pith. sign in

arxiv: 2606.25359 · v1 · pith:XH52PFGYnew · submitted 2026-06-24 · 🌌 astro-ph.GA

Cosmological Galaxy Formation Modelling in the Era of the Square Kilometre Array

Claudia del P. Lagos (1) , Carlton M. Baugh , Connor Bottrell , Romeel Dave , Gabriella De Lucia , Jindra Gensior , Filip Hu\v{s}ko , Cedric G. Lacey
show 11 more authors
Danail Obreschkow Kyle Oman Chris Power Nicole Thomas Ruby J. Wright Lizhi Xie ((1) International Centre for Radio Astronomy Research (ICRAR) M468 University of Western Australia Crawley WA Australia)
This is my paper

Pith reviewed 2026-06-25 21:30 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy formationcosmological simulationssemi-analytic modelsSquare Kilometre Arrayatomic hydrogenmolecular gasradio continuumforward modeling
0
0 comments X

The pith

Galaxy formation models must combine simulations across scales with forward modeling to interpret Square Kilometre Array observations of cold gas and radio emission.

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

The paper reviews advances showing that cosmological hydrodynamical simulations and semi-analytic models now jointly match many observed properties of atomic hydrogen, molecular gas, and radio continuum from star formation and active galactic nuclei. It identifies the ongoing difficulty of connecting sub-parsec star formation physics to gigaparsec cosmic structure as the main remaining obstacle to using the Square Kilometre Array to map galaxies across cosmic time. The central proposal is that a coordinated wedding-cake strategy linking simulations at different resolutions, plus forward modeling of observables and AI-driven emulators, will let these models both explain SKA data and actively guide future observations.

Core claim

Cosmological hydrodynamical simulations and semi-analytic models now jointly reproduce many observed gas properties, yet the challenge of bridging physical scales from sub-parsec star formation to gigaparsec cosmic structure remains. A coordinated wedding-cake strategy that unites simulations of different scales, forward modelling of observables to ensure fair comparison with data, and integration of AI-driven emulators will enable theoretical models to both interpret and guide SKA science on the cold gas and radio continuum of galaxies across cosmic time.

What carries the argument

The wedding-cake strategy that unites simulations of different scales, together with forward modelling of observables.

If this is right

  • Models will predict atomic hydrogen, molecular gas distributions, and radio continuum from star formation and active galactic nuclei across cosmic time.
  • Forward modelling will produce simulated observables that can be compared directly to SKA data without selection biases.
  • AI-driven emulators will speed up exploration of model parameters and uncertainty quantification.
  • Theoretical models will shift from post-observation interpretation to active prediction and experimental design for SKA surveys.

Where Pith is reading between the lines

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

  • The same coordinated multi-scale approach could be adapted to prepare models for other upcoming large radio or optical surveys.
  • Success of the strategy might isolate specific physical processes that still require new implementations in the simulations.
  • One could test the framework by applying it to predict SKA-detectable signals in particular galaxy types or redshift ranges not yet observed.

Load-bearing premise

The scale-bridging challenge can be solved by coordinating existing simulations of different resolutions and adding forward modelling plus emulators, without needing fundamental new physics.

What would settle it

SKA observations revealing gas properties or radio emission patterns that remain irreproducible by any combination of current hydrodynamical and semi-analytic models after forward modelling and emulator application.

Figures

Figures reproduced from arXiv: 2606.25359 by Australia), Carlton M. Baugh, Cedric G. Lacey, Chris Power, Claudia del P. Lagos (1), Connor Bottrell, Crawley, Danail Obreschkow, Filip Hu\v{s}ko, Gabriella De Lucia, Jindra Gensior, Kyle Oman, Lizhi Xie ((1) International Centre for Radio Astronomy Research (ICRAR), M468, Nicole Thomas, Romeel Dave, Ruby J. Wright, University of Western Australia, WA.

