as stellar and dark matter scales adjust together over time.
  • The relation's normalization decreases mildly and its slope flattens slightly from z=2 to z=0.
  • Stellar feedback is sufficient to establish the observed coupling without additional dark-sector physics.
  • Three distinct evolutionary classes appear: disk expansion, contraction, and quasi-static evolution.

Where Pith is reading between the lines

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

  • Similar feedback-driven adjustments may underlie other tight galaxy scaling relations such as the Tully-Fisher or size-luminosity correlations.
  • High-redshift surveys could test whether the relation's scatter decreases toward lower redshift as predicted.
  • If the mechanism holds, models of galaxy formation can rely on standard feedback prescriptions rather than invoking direct dark matter-baryon couplings.

Load-bearing premise

The specific feedback implementation and numerical resolution used in the simulations correctly capture the dominant processes that set the relation between stellar disks and dark matter halos in real galaxies.

What would settle it

Precise measurements of the Rd-r0 relation at redshift 2 that show a normalization offset larger than 0.1 dex or a slope outside 0.8-1.2 would contradict the predicted mild evolution.

Figures

Figures reproduced from arXiv: 2605.16505 by Andrea V. Macci\`o, Carlo Cannarozzo, Leen Alrawas.

Figure 1
Figure 1. Figure 1: 𝑟0 versus 𝑅𝑑 in observed and simulated galaxies. The dashed line is the fit calculated in this work for the observed galaxies, and the green line is the fit reported in Salucci et al. (2020); Nesti et al. (2023) for selected datasets. following the methodology adopted in Salucci et al. (2020) and Nesti et al. (2023). Two examples of simulated profiles and relative fits are shown in Fig.2 for the dark matte… view at source ↗
Figure 2
Figure 2. Figure 2: The dark matter density profile for a halo of mass 2.41 × 1011𝑀⊙ fitted to the ISO profile 3, and the surface stellar density profile for the same halo fitted to the Freeman disk 1. in both scales. Additionally, a small number of galaxies exhibit more stochastic behavior, scattering around a localized region of the plane without adhering to a clear evolutionary path. To better quantify the evolutionary beh… view at source ↗
Figure 3
Figure 3. Figure 3: Evolution of the 𝑅𝑑 −𝑟0 relation for individual galaxies in the NIHAO sample. Each panel shows the evolutionary track of a single galaxy in the log(𝑅𝑑 )–log(𝑟0 ) plane, color-coded by redshift from 𝑧 = 2 (red) to 𝑧 = 0 (violet). The trajectories have been smoothed using spline interpolation, and arrows indicate the direction of evolution toward decreasing redshift. The black solid curve represents the medi… view at source ↗
Figure 5
Figure 5. Figure 5: 𝑟0 versus 𝑅𝑑 for simulated galaxies at 𝑧 = 0, divided into three groups, expanding (red dots), contracting (blue squares), and quasi-static galaxies (green diamonds), according to their evolutionary tracks on the plane. The gray line represents the fit derived in this work for observed galaxies. ulations exhibit markedly different trajectories and a larger scatter, indicating that baryonic processes signif… view at source ↗
Figure 4
Figure 4. Figure 4: The time evolution of three halos on the 𝑅𝑑 −𝑟0 relation from 𝑧 = 2 to 𝑧 = 0 where a fainter point indicates an earlier time. The plot shows an expansion of the 3.49 × 1011𝑀⊙ galaxy and a contraction of the 1.77 × 1012𝑀⊙ galaxy over time, while the third galaxy of mass 5.02 × 1011𝑀⊙ doesn’t follow either trend but remains scattered around the same region. Here, 𝜌0 denotes the central density, corresponding… view at source ↗
Figure 6
Figure 6. Figure 6: The dark matter core radius 𝑟0 versus the total dark matter halo mass of all galaxies at 𝑧 = 0. properties across the three classified groups. Our analysis indicates that stellar and halo mass are key drivers of the evolutionary di￾rection, as shown in [PITH_FULL_IMAGE:figures/full_fig_p006_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The time evolution of three halos on the 𝑟0–dark matter halo mass plane from 𝑧 = 2 to 𝑧 = 0 comparing Hydro and DMO runs. The figure shows three representative cases: a contracting galaxy with halo mass 1.77 × 1012, 𝑀⊙ (upper panel); a quasi-static galaxy with mass 5.02 × 1011, 𝑀⊙ (mid panel); an expanding galaxy with mass 3.49 × 1011, 𝑀⊙ (lower panel). original NFW-like profile (Navarro 2000), showing no … view at source ↗
Figure 8
Figure 8. Figure 8: The stellar mass versus the total halo mass of all galaxies at 𝑧 = 0. 0 2 4 6 Median SFR [ M yr − 1 ] Expanding Contracting Quasi-static 0 2 4 6 8 10 12 14 Time [Gyr] 109 1010 Median DM Mass (r <4 kpc) [ M ] [PITH_FULL_IMAGE:figures/full_fig_p007_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The top plot shows the median star formation rate over galaxies in each group according to how the galaxy evolves on the 𝑅𝑑 −𝑟0 relation, while the bottom plot shows the median dark matter mass within 4 kpc for each group. 108 109 1010 1011 10 12 Total Stellar Mass [M ] −2.00 −1.75 −1.50 −1.25 −1.00 −0.75 −0.50 −0.25 α (1 − 2%r/Rvir ) Model - Macci`o et al. (2020) Expanding Contracting Quasi-static [PITH_… view at source ↗
Figure 11
Figure 11. Figure 11: Cosmic evolution of the 𝑅𝑑 −𝑟0 relation from 𝑧 = 2 to 𝑧 = 0. The solid colored lines show the median relation at different redshifts (𝑧 = 0, 0.5, 1, 1.5, 2). The shaded bands represent the 1𝜎 credible regions from the Bayesian hierarchical model. The black points correspond to all NIHAO galaxies across all available snapshots between 𝑧 = 2 and 𝑧 = 0. The light gray dotted line shows the relation from Salu… view at source ↗
Figure 12
Figure 12. Figure 12: Posterior probability density functions (PDFs) for the normal￾ization (log 𝑟0,0, left) and slope (𝛼0, right) of the 𝑅𝑑 −𝑟0 relation at 𝑧 = 0. The colored curves show the marginalized PDFs, with dashed vertical lines marking the median values and shaded regions indicating the 1𝜎 (dark) and 2𝜎 (light) credible intervals. Black circles and horizontal error bars denote the observational estimates from Salucci… view at source ↗
Figure 13
Figure 13. Figure 13: Cartoon representation of the evolutionary pathways of galaxies in the 𝑅𝑑–𝑟0 plane and related quantities. The left panel illustrates the average evolutionary trajectories of “expanding” (red), “contracting” (blue), and “quasi-static” (green) galaxies, which follow distinct pathways but converge toward the same tight 𝑧 = 0 relation (orange line). The large teal arrow indicates the overall trend with galax… view at source ↗
read the original abstract

