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arxiv: 2606.04793 · v1 · pith:VHOPQBPZnew · submitted 2026-06-03 · 🌌 astro-ph.GA

Cooler Phases of the Circumgalactic Medium Are More Centrally Concentrated: Constraints from Multiphase Absorption Lines

Weiwen Kong , Zeyu Chen , Enci Wang , Haoran Yu , Kai Wang , Dongdong Shi , Cheqiu Lyu , Yuxuan Zhang
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Haoyi Zhang Haowen Guan
This is my paper

Pith reviewed 2026-06-28 05:30 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords circumgalactic mediumabsorption linesmultiphase gasradial profilesgalaxy haloscool gaswarm gasequivalent width
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The pith

Cooler circumgalactic gas concentrates closer to galaxies than warmer gas.

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

The paper stacks absorption signals from Ca II, Mg II, and C IV ions around galaxies and quasars to measure how absorption strength changes with distance. Ions linked to cooler gas produce steeper declines in equivalent width than ions linked to warmer gas. The pattern matches simulation predictions and differs between emission-line galaxy halos, which show a clear cool-to-warm shift, and quasar halos, which appear more uniform. The scaling with distance also depends strongly on host stellar mass for the cooler phases.

Core claim

Equivalent width profiles traced by ions that probe progressively cooler gas become increasingly steep with radius, establishing that cooler phases of the circumgalactic medium are more centrally concentrated than warmer phases, with the structure varying by central object type and host mass.

What carries the argument

Stacking technique applied to multiple absorption doublets to extract radial equivalent width profiles across temperature phases.

If this is right

  • Emission-line galaxy halos display a sharp radial transition from cool to warm gas.
  • Quasar halos maintain a more uniform mix of phases, consistent with regulation by AGN feedback.
  • Cold gas traced by Ca II remains tightly confined to the inner halo in low-redshift systems.
  • The radial scaling of absorption strength for cool gas is set mainly by host stellar mass.

Where Pith is reading between the lines

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

  • The observed mass dependence implies that heating becomes more efficient inside massive halos, reducing the amount of cool gas available at larger radii.
  • If the stratification persists across cosmic time, it would affect how quickly galaxies can accrete fresh material from the surrounding reservoir.
  • Higher-resolution spectra could separate velocity components and test whether the radial trends arise from distinct kinematic structures.

Load-bearing premise

The ions cleanly mark distinct temperature phases whose ionization states and covering fractions stay constant enough with radius that they do not create the observed profile differences on their own.

What would settle it

A measurement in which the radial equivalent width slopes are statistically identical for Ca II, Mg II, and C IV regardless of the temperature each ion is expected to trace.

Figures

Figures reproduced from arXiv: 2606.04793 by Cheqiu Lyu, Dongdong Shi, Enci Wang, Haoran Yu, Haowen Guan, Haoyi Zhang, Kai Wang, Weiwen Kong, Yuxuan Zhang, Zeyu Chen.

Figure 1
Figure 1. Figure 1: Stellar mass–redshift distributions of the foreground galaxy samples used for the absorption-line stacking analysis. The left panel shows ELGs, and the right panel shows BGSs. Gray points represent the full parent samples, with black contours indicating the 1-σ and 2-σ density levels. Colored contours denote the subsamples with spectral coverage suitable for different absorption-line tracers: Mg ii (blue; … view at source ↗
Figure 2
Figure 2. Figure 2: The radial profiles and corresponding stacked spectra of representative CGM absorption lines around ELG host galaxies selected from the left panel of [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Same as [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Left panel: radial dependence of the rest-frame equivalent-width ratios relative to Mg ii as a function of impact parameter. The symbols denote ratios derived from Gaussian fits to the stacked spectra: pink squares (ELGs) and circles (foreground quasar host galaxies) represent C iv/Mg ii, while green triangles indicate Ca ii/Mg ii in BGS halos (filled for the K transition and open for the H transition). Th… view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: dependence of the radial power-law index α on stellar mass. Symbols distinguish different ionic species (pink: C iv; blue: Mg ii; green: Ca ii K) and host galaxy populations (squares: ELGs; triangles: BGSs). The curves represent the best-fit linear trends, shown as dashed lines for ELGs and dash-dotted lines for BGSs. Right panel: redshift evolution of the radial power-law index α as a function… view at source ↗
read the original abstract