Figure 1
Figure 1. Figure 1: Modified from Crain and van de Voort (2023) to show the processes that are happening at different scales and place them into the context of what is directly simulated and what is modelled via so called “subgrid physics models”. The exact transition of when one goes from directly simulating to modelling depends on the tools at hand. The arrows at the top show the regions that are typically directly simulate… view at source ↗
Figure 2
Figure 2. Figure 2: The distribution of gas particles or cells in the temperature vs density plane at 𝑧 = 0 in three different cosmological hydrodynamical simulations. Eagle (left panel) (Crain et al., 2017) lacked an explicit model of the ISM and instead imposed an equation of state. Here, pixels are coloured by the mass fraction, showing that most of the gas mass in the 𝑧 = 0 universe is in the form of hot, low-density gas.… view at source ↗
Figure 3
Figure 3. Figure 3: Left panels: Joint distribution of HI column density (𝑁HI) and velocity dispersion (𝜎). Pairs of values are drawn from corresponding pixels in the 0 th and 2 nd moment maps of high- (∼ 25” ; top row – HR) and low-resolution (∼ 65” ; bottom row – LR) spectral cubes obtained with MeerKAT (left column) for a sample of 5 L★ galaxies. The centre and right columns show the same measurement for samples of galaxie… view at source ↗
Figure 4
Figure 4. Figure 4: A compilation of observed galaxies collected by Santos-Santos et al. (2020) in the space of 𝜂rot and 𝜂bar. The 𝜂rot parameter is the ratio of the rotation curve amplitude at a suitably chosen ‘inner’ radius (𝑉fid) and its maximum (𝑉max), and serves as a proxy for the rotation curve shape: a higher (lower) value of 𝜂rot is suggestive of a dark matter cusp (core). The horizontal grey line marks the expectati… view at source ↗
Figure 5
Figure 5. Figure 5: The HI velocity width function is a strong constraint on the halo mass function of gas rich galaxies and therefore a potential test of cosmological models, but faithfully modelling the galaxy distribution in HI mass (𝑀HI) and line width (𝑤50) requires capturing the complexity of cold gas dynamics. A detailed forward model of the spectra of galaxies in the GALFORM semi-analytic model (green line, adapted fr… view at source ↗
Figure 6
Figure 6. Figure 6: Taken from Figures 4 and 7 in Gensior et al. (2024). The maps on the left show face-on projection of the HI surface density for four example galaxies in the EMP-Pathfinder simulations employing a constant star formation efficiency (top) and an efficiency that depends on the turbulence of the ISM (bottom). The plot on the right shows radial profiles of the HI disc scale heights of the simulated galaxies, sh… view at source ↗
Figure 7
Figure 7. Figure 7 [PITH_FULL_IMAGE:figures/full_fig_p016_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: The HI mass function at 𝑧 = 0 (solid lines), 𝑧 = 1 (dashed lines), and 𝑧 = 2 (dotted lines) in 3 semi-analytic models (Shark, GAEA, GALFORM) and 3 cosmological hydrodynamical simulations (Eagle, TNG and Simba), as labelled in each panel. Observations at 𝑧 ≈ 0 from Zwaan et al. (2005) and Jones et al. (2018) are shown as grey circles and crosses, respectively; while the inferred HI mass function at 𝑧 ≈ 1 fr… view at source ↗
Figure 9
Figure 9. Figure 9: The HI mass vs halo mass relation at 𝑧 = 0 in 3 cosmological hydrodynamical simulations (TNG and two Eagle realisations) and 3 semi-analytic models of galaxy formation (Shark, GAEA and GALFORM). Also included is the empirical results of Padmanabhan et al. (2017) for reference. For Eagle we also show individual massive halos with symbols in the regime where medians cannot be calculated due to the low number… view at source ↗
Figure 10
Figure 10. Figure 10: The Radio Luminosity Function (RLF) at 1.4 GHz between 𝑧=0 and 4 in the Shark semi-analytic model (Lagos et al., 2018, 2024). The top panels show the contribution from star formation; the middle panels from AGNs; and the lower panels show the combined contributions (i.e. star formation and AGNs). Comparisons are made with observational data of galaxies classified as star forming galaxies in the top panels… view at source ↗
Figure 11
Figure 11. Figure 11 [PITH_FULL_IMAGE:figures/full_fig_p023_11.png] view at source ↗
read the original abstract