The tight empirical correlation linking the stellar disk scale length $R_d$ to the dark matter scale radius $r_0$ has been proposed as possible evidence for a fundamental coupling between baryons and dark matter beyond gravity. We re-examine the physical origin of this relation using a sample of 31 galaxies from the NIHAO cosmological hydrodynamical simulations, which include no dark matter-baryon interactions beyond gravity and baryonic feedback processes. NIHAO naturally reproduces both the normalization and the small scatter of the observed $R_d-r_0$ relation at $z=0$, while yielding a slightly shallower slope. By tracking galaxies from $z=2$ to $z=0$, we identify three distinct evolutionary classes: systems undergoing disk expansion, contraction, and quasi-static evolution. Using a Bayesian hierarchical framework, we provide the first characterization of the cosmic evolution of the $R_d-r_0$ relation, tracing the evolution of its normalization, slope, and intrinsic scatter from $z=2$ to the present day. We find a mild decrease in normalization ($\sim0.07$ dex), a flattening of the slope from $\alpha \simeq 1.05$ to $\alpha \simeq 0.95$, and a weak decline in the intrinsic scatter toward lower redshift, suggesting that galaxies evolve preferentially along the relation while jointly re-balancing their stellar and dark matter scales. By comparing hydrodynamical simulations with their dark-matter-only counterparts, we isolate the impact of baryons and baryonic feedback on halo structure. Our results show that stellar feedback alone can reshape the central potential and naturally establish the observed coupling between luminous and dark matter, without requiring modifications to the dark sector.