We present a systematic study of the multiphase circumgalactic medium (CGM) around galaxies and quasars, traced by Ca II $\lambda\lambda3934,3969$, Mg II $\lambda\lambda2796,2803$, and C IV $\lambda\lambda1548,1550$, using the Year 1 dataset from the Dark Energy Spectroscopic Instrument. These three doublets trace CGM gas across a range of temperatures, from cold to warm phases, and we employ a stacking technique to measure the corresponding absorption signals using background sources. We show that CGM structure is strongly phase-dependent: ions tracing progressively cooler gas exhibit increasingly steep radial profiles in equivalent width ($W_i$). These trends are broadly consistent with predictions from cosmological simulations, supporting a phase-stratified CGM in which cooler gas is more centrally concentrated. Specifically, halos of emission-line galaxies exhibit a strong radial transition from cool to warm gas, whereas halos of quasars show a more uniform distribution, likely regulated by active galactic nuclei feedback; in contrast, the cold gas traced by Ca II in low-redshift galaxies is tightly confined to inner regions. We further demonstrate that the radial scaling $W_i \propto D^{\alpha}$ is primarily set by host stellar mass, particularly for the cool-phase medium, suggesting efficient heating processes in massive halos. By jointly leveraging multiple absorption tracers from observations and simulations, we map the CGM from cold to warm phases and place new constraints on the baryon cycle governing galaxy evolution.

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

1 major / 0 minor

Summary. The paper claims that stacked equivalent-width radial profiles (W_i) from Ca II, Mg II, and C IV absorption in DESI Year 1 data around emission-line galaxies and quasars become progressively steeper for ions tracing cooler gas. These trends are reported as consistent with cosmological simulations and interpreted as evidence for a phase-stratified CGM in which cooler phases are more centrally concentrated, with additional dependence on host type (ELG vs. quasar) and stellar mass.

Significance. If the central mapping from observed W_i(D) slopes to phase-dependent concentration holds after controlling for ionization and covering-fraction effects, the result would supply one of the first large-sample, multi-ion observational constraints on radial phase structure in the CGM, directly testable against simulations and relevant to baryon-cycle models.

major comments (1)
  1. Abstract and central claim: the inference that steeper W_i profiles for Ca II/Mg II versus C IV demonstrate that cooler gas is more centrally concentrated rests on the assumption that each ion’s ionization fraction and the absorber covering fraction remain sufficiently constant (or vary in a non-degenerate way) across the sampled impact-parameter range. No test that isolates this degeneracy—e.g., by holding total hydrogen column fixed while varying only the ionization parameter—is described, leaving open the possibility that radial gradients in density, temperature, or UV field alone could produce the observed slopes without requiring phase-dependent spatial distributions.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address the major comment below and indicate where we will revise the text.

read point-by-point responses

  1. Referee: Abstract and central claim: the inference that steeper W_i profiles for Ca II/Mg II versus C IV demonstrate that cooler gas is more centrally concentrated rests on the assumption that each ion’s ionization fraction and the absorber covering fraction remain sufficiently constant (or vary in a non-degenerate way) across the sampled impact-parameter range. No test that isolates this degeneracy—e.g., by holding total hydrogen column fixed while varying only the ionization parameter—is described, leaving open the possibility that radial gradients in density, temperature, or UV field alone could produce the observed slopes without requiring phase-dependent spatial distributions.