Over the past decade, galaxy formation simulations have advanced dramatically, transforming our ability to model the interstellar medium (ISM) and predict galaxies' radio emission. Yet the challenge of bridging physical scales--from sub-parsec star formation to gigaparsec cosmic structure--remains. The Square Kilometre Array (SKA) will map the cold gas and radio continuum of galaxies across cosmic time, demanding models that couple physical realism with cosmological reach. This chapter reviews the state-of-the-art in cosmological galaxy formation modelling in preparation for the SKA. We outline progress in simulating atomic hydrogen (HI), molecular gas, and radio continuum emission from both star formation and active galactic nuclei, highlighting how cosmological hydrodynamical simulations and semi-analytic models now jointly reproduce many observed gas properties. We emphasise the need for a coordinated, ``wedding-cake'' strategy that unites simulations of different scales, for forward modelling of observables to ensure fair comparison with data, and for the integration of new technologies such as AI-driven emulators to accelerate progress. Together, these efforts will enable theoretical models to both interpret and guide SKA science, turning simulations from passive interpreters into active engines for discovery.

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

0 major / 1 minor

Summary. This review chapter summarizes advances in cosmological hydrodynamical simulations and semi-analytic models for predicting atomic (HI) and molecular gas properties as well as radio continuum emission from star formation and AGN. It states that these models now jointly reproduce many observed gas properties, identifies the persistent challenge of bridging sub-parsec to gigaparsec scales, and advocates a coordinated 'wedding-cake' multi-scale simulation strategy together with forward modeling of observables and AI-driven emulators to prepare for and interpret SKA data.

Significance. As a synthesis of the literature on ISM and radio modeling in cosmological contexts, the chapter provides a timely overview for the community ahead of SKA operations. Its emphasis on practical coordination strategies and new computational tools (emulators, forward modeling) offers guidance that could help turn existing simulation frameworks into more effective tools for both interpreting and planning SKA observations, provided the cited progress is accurately represented.

minor comments (1)
  1. The abstract paragraph on the 'wedding-cake' strategy would benefit from a brief parenthetical definition or cross-reference to the section where the term is first introduced in the main text, to aid readers unfamiliar with the concept.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive and constructive review. We are pleased that the manuscript is viewed as a timely synthesis providing useful guidance for the community ahead of SKA operations, and we appreciate the recommendation to accept.

Circularity Check

0 steps flagged

Review paper with no derivations or predictions that reduce to inputs

full rationale

This document is a review chapter summarizing published progress in hydrodynamical simulations and semi-analytic models for HI, molecular gas, and radio continuum. It advocates a wedding-cake multi-scale strategy, forward modeling, and AI emulators but presents no new equations, parameter fits, quantitative predictions, or derivation chains. All cited results come from external literature; the text contains no self-contained technical claims that could be circular by construction. This matches the default expectation of no significant circularity for review-style papers.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a review paper summarizing existing work; no new free parameters, axioms or invented entities are introduced.

pith-pipeline@v0.9.1-grok · 5822 in / 1072 out tokens · 35905 ms · 2026-06-25T21:30:28.719553+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

211 extracted references · 195 canonical work pages · 87 internal anchors

  1. [1]

    2026 ,publisher =

    Ran Wang and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  2. [2]

    Hardcastle and author2 and author3 and author4 and author5 ,title =

    Martin J. Hardcastle and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  3. [3]

    Duncan and author2 and author3 and author4 and author5 ,title =

    Kenneth J. Duncan and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  4. [4]