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 uses a sample of 31 galaxies from the NIHAO cosmological hydrodynamical simulations (no dark matter-baryon interactions beyond gravity) to argue that stellar feedback alone reshapes the central potential and reproduces the observed tight Rd-r0 scaling relation at z=0, including normalization and small scatter (with a slightly shallower slope). By tracking galaxies from z=2 to z=0, the authors identify three evolutionary classes and employ a Bayesian hierarchical framework to characterize the mild redshift evolution of normalization, slope, and scatter, concluding that galaxies evolve preferentially along the relation and that no modifications to the dark sector are required.

Significance. If robust, the result would be significant for galaxy formation studies: it supplies a concrete baryonic mechanism for the Rd-r0 coupling via feedback-driven potential reshaping, supported by forward simulation rather than post-hoc fitting and by direct hydro versus DM-only contrasts. The evolutionary tracking and first characterization of the relation's cosmic evolution add value, as does the isolation of baryonic effects on halo structure.

major comments (3)
  1. [Methods] Methods section: NIHAO feedback efficiencies were previously tuned to reproduce the stellar mass function and other z=0 properties. Without resolution convergence tests or explicit variations in feedback strength, it remains possible that the reproduction of the Rd-r0 normalization, slope, and scatter is a consequence of this calibration rather than a generic outcome of stellar feedback. This directly affects the central claim that the coupling arises naturally without dark-sector modifications.
  2. [Results] Results (hydro vs. DM-only comparison): The manuscript states that hydro runs reproduce the relation while matched DM-only runs do not, but does not quantify the changes in central potential or density profile (e.g., via explicit profiles or potential depth metrics) that would demonstrate how feedback sets r0 to track Rd. This step is load-bearing for isolating the baryonic mechanism.
  3. [Evolutionary analysis] Evolutionary analysis (§ on tracking from z=2 to z=0): The Bayesian hierarchical fit reports a mild normalization decrease (~0.07 dex), slope flattening from α ≃ 1.05 to α ≃ 0.95, and weak scatter decline. The priors, likelihood construction, and robustness to sample selection within the 31-galaxy suite should be shown explicitly, as the evolutionary classes (expansion, contraction, quasi-static) rely on internal tracking that could be sensitive to the specific sub-grid implementation.
minor comments (2)
  1. [Abstract] Abstract and main text: The slope parameter α is introduced without an explicit equation (e.g., whether log Rd = α log r0 + const); adding this definition would improve clarity for readers.
  2. [Figures] Figures: Captions for the Rd-r0 plots should explicitly reference the observational sample used for comparison and indicate which points correspond to the three evolutionary classes.

Simulated Author's Rebuttal

3 responses · 1 unresolved

We thank the referee for their constructive and detailed comments, which have helped clarify several aspects of our analysis. We address each major comment point by point below. Revisions have been made to improve methodological transparency, add quantitative comparisons, and expand the evolutionary analysis where feasible. These changes strengthen the manuscript without altering its core conclusions regarding stellar feedback's role in the Rd-r0 relation.

read point-by-point responses

  1. Referee: [Methods] Methods section: NIHAO feedback efficiencies were previously tuned to reproduce the stellar mass function and other z=0 properties. Without resolution convergence tests or explicit variations in feedback strength, it remains possible that the reproduction of the Rd-r0 normalization, slope, and scatter is a consequence of this calibration rather than a generic outcome of stellar feedback. This directly affects the central claim that the coupling arises naturally without dark-sector modifications.

    Authors: We acknowledge that the NIHAO feedback parameters were calibrated to match the stellar mass function and other z=0 global properties, as detailed in the original NIHAO papers. However, the Rd-r0 relation was not a target of this calibration and emerges as an independent prediction. In the revised manuscript, we have added a dedicated paragraph in the Methods section emphasizing this distinction and noting that the relation holds across the diverse galaxy sample. We also reference prior NIHAO studies that performed resolution convergence tests for structural properties. While we cannot introduce new feedback variations or resolution tests in this work, the reproduction of the observed normalization and scatter with the standard setup supports our conclusion that stellar feedback can establish the coupling without dark-sector modifications. revision: partial

  2. Referee: [Results] Results (hydro vs. DM-only comparison): The manuscript states that hydro runs reproduce the relation while matched DM-only runs do not, but does not quantify the changes in central potential or density profile (e.g., via explicit profiles or potential depth metrics) that would demonstrate how feedback sets r0 to track Rd. This step is load-bearing for isolating the baryonic mechanism.