    Authors: We acknowledge that the interpretation of steeper W_i profiles for cooler ions as evidence of central concentration assumes that ionization fractions and covering fractions do not introduce a dominant degeneracy. Our analysis relies on the differential behavior across ions with distinct ionization potentials, combined with direct comparison to cosmological simulations that self-consistently compute ionization states from local gas properties and the UV background. These simulations produce analogous radial trends driven by phase-dependent spatial distributions rather than ionization gradients alone. We did not include an explicit test holding total hydrogen column fixed (as stacked equivalent widths do not yield per-absorber N_H), but we will add a dedicated paragraph in the discussion section quantifying the potential contribution of radial ionization variations using the simulation outputs. This will make the assumptions and their robustness more explicit. revision: partial

Circularity Check

0 steps flagged

No circularity: direct observational stacking compared to external simulations

full rationale

The paper measures equivalent widths via stacking of DESI spectra for Ca II, Mg II, and C IV, reports radial trends W_i(D), and notes consistency with external cosmological simulations. No derivation step reduces by construction to a fitted parameter within the paper, no self-citation is load-bearing for the central claim, and no ansatz or uniqueness theorem is imported from the authors' prior work. The mapping from ion to phase is presented as an interpretive assumption rather than a mathematical identity, and the radial profiles are reported as measured quantities, not predictions derived from the same data.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Based solely on the abstract; no explicit free parameters, axioms, or invented entities are stated. The radial scaling W_i ∝ D^α is described as set by stellar mass, but no fitting details are given.

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Works this paper leans on

113 extracted references · 110 canonical work pages · 11 internal anchors

  1. [1]

    Aird, J., & Coil, A. L. 2021, MNRAS, 502, 5962, doi: 10.1093/mnras/stab312

    work page doi:10.1093/mnras/stab312 2021

  2. [2]

    2021, MNRAS, 504, 65, doi: 10.1093/mnras/stab871

    Anand, A., Nelson, D., & Kauffmann, G. 2021, MNRAS, 504, 65, doi: 10.1093/mnras/stab871

    work page doi:10.1093/mnras/stab871 2021

  3. [3]

    , keywords =

    Anand, A., Guy, J., Bailey, S., et al. 2024, AJ, 168, 124, doi: 10.3847/1538-3881/ad60c2 Angl´ es-Alc´ azar, D., Faucher-Gigu` ere, C.-A., Kereˇ s, D., et al. 2017, MNRAS, 470, 4698, doi: 10.1093/mnras/stx1517

    work page doi:10.3847/1538-3881/ad60c2 2024

  4. [4]

    1986, A&A, 169, 1

    Bergeron, J., & Stasi´ nska, G. 1986, A&A, 169, 1

    1986

  5. [5]

    2019, A&A, 622, A103, doi: 10.1051/0004-6361/201834156 24

    Boquien, M., Burgarella, D., Roehlly, Y., et al. 2019, A&A, 622, A103, doi: 10.1051/0004-6361/201834156

    work page internal anchor Pith review doi:10.1051/0004-6361/201834156 2019

  6. [6]

    K., et al

    Bordoloi, R., Tumlinson, J., Werk, J. K., et al. 2014, ApJ, 796, 136, doi: 10.1088/0004-637X/796/2/136

    work page doi:10.1088/0004-637x/796/2/136 2014

  7. [7]

    M., Fender, R

    Bower, R. G., Benson, A. J., Malbon, R., et al. 2006, MNRAS, 370, 645, doi: 10.1111/j.1365-2966.2006.10519.x

    work page doi:10.1111/j.1365-2966.2006.10519.x 2006

  8. [8]

    and Norman, Michael L

    Bryan, G. L., & Norman, M. L. 1998, ApJ, 495, 80, doi: 10.1086/305262

    work page internal anchor Pith review doi:10.1086/305262 1998

  9. [9]

    2012, Advances in Astronomy, 2012, 853701, doi: 10.1155/2012/853701

    Cappelluti, N., Allevato, V., & Finoguenov, A. 2012, Advances in Astronomy, 2012, 853701, doi: 10.1155/2012/853701

    work page doi:10.1155/2012/853701 2012

  10. [10]

    , keywords =

    Chaussidon, E., Y` eche, C., Palanque-Delabrouille, N., et al. 2023, ApJ, 944, 107, doi: 10.3847/1538-4357/acb3c2

    work page doi:10.3847/1538-4357/acb3c2 2023

  11. [11]

    A two-phase model of galaxy formation: IV. Seeding and growing supermassive black holes in dark matter halos

    Chen, Y., Mo, H., & Wang, H. 2025a, arXiv e-prints, arXiv:2509.03283, doi: 10.48550/arXiv.2509.03283

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.03283

  12. [12]