    2026 ,publisher =

    Manisha Caleb and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  5. [5]

    Mahony and author2 and author3 and author4 and author5 ,title =

    Elizabeth K. Mahony and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  6. [6]

    Tabatabaei and author2 and author3 and author4 and author5 ,title =

    Fatemeh S. Tabatabaei and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  7. [7]

    2026 ,publisher =

    Hiddo Sunny Bouwe Algera and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  8. [8]

    2026 ,publisher =

    Baerbel Koribalski and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  9. [9]

    2026 ,publisher =

    Hengxing Pan and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  10. [10]

    2026 ,publisher =

    Nathan Deg and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  11. [11]

    2026 ,publisher =

    Erik Rosolowsky and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  12. [12]

    2026 ,publisher =

    Erwin de Blok and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  13. [13]

    2026 ,publisher =

    Tommaso Ronconi and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  14. [14]

    2026 ,publisher =

    Federico Lelli and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  15. [15]

    2005, MNRAS, 364, L18, doi: 10.1111/j.1745-3933.2005.00096.x

    The HIPASS catalogue: _ HI and environmental effects on the HI mass function of galaxies. , eprint =. doi:10.1111/j.1745-3933.2005.00029.x , adsurl =

    work page doi:10.1111/j.1745-3933.2005.00029.x 2005

  16. [16]

    , keywords =

    The effects of local stellar radiation and dust depletion on non-equilibrium interstellar chemistry. , keywords =. doi:10.1093/mnras/stac2338 , archivePrefix =. 2208.02288 , primaryClass =

    work page doi:10.1093/mnras/stac2338

  17. [17]

    , keywords =

    Quenching massive galaxies across cosmic time with the semi-analytic model SHARK V2.0. , keywords =. doi:10.1093/mnras/stae1024 , archivePrefix =. 2309.02310 , primaryClass =

    work page doi:10.1093/mnras/stae1024

  18. [18]

    , eprint =

    The Global Schmidt Law in Star-forming Galaxies. , keywords =. doi:10.1086/305588 , archivePrefix =. astro-ph/9712213 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/305588

  19. [19]

    , keywords =

    Emergence and cosmic evolution of the Kennicutt-Schmidt relation driven by interstellar turbulence. , keywords =. doi:10.1051/0004-6361/202347917 , archivePrefix =. 2309.06485 , primaryClass =

    work page doi:10.1051/0004-6361/202347917

  20. [20]

    Kennicutt-Schmidt relation of galaxies over 13 billion years in the COLIBRE hydrodynamical simulations

    Kennicutt-Schmidt relation of galaxies over 13 billion years in the COLIBRE hydrodynamical simulations. , keywords =. doi:10.1093/mnras/stag947 , archivePrefix =. 2512.11309 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stag947

  21. [21]

    , keywords =

    WALLABY Pilot Survey: Characterizing Low-rotation Kinematically Modeled Galaxies. , keywords =. doi:10.3847/1538-4357/ae1003 , archivePrefix =. 2510.02522 , primaryClass =

    work page doi:10.3847/1538-4357/ae1003

  22. [22]

    , keywords =

    Dynamical disequilibrium in dwarf galaxies: rethinking gas dynamics, rotation curves, and dark matter inference. , keywords =. doi:10.1093/mnras/stag356 , archivePrefix =. 2512.11033 , primaryClass =

    work page doi:10.1093/mnras/stag356

  23. [23]

    , keywords =

    The physical drivers of gas turbulence in simulated disc galaxies. , keywords =. doi:10.1093/mnras/stad2119 , archivePrefix =. 2210.09673 , primaryClass =

    work page doi:10.1093/mnras/stad2119

  24. [24]

    HI-selected Galaxies in Hierarchical Models of Galaxy Formation and Evolution

    H I-selected galaxies in hierarchical models of galaxy formation and evolution. , keywords =. doi:10.1093/mnras/stw2901 , archivePrefix =. 1610.02042 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2901