    Authors: We agree that explicit quantification of the central potential and density profile changes would strengthen the isolation of the baryonic mechanism. In the revised Results section, we now include direct comparisons of dark matter density profiles for matched hydrodynamical and DM-only runs at z=0. We additionally report metrics such as the central potential depth (evaluated at 0.1 r_vir) and show that feedback induces a shallower inner density slope, enabling r0 to adjust in tandem with Rd. These additions demonstrate how stellar feedback reshapes the halo to produce the observed coupling. revision: yes

  3. Referee: [Evolutionary analysis] Evolutionary analysis (§ on tracking from z=2 to z=0): The Bayesian hierarchical fit reports a mild normalization decrease (~0.07 dex), slope flattening from α ≃ 1.05 to α ≃ 0.95, and weak scatter decline. The priors, likelihood construction, and robustness to sample selection within the 31-galaxy suite should be shown explicitly, as the evolutionary classes (expansion, contraction, quasi-static) rely on internal tracking that could be sensitive to the specific sub-grid implementation.

    Authors: We have expanded the Evolutionary analysis section to explicitly document the Bayesian hierarchical model. This includes the priors (wide normal distributions for normalization and slope, half-normal for intrinsic scatter), the likelihood formulation (linear relation with redshift-dependent parameters and Gaussian scatter), and robustness checks via jackknife resampling of the 31-galaxy sample, which yields consistent evolutionary trends. The three evolutionary classes are now defined quantitatively based on the sign and magnitude of ΔRd and Δr0 from z=2 to z=0, with a supplementary table listing classifications for each galaxy. While some sensitivity to sub-grid physics is inherent to any simulation suite, our results are presented as specific to the NIHAO model. revision: yes

standing simulated objections not resolved
  • New simulations with explicit variations in feedback strength or additional resolution convergence tests tailored to the Rd-r0 relation cannot be performed within the scope of this revision, as they would require rerunning the full NIHAO suite.

Circularity Check

0 steps flagged

No circularity: forward simulations compared to external observations

full rationale

The paper performs forward cosmological hydrodynamical simulations in the NIHAO suite, evolves galaxies from z=2 to z=0, and directly compares the resulting Rd-r0 distribution to independent observational data. The central claim that stellar feedback reshapes the central potential is supported by the difference between hydro runs and matched DM-only runs, plus the match to external galaxy scaling relations. The Bayesian hierarchical fit is applied only to characterize evolution inside the simulated sample and does not redefine or fit the target relation parameters to the same data used to claim success. No step reduces the reported outcome to a fitted input or self-citation by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The claim depends on the assumption that the chosen feedback implementation and galaxy sample faithfully represent real baryonic physics; no new particles or forces are introduced.

axioms (1)
  • domain assumption NIHAO simulations include standard baryonic feedback processes without additional dark-matter-baryon interactions beyond gravity
    Invoked to explain the emergence of the Rd-r0 relation from gravity plus feedback alone

pith-pipeline@v0.9.0 · 5854 in / 1223 out tokens · 42360 ms · 2026-05-20T15:48:59.552801+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

91 extracted references · 91 canonical work pages · 6 internal anchors

  1. [1]

    A Universal Density Profile from Hierarchical Clustering

    A Universal Density Profile from Hierarchical Clustering. , keywords =. doi:10.1086/304888 , archivePrefix =. astro-ph/9611107 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/304888

  2. [2]

    and Häußler, Boris and Brough, Sarah and Driver, Simon P

    Kennedy, Rebecca and Bamford, Steven P. and Häußler, Boris and Brough, Sarah and Driver, Simon P. and others , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2015 , doi =

    work page 2015

  3. [3]

    and Häußler, Boris and Vika, Marina and Brough, Sarah and others , title =

    Vulcani, Benedetta and Bamford, Steven P. and Häußler, Boris and Vika, Marina and Brough, Sarah and others , title =. The Astrophysical Journal , volume =. 2014 , doi =

    work page 2014

  4. [4]

    Astronomy & Astrophysics , volume =

    Baes, Maarten and Camps, Peter and Rodriguez-Gomez, Vicente and Nelson, Dylan and Pillepich, Annalisa and others , title =. Astronomy & Astrophysics , volume =. 2024 , doi =

    work page 2024

  5. [5]

    An important paper , journal=

    work page

  6. [6]

    Reproducing the inefficiency of galaxy formation across cosmic time with a large sample of cosmological hydrodynamical simulations , author=

    NIHAO project--I. Reproducing the inefficiency of galaxy formation across cosmic time with a large sample of cosmological hydrodynamical simulations , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2015 , publisher=

    work page 2015

  7. [7]

    Introducing black hole formation, accretion, and feedback into the NIHAO simulation suite , author=

    NIHAO--XXII. Introducing black hole formation, accretion, and feedback into the NIHAO simulation suite , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2019 , publisher=

    work page 2019

  8. [8]

    Monthly Notices of the Royal Astronomical Society , volume=

    Gasoline2: a modern smoothed particle hydrodynamics code , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2017 , publisher=

    work page 2017

  9. [9]

    Monthly Notices of the Royal Astronomical Society , volume=

    Making Galaxies In a Cosmological Context: the need for early stellar feedback , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2013 , publisher=

    work page 2013

  10. [10]

    cosmological parameters , author=

    Planck 2015 results-xiii. cosmological parameters , author=. Astronomy & Astrophysics , volume=. 2016 , publisher=

    work page 2015

  11. [11]

    Universe , volume=

    Paradigms and scenarios for the dark matter phenomenon , author=. Universe , volume=. 2020 , publisher=

    work page 2020

  12. [12]

    Astrophysical Journal, vol

    On the disks of spiral and S0 galaxies , author=. Astrophysical Journal, vol. 160, p. 811 , volume=

    work page

  13. [13]

    The Astrophysical Journal , volume=

    Dark matter scaling relations , author=. The Astrophysical Journal , volume=. 2000 , publisher=

    work page 2000

  14. [14]

    Astronomy , volume=

    The Quest for the Nature of the Dark Matter: The Need of a New Paradigm , author=. Astronomy , volume=. 2023 , publisher=

    work page 2023

  15. [15]

    A numerical convergence study , author=

    The inner structure of CDM haloes—I. A numerical convergence study , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2003 , publisher=

    work page 2003

  16. [16]

    Dark matter density shaped by black hole feedback , author=

    NIHAO--XXIII. Dark matter density shaped by black hole feedback , author=. Monthly Notices of the Royal Astronomical Society: Letters , volume=. 2020 , publisher=

    work page 2020

  17. [17]

    Monthly Notices of the Royal Astronomical Society , volume=

    NIHAO--IV: core creation and destruction in dark matter density profiles across cosmic time , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2016 , publisher=

    work page 2016

  18. [18]

    Monthly Notices of the Royal Astronomical Society , volume=

    The universal rotation curve of dwarf disc galaxies , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2017 , publisher=

    work page 2017

  19. [19]

    Monthly Notices of the Royal Astronomical Society , volume=

    Cores of dark matter haloes correlate with stellar scalelengths , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2004 , publisher=

    work page 2004

  20. [20]

    Galaxies , volume=

    Small scale problems of the CDM model: a short review , author=. Galaxies , volume=. 2017 , publisher=

    work page 2017

  21. [21]

    The Astrophysical Journal , volume=

    The baryonic tully-fisher relation , author=. The Astrophysical Journal , volume=. 2000 , publisher=

    work page 2000

  22. [22]

    Standard CDM model , author=

    The stellar-to-halo mass relation over the past 12 Gyr-I. Standard CDM model , author=. Astronomy & Astrophysics , volume=. 2020 , publisher=

    work page 2020

  23. [23]

    The Astrophysical Journal Letters , volume=

    The stellar-to-halo mass relation for local group galaxies , author=. The Astrophysical Journal Letters , volume=. 2014 , publisher=

    work page 2014

  24. [24]

    The Astrophysical Journal , volume=

    Metallicity calibrations and the mass-metallicity relation for star-forming galaxies , author=. The Astrophysical Journal , volume=. 2008 , publisher=

    work page 2008

  25. [25]

    Monthly Notices of the Royal Astronomical Society , volume=

    The origin and evolution of the galaxy mass--metallicity relation , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2016 , publisher=

    work page 2016

  26. [26]

    Dark Halo and Disk Galaxy Scaling Laws

    Dark halo and disk galaxy scaling laws , author=. arXiv preprint astro-ph/0012334 , year=

    work page internal anchor Pith review Pith/arXiv arXiv

  27. [27]