  25. [25]

    , keywords =

    First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time. , keywords =. doi:10.1093/mnras/stz2338 , archivePrefix =. 1902.05553 , primaryClass =

    work page doi:10.1093/mnras/stz2338 1902

  26. [26]

    , keywords =

    The diverse star formation histories of early massive, quenched galaxies in modern galaxy formation simulations. , keywords =. doi:10.1093/mnras/stae2626 , archivePrefix =. 2409.16916 , primaryClass =

    work page doi:10.1093/mnras/stae2626

  27. [27]

    The CAMELS project: Cosmology and Astrophysics with MachinE Learning Simulations

    The CAMELS Project: Cosmology and Astrophysics with Machine-learning Simulations. , keywords =. doi:10.3847/1538-4357/abf7ba , archivePrefix =. 2010.00619 , primaryClass =

    work page doi:10.3847/1538-4357/abf7ba 2010

  28. [28]

    , keywords =

    Cosmological baryon spread and impact on matter clustering in CAMELS. , keywords =. doi:10.1093/mnras/stae817 , archivePrefix =. 2307.11832 , primaryClass =

    work page doi:10.1093/mnras/stae817

  29. [29]

    A unified multi-wavelength model of galaxy formation

    A unified multiwavelength model of galaxy formation. , keywords =. doi:10.1093/mnras/stw1888 , archivePrefix =. 1509.08473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1888

  30. [30]

    MNRAS , keywords =

    The effect of the environment on the H I scaling relations. , keywords =. doi:10.1111/j.1365-2966.2011.18822.x , archivePrefix =. 1103.5889 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18822.x 2011

  31. [31]

    Simulating Galaxy Formation with the IllustrisTNG Model

    Simulating galaxy formation with the IllustrisTNG model. , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2656

  32. [32]

    The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations

    The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations. , keywords =. doi:10.1093/mnras/stv725 , archivePrefix =. 1501.01311 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv725

  33. [33]

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

    COLIBRE: calibrating subgrid feedback in cosmological simulations that include a cold gas phase. , keywords =. doi:10.1093/mnras/stag300 , archivePrefix =. 2509.04067 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stag300

  34. [34]

    , keywords =

    Efficient Long-range Active Galactic Nuclei (AGNs) Feedback Affects the Low-redshift Ly Forest. , keywords =. doi:10.3847/2041-8213/acb7f1 , archivePrefix =. 2210.02467 , primaryClass =

    work page doi:10.3847/2041-8213/acb7f1 2041

  35. [35]

    , keywords =

    The FLAMINGO project: baryon effects on the matter power spectrum. , keywords =. doi:10.1093/mnras/staf569 , archivePrefix =. 2410.17109 , primaryClass =

    work page doi:10.1093/mnras/staf569

  36. [36]

    The effect of baryons on redshift space distortions and cosmic density and velocity fields in the EAGLE simulation

    The effect of baryons on redshift space distortions and cosmic density and velocity fields in the EAGLE simulation. , keywords =. doi:10.1093/mnrasl/slw081 , archivePrefix =. 1603.03328 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slw081

  37. [37]

    , keywords =

    Tracing the quenching journey across cosmic time. , keywords =. doi:10.1051/0004-6361/202349045 , archivePrefix =. 2401.06211 , primaryClass =

    work page doi:10.1051/0004-6361/202349045

  38. [38]

    The EAGLE project: Simulating the evolution and assembly of galaxies and their environments

    The EAGLE project: simulating the evolution and assembly of galaxies and their environments. , keywords =. doi:10.1093/mnras/stu2058 , archivePrefix =. 1407.7040 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2058

  39. [39]

    A New Public Release of the GIZMO Code

    A New Public Release of the GIZMO Code. arXiv e-prints , keywords =. doi:10.48550/arXiv.1712.01294 , archivePrefix =. 1712.01294 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1712.01294

  40. [40]