    Monthly Notices of the Royal Astronomical Society: Letters , volume=

    NIHAO V: too big does not fail--reconciling the conflict between CDM predictions and the circular velocities of nearby field galaxies , author=. Monthly Notices of the Royal Astronomical Society: Letters , volume=. 2016 , publisher=

    work page 2016

  28. [28]

    Monthly Notices of the Royal Astronomical Society , volume=

    NIHAO-UHD: the properties of MW-like stellar discs in high-resolution cosmological simulations , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2020 , publisher=

    work page 2020

  29. [29]

    Astronomy and Astrophysics, vol

    A new method of determining distances to galaxies , author=. Astronomy and Astrophysics, vol. 54, no. 3, Feb. 1977, p. 661-673. , volume=

    work page 1977

  30. [30]

    Monthly Notices of the Royal Astronomical Society: Letters , volume=

    A scaling relation for disc galaxies: Circular-velocity gradient versus central surface brightness , author=. Monthly Notices of the Royal Astronomical Society: Letters , volume=. 2013 , publisher=

    work page 2013

  31. [31]

    The Astrophysical Journal , volume=

    On the relation between circular velocity and central velocity dispersion in high and low surface brightness galaxies , author=. The Astrophysical Journal , volume=. 2005 , publisher=

    work page 2005

  32. [32]

    The interrelation between dark and luminous matter , author=

    The universal rotation curve of low surface brightness galaxies--IV. The interrelation between dark and luminous matter , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2019 , publisher=

    work page 2019

  33. [33]

    The Astrophysical Journal , volume=

    One law to rule them all: the radial acceleration relation of galaxies , author=. The Astrophysical Journal , volume=. 2017 , publisher=

    work page 2017

  34. [34]

    The Astrophysical Journal , volume=

    The accurate mass distribution of M87, the Giant Galaxy with imaged shadow of its supermassive black hole, as a portal to new Physics , author=. The Astrophysical Journal , volume=. 2022 , publisher=

    work page 2022

  35. [35]

    Monthly Notices of the Royal Astronomical Society , volume=

    Dark matter halo structure in CDM hydrodynamical simulations , author=. Monthly Notices of the Royal Astronomical Society , volume=. 1998 , publisher=

    work page 1998

  36. [36]

    Monthly Notices of the Royal Astronomical Society , volume=

    Chaos and variance in galaxy formation , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2019 , publisher=

    work page 2019

  37. [37]

    Monthly Notices of the Royal Astronomical Society , volume=

    A recipe for galaxy formation , author=. Monthly Notices of the Royal Astronomical Society , volume=. 1994 , publisher=

    work page 1994

  38. [38]

    Monthly Notices of the Royal Astronomical Society , volume=

    Concentration, spin and shape of dark matter haloes: scatter and the dependence on mass and environment , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2007 , publisher=

    work page 2007

  39. [39]

    The Astrophysical Journal , volume=

    The average star formation histories of galaxies in dark matter halos from z= 0--8 , author=. The Astrophysical Journal , volume=. 2013 , publisher=

    work page 2013

  40. [40]

    Origin of the MOND phenomenology of galactic rotation curves in a CDM universe , author=

    NIHAO--XVIII. Origin of the MOND phenomenology of galactic rotation curves in a CDM universe , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2019 , publisher=

    work page 2019

  41. [41]

    Monthly Notices of the Royal Astronomical Society , volume=

    A dark matter profile to model diverse feedback-induced core sizes of CDM haloes , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2020 , publisher=

    work page 2020

  42. [42]

    The Astrophysical Journal , volume=

    Fuzzy dark matter and dark matter halo cores , author=. The Astrophysical Journal , volume=. 2020 , publisher=

    work page 2020

  43. [43]

    Physical Review Letters , volume=

    Fuzzy cold dark matter: the wave properties of ultralight particles , author=. Physical Review Letters , volume=. 2000 , publisher=

    work page 2000

  44. [44]

    Monthly Notices of the Royal Astronomical Society , volume=

    Fuzzy Aquarius: evolution of a Milky-way like system in the Fuzzy Dark Matter scenario , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2023 , publisher=

    work page 2023

  45. [45]

    arXiv preprint arXiv:2411.09733 , year=

    Fuzzy Gasoline: Cosmological hydrodynamical simulations of dwarf galaxy formation with Fuzzy Dark Matter , author=. arXiv preprint arXiv:2411.09733 , year=

    work page arXiv

  46. [46]

    Journal of Cosmology and Astroparticle Physics , volume=

    Tully-Fisher relation, galactic rotation curves and dissipative mirror dark matter , author=. Journal of Cosmology and Astroparticle Physics , volume=. 2014 , publisher=

    work page 2014

  47. [47]

    DEUS Full Observable {\Lambda}CDM Universe Simulation: the numerical challenge

    DEUS Full Observable \ Lambda \ CDM Universe Simulation: the numerical challenge , author=. arXiv preprint arXiv:1206.2838 , year=

    work page internal anchor Pith review Pith/arXiv arXiv

  48. [48]

    arXiv preprint arXiv:2504.18618 , year=

    Lambda CDM is still not broken: empirical constraints on the star formation efficiency at z sim 12-30 , author=. arXiv preprint arXiv:2504.18618 , year=

    work page arXiv

  49. [49]

    , keywords =

    The challenge of simultaneously matching the observed diversity of chemical abundance patterns in cosmological hydrodynamical simulations. , keywords =. doi:10.1093/mnras/stab2736 , archivePrefix =. 2103.03884 , primaryClass =

    work page doi:10.1093/mnras/stab2736

  50. [50]

    Monthly Notices of the Royal Astronomical Society: Letters , volume=

    NIHAO X: reconciling the local galaxy velocity function with cold dark matter via mock H i observations , author=. Monthly Notices of the Royal Astronomical Society: Letters , volume=. 2016 , publisher=

    work page 2016

  51. [51]

    Galaxy metallicity scaling relations in the EAGLE simulations , journal =

    Mar. Galaxy metallicity scaling relations in the EAGLE simulations , journal =. 2017 , volume =

    work page 2017

  52. [52]

    , keywords =

    Abundance matching tested on small scales with galaxy dynamics. , keywords =. doi:10.1093/mnrasl/slaa094 , archivePrefix =. 2006.00818 , primaryClass =

    work page doi:10.1093/mnrasl/slaa094 2006

  53. [53]

    Computational Astrophysics and Cosmology , year =

    Dylan Nelson and Volker Springel and Federico Marinacci and Paul Torrey and Mark Vogelsberger and Annalisa Pillepich and … , title =. Computational Astrophysics and Cosmology , year =

    work page

  54. [54]

    , keywords =

    Galaxy-induced transformation of dark matter haloes. , keywords =. doi:10.1111/j.1365-2966.2010.16912.x , archivePrefix =. 0902.2477 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.16912.x 2010

  55. [55]

    dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evidences

    DYNESTY: a dynamic nested sampling package for estimating Bayesian posteriors and evidences. , keywords =. doi:10.1093/mnras/staa278 , archivePrefix =. 1904.02180 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa278 1904

  56. [56]

    doi:10.5281/zenodo.8408702 , version =

    joshspeagle/dynesty: v2.1.3. doi:10.5281/zenodo.8408702 , version =

    work page doi:10.5281/zenodo.8408702

  57. [57]

    Nested Sampling. Bayesian Inference and Maximum Entropy Methods in Science and Engineering: 24th International Workshop on Bayesian Inference and Maximum Entropy Methods in Science and Engineering , year = 2004, editor =. doi:10.1063/1.1835238 , adsurl =

    work page doi:10.1063/1.1835238 2004

  58. [58]

    Bayesian Analysis , keywords =

    John Skilling , doi =. Bayesian Analysis , keywords =. 2006 , bdsk-url-1 =

    work page 2006

  59. [59]

    , keywords =

    Contraction of Dark Matter Galactic Halos Due to Baryonic Infall. , keywords =. doi:10.1086/163867 , adsurl =

    work page doi:10.1086/163867

  60. [60]

    Halo expansion in cosmological hydro simulations: towards a baryonic solution of the cusp/core problem in massive spirals

    Halo Expansion in Cosmological Hydro Simulations: Toward a Baryonic Solution of the Cusp/Core Problem in Massive Spirals. , keywords =. doi:10.1088/2041-8205/744/1/L9 , archivePrefix =. 1111.5620 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/744/1/l9 2041

  61. [61]

    , author Padovani, P

    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

  62. [62]

    , author Tavecchio, F

    How supernova feedback turns dark matter cusps into cores. , keywords =. doi:10.1111/j.1365-2966.2012.20571.x , archivePrefix =. 1106.0499 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20571.x 2012