    , keywords =

    E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh. , keywords =. doi:10.1111/j.1365-2966.2009.15715.x , archivePrefix =. 0901.4107 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15715.x 2009

  41. [41]

    , keywords =

    SWIFT: A modern highly-parallel gravity and smoothed particle hydrodynamics solver for astrophysical and cosmological applications. , keywords =. doi:10.1093/mnras/stae922 , archivePrefix =. 2305.13380 , primaryClass =

    work page doi:10.1093/mnras/stae922

  42. [42]

    , keywords =

    Galaxy assembly and evolution in the P-Millennium simulation: Galaxy clustering. , keywords =. doi:10.1051/0004-6361/202452029 , archivePrefix =. 2409.02194 , primaryClass =

    work page doi:10.1051/0004-6361/202452029

  43. [43]

    , keywords =

    The radio galaxy population in the SIMBA simulations. , keywords =. doi:10.1093/mnras/stab654 , archivePrefix =. 2010.11225 , primaryClass =

    work page doi:10.1093/mnras/stab654 2010

  44. [44]

    , keywords =

    Environmental effects on satellite galaxies from the perspective of cold gas. , keywords =. doi:10.1093/mnras/stae162 , archivePrefix =. 2401.07158 , primaryClass =

    work page doi:10.1093/mnras/stae162

  45. [45]

    xGASS: Total cold gas scaling relations and molecular-to-atomic gas ratios of galaxies in the local Universe

    xGASS: total cold gas scaling relations and molecular-to-atomic gas ratios of galaxies in the local Universe. , keywords =. doi:10.1093/mnras/sty089 , archivePrefix =. 1802.02373 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty089

  46. [46]

    , keywords =

    The impact of ram pressure on cluster galaxies, insights from GAEA and TNG. , keywords =. doi:10.1051/0004-6361/202553915 , archivePrefix =. 2504.12863 , primaryClass =

    work page doi:10.1051/0004-6361/202553915

  47. [47]

    On the influence of environment on star forming galaxies

    On the influence of environment on star-forming galaxies. , keywords =. doi:10.1093/mnras/sty2131 , archivePrefix =. 1808.01628 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2131

  48. [48]

    , keywords =

    Exploring the Statistical Properties of Double Radio Relics in the TNG-cluster and TNG300 Simulations. , keywords =. doi:10.3847/1538-4357/ae3245 , archivePrefix =. 2510.21632 , primaryClass =

    work page doi:10.3847/1538-4357/ae3245

  49. [49]

    , keywords =

    An orbital perspective on the starvation, stripping, and quenching of satellite galaxies in the EAGLE simulations. , keywords =. doi:10.1093/mnras/stac2042 , archivePrefix =. 2205.08414 , primaryClass =

    work page doi:10.1093/mnras/stac2042

  50. [50]

    Physical drivers of galaxies' cold-gas content: exploring environmental and evolutionary effects with DARK SAGE

    Physical drivers of galaxies' cold-gas content: exploring environmental and evolutionary effects with Dark Sage. , keywords =. doi:10.1093/mnras/stx1596 , archivePrefix =. 1706.07434 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1596

  51. [51]

    Cold gas properties of the Herschel Reference Survey. III. Molecular gas stripping in cluster galaxies. , keywords =. doi:10.1051/0004-6361/201322313 , archivePrefix =. 1402.0326 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322313

  52. [52]

    , keywords =

    Angular momentum-related probe of cold gas deficiencies. , keywords =. doi:10.1093/mnras/staa514 , archivePrefix =. 2002.09083 , primaryClass =

    work page doi:10.1093/mnras/staa514 2002

  53. [53]

    The Messenger , year = 2023, month = mar, volume =

    The 4MOST Hemisphere Survey of the Nearby Universe (4HS). The Messenger , year = 2023, month = mar, volume =. doi:10.18727/0722-6691/5312 , adsurl =

    work page doi:10.18727/0722-6691/5312 2023

  54. [54]

    4MOST Consortium Survey 7: Wide-Area VISTA Extragalactic Survey (WAVES)

    4MOST Consortium Survey 7: Wide-Area VISTA Extragalactic Survey (WAVES). The Messenger , keywords =. doi:10.18727/0722-6691/5126 , archivePrefix =. 1903.02473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.18727/0722-6691/5126 1903

  55. [55]

    , keywords =

    Unveiling the atomic hydrogen-halo mass relation via spectral stacking. , keywords =. doi:10.1093/mnras/stab1925 , archivePrefix =. 2102.12203 , primaryClass =

    work page doi:10.1093/mnras/stab1925

  56. [56]

    Ingredients for 21cm intensity mapping

    Ingredients for 21 cm Intensity Mapping. , keywords =. doi:10.3847/1538-4357/aadba0 , archivePrefix =. 1804.09180 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aadba0

  57. [57]

    , keywords =

    The physical drivers of the atomic hydrogen-halo mass relation. , keywords =. doi:10.1093/mnras/staa2251 , archivePrefix =. 2006.12102 , primaryClass =

    work page doi:10.1093/mnras/staa2251 2006

  58. [58]

    The atomic hydrogen content of the post-reionization Universe , volume=

    The atomic hydrogen content of the post-reionization Universe. , keywords =. doi:10.1093/mnras/staa604 , archivePrefix =. 1909.02242 , primaryClass =

    work page doi:10.1093/mnras/staa604 1909

  59. [59]

    Galaxy formation in the Planck Millennium: the atomic hydrogen content of dark matter halos

    Galaxy formation in the Planck Millennium: the atomic hydrogen content of dark matter haloes. , keywords =. doi:10.1093/mnras/sty3427 , archivePrefix =. 1808.08276 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty3427

  60. [60]

    The clustering of ALFALFA galaxies: dependence on HI mass, relationship to optical samples & clues on host halo properties

    The Clustering of ALFALFA Galaxies: Dependence on H I Mass, Relationship with Optical Samples, and Clues of Host Halo Properties. , keywords =. doi:10.1088/0004-637X/776/1/43 , archivePrefix =. 1308.2661 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/776/1/43

  61. [61]

    The Weak Clustering of Gas-Rich Galaxies

    The Weak Clustering of Gas-rich Galaxies. , keywords =. doi:10.1086/508799 , archivePrefix =. astro-ph/0608633 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/508799

  62. [62]

    Evidence for the inside-out formation of Galactic discs

    Grand unification of AGN activity in the CDM cosmology. , keywords =. doi:10.1111/j.1365-2966.2010.17427.x , archivePrefix =. 0911.1128 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17427.x 2010

  63. [63]

    , keywords =

    A hybrid active galactic nucleus feedback model with spinning black holes, winds and jets. , keywords =. doi:10.1093/mnras/stag324 , archivePrefix =. 2509.05179 , primaryClass =

    work page doi:10.1093/mnras/stag324

  64. [64]

    , keywords =

    Radio galaxies in SIMBA: a MIGHTEE comparison. , keywords =. doi:10.1093/mnras/stae2724 , archivePrefix =. 2412.09824 , primaryClass =

    work page doi:10.1093/mnras/stae2724

  65. [65]

    A simulation-based analytic model of radio galaxies

    A simulation-based analytic model of radio galaxies. , keywords =. doi:10.1093/mnras/stx3358 , archivePrefix =. 1801.00667 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3358

  66. [66]

    , keywords =

    BRAiSE: Synthetic polarisation in RMHD AGN jet simulations. , keywords =. doi:10.1017/pasa.2025.10101 , archivePrefix =. 2506.19541 , primaryClass =

    work page doi:10.1017/pasa.2025.10101 2025

  67. [67]