  63. [63]

    The Impact of Baryonic Physics on the Structure of Dark Matter Halos: the View from the FIRE Cosmological Simulations

    The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations. , keywords =. doi:10.1093/mnras/stv2165 , archivePrefix =. 1507.02282 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2165

  64. [64]

    , title =

    Mark Vogelsberger and Federico Marinacci and Paul Torrey and et al. , title =. Nature Reviews Physics , year =

    work page

  65. [65]

    Crain and Joop Schaye and Richard G

    Robert A. Crain and Joop Schaye and Richard G. Bower and Michelle Furlong and Matthieu Schaller and Tom Theuns and Claudio Dalla Vecchia and Carlos S. Frenk and Ian G. McCarthy and John C. Helly and Adrian Jenkins and Yetli M. Rosas-Guevara and Simon D. M. White and James W. Trayford , title =. Monthly Notices of the Royal Astronomical Society , year =

    work page

  66. [66]

    Monthly Notices of the Royal Astronomical Society , volume=

    NIHAO XII: galactic uniformity in a CDM universe , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2017 , publisher=

    work page 2017

  67. [67]

    Reproducing the observed diversity of dwarf galaxy rotation curve shapes in CDM , author=

    NIHAO--XIV. Reproducing the observed diversity of dwarf galaxy rotation curve shapes in CDM , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2018 , publisher=

    work page 2018

  68. [68]

    Monthly Notices of the Royal Astronomical Society , volume=

    NIHAO XV: the environmental impact of the host galaxy on galactic satellite and field dwarf galaxies , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2019 , publisher=

    work page 2019

  69. [69]

    , keywords =

    The cosmic evolution of the stellar mass-velocity dispersion relation of early-type galaxies. , keywords =. doi:10.1093/mnras/staa2147 , archivePrefix =. 1910.06987 , primaryClass =

    work page doi:10.1093/mnras/staa2147 1910

  70. [70]

    , keywords =

    Gas accretion at high redshift: cold flows all the way. , keywords =. doi:10.1093/mnras/staf198 , archivePrefix =. 2501.19009 , primaryClass =

    work page doi:10.1093/mnras/staf198

  71. [71]

    A detailed comparison of observed and simulated spiral galaxy scaling relations , author=

    MaNGA galaxy properties--II. A detailed comparison of observed and simulated spiral galaxy scaling relations , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2023 , publisher=

    work page 2023

  72. [72]

    Dark matter in the Milky Way. I. The isothermal disk approximation , author=. The Astrophysical Journal , volume=. 2003 , publisher=

    work page 2003

  73. [73]

    Monthly Notices of the Royal Astronomical Society , volume=

    Extended rotation curves of spiral galaxies: Dark haloes and modified dynamics , author=. Monthly Notices of the Royal Astronomical Society , volume=. 1991 , publisher=

    work page 1991

  74. [74]

    The Astrophysical Journal , volume=

    The structure of dark matter halos in dwarf galaxies , author=. The Astrophysical Journal , volume=. 1995 , publisher=

    work page 1995

  75. [75]

    Annual Review of Astronomy and Astrophysics , volume=

    Physical models of galaxy formation in a cosmological framework , author=. Annual Review of Astronomy and Astrophysics , volume=. 2015 , publisher=

    work page 2015

  76. [76]

    Annual review of astronomy and astrophysics , volume=

    Theoretical challenges in galaxy formation , author=. Annual review of astronomy and astrophysics , volume=. 2017 , publisher=

    work page 2017

  77. [77]

    Monthly Notices of the Royal Astronomical Society , volume=

    FIRE-2 simulations: physics versus numerics in galaxy formation , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2018 , publisher=

    work page 2018

  78. [78]

    Annual Review of Astronomy and Astrophysics , volume=

    The evolution of galaxy structure over cosmic time , author=. Annual Review of Astronomy and Astrophysics , volume=. 2014 , publisher=

    work page 2014

  79. [79]

    Monthly Notices of the Royal Astronomical Society , volume=

    Synthetic galaxy images and spectra from the Illustris simulation , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2015 , publisher=

    work page 2015

  80. [80]

    Monthly Notices of the Royal Astronomical Society , volume=

    The EAGLE project: simulating the evolution and assembly of galaxies and their environments , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2015 , publisher=

    work page 2015

Showing first 80 references.