    , keywords =

    3D hybrid fluid-particle jet simulations and the importance of synchrotron radiative losses. , keywords =. doi:10.1051/0004-6361/202450978 , archivePrefix =. 2409.05256 , primaryClass =

    work page doi:10.1051/0004-6361/202450978

  68. [68]

    2023, MNRAS, 526, 4978, doi: 10.1093/mnras/stad2419

    The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys. , keywords =. doi:10.1093/mnras/stad2419 , archivePrefix =. 2306.04024 , primaryClass =

    work page doi:10.1093/mnras/stad2419

  69. [69]

    , keywords =

    NEUTRALUNIVERSEMACHINE: Predictions of H I gas in different theoretical models. , keywords =. doi:10.1051/0004-6361/202452697 , archivePrefix =. 2410.19340 , primaryClass =

    work page doi:10.1051/0004-6361/202452697

  70. [70]

    Modeling the atomic-to-molecular transition in cosmological simulations of galaxy formation

    Modeling the Atomic-to-molecular Transition in Cosmological Simulations of Galaxy Formation. , keywords =. doi:10.3847/1538-4365/aae387 , archivePrefix =. 1806.02341 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aae387

  71. [71]

    , keywords =

    Resolution criteria to avoid artificial clumping in Lagrangian hydrodynamic simulations with a multiphase interstellar medium. , keywords =. doi:10.1093/mnras/stad3935 , archivePrefix =. 2310.10721 , primaryClass =

    work page doi:10.1093/mnras/stad3935

  72. [72]

    Variation of galactic cold gas reservoirs with stellar mass

    Variation of galactic cold gas reservoirs with stellar mass. , keywords =. doi:10.1093/mnras/stu2532 , archivePrefix =. 1412.0852 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2532

  73. [73]

    Which galaxies dominate the neutral gas content of the Universe?

    Which galaxies dominate the neutral gas content of the Universe?. , keywords =. doi:10.1093/mnras/stu266 , archivePrefix =. 1310.4178 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu266

  74. [74]

    Line Overlap and Self-Shielding of Molecular Hydrogen in Galaxies

    Line Overlap and Self-Shielding of Molecular Hydrogen in Galaxies. , keywords =. doi:10.1088/0004-637X/795/1/37 , archivePrefix =. 1406.4129 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/795/1/37

  75. [75]

    Shark: introducing an open source, free and flexible semi-analytic model of galaxy formation

    Shark: introducing an open source, free, and flexible semi-analytic model of galaxy formation. , keywords =. doi:10.1093/mnras/sty2440 , archivePrefix =. 1807.11180 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2440

  76. [76]

    , keywords =

    Origin of the galaxy H I size-mass relation. , keywords =. doi:10.1093/mnras/stz2513 , archivePrefix =. 1908.11149 , primaryClass =

    work page doi:10.1093/mnras/stz2513 1908

  77. [77]

    , keywords =

    The Variation of the Gas Content of Galaxy Groups and Pairs Compared to Isolated Galaxies. , keywords =. doi:10.3847/1538-4357/ac49ea , archivePrefix =. 2201.03575 , primaryClass =

    work page doi:10.3847/1538-4357/ac49ea

  78. [78]

    , keywords =

    Global H I asymmetries in IllustrisTNG: a diversity of physical processes disturb the cold gas in galaxies. , keywords =. doi:10.1093/mnras/staa3200 , archivePrefix =. 2010.05422 , primaryClass =

    work page doi:10.1093/mnras/staa3200 2010

  79. [79]

    , keywords =

    Exploring the angular momentum - atomic gas content connection with EAGLE and IllustrisTNG. , keywords =. doi:10.1093/mnras/stad2805 , archivePrefix =. 2307.02722 , primaryClass =

    work page doi:10.1093/mnras/stad2805

  80. [80]

    , keywords =

    Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time. , keywords =. doi:10.1051/0004-6361/202039429 , archivePrefix =. 2009.10578 , primaryClass =

    work page doi:10.1051/0004-6361/202039429 2009

Showing first 80 references.