    2025b, ApJL, 988, L39, doi: 10.3847/2041-8213/ade545 —

    Chen, Z., Wang, E., Zou, H., et al. 2025b, ApJL, 988, L39, doi: 10.3847/2041-8213/ade545 —. 2025c, ApJ, 981, 81, doi: 10.3847/1538-4357/ada942

    work page doi:10.3847/2041-8213/ade545 2041

  13. [13]

    Cook, A. W. S., van de Voort, F., Pakmor, R., & Grand, R. J. J. 2025, MNRAS, 543, 1224, doi: 10.1093/mnras/staf1537

    work page doi:10.1093/mnras/staf1537 2025

  14. [14]

    , keywords =

    Croton, D. J., Springel, V., White, S. D. M., et al. 2006, MNRAS, 365, 11, doi: 10.1111/j.1365-2966.2005.09675.x

    work page doi:10.1111/j.1365-2966.2005.09675.x 2006

  15. [15]

    S., Schlegel, D

    Dawson, K. S., Schlegel, D. J., Ahn, C. P., et al. 2013, AJ, 145, 10, doi: 10.1088/0004-6256/145/1/10

    work page internal anchor Pith review doi:10.1088/0004-6256/145/1/10 2013

  16. [16]

    arXiv , author =:2102.08383 , journal =

    DeFelippis, D., Bouch´ e, N. F., Genel, S., et al. 2021, ApJ, 923, 56, doi: 10.3847/1538-4357/ac2cbf

    work page doi:10.3847/1538-4357/ac2cbf 2021

  17. [17]

    M., Fender, R

    Dekel, A., & Birnboim, Y. 2006, MNRAS, 368, 2, doi: 10.1111/j.1365-2966.2006.10145.x

    work page doi:10.1111/j.1365-2966.2006.10145.x 2006

  18. [18]

    Data Release 1 of the Dark Energy Spectroscopic Instrument

    Dekel, A., Birnboim, Y., Engel, G., et al. 2009, Nature, 457, 451, doi: 10.1038/nature07648 DESI Collaboration, Adame, A. G., Aguilar, J., et al. 2024, AJ, 168, 58, doi: 10.3847/1538-3881/ad3217 DESI Collaboration, Karim, M. A., Adame, A. G., et al. 2025, arXiv e-prints, arXiv:2503.14745, doi: 10.48550/arXiv.2503.14745

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature07648 2009

  19. [19]

    S., Sharma, P., et al

    Dutta, A., Bisht, M. S., Sharma, P., et al. 2024, MNRAS, 531, 5117, doi: 10.1093/mnras/stae977

    work page doi:10.1093/mnras/stae977 2024

  20. [20]

    2021, MNRAS, 508, 4573, doi: 10.1093/mnras/stab2752 Euclid Collaboration, Scaramella, R., Amiaux, J., et al

    Dutta, R., Fumagalli, M., Fossati, M., et al. 2021, MNRAS, 508, 4573, doi: 10.1093/mnras/stab2752 Euclid Collaboration, Scaramella, R., Amiaux, J., et al. 2022, A&A, 662, A112, doi: 10.1051/0004-6361/202141938 Euclid Collaboration, Mellier, Y., Abdurro’uf, et al. 2024, arXiv e-prints, arXiv:2405.13491, doi: 10.48550/arXiv.2405.13491 Faucher-Gigu` ere, C.-...

    work page doi:10.1093/mnras/stab2752 2021

  21. [21]

    B., Oppenheimer, B

    Ford, A. B., Oppenheimer, B. D., Dav´ e, R., et al. 2013, MNRAS, 432, 89, doi: 10.1093/mnras/stt393

    work page doi:10.1093/mnras/stt393 2013

  22. [22]

    B., Werk, J

    Ford, A. B., Werk, J. K., Dav´ e, R., et al. 2016, MNRAS, 459, 1745, doi: 10.1093/mnras/stw595

    work page doi:10.1093/mnras/stw595 2016

  23. [23]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306, doi: 10.1086/670067

    work page doi:10.1086/670067 2013

  24. [24]

    2023, MNRAS, 524, 3474, doi: 10.1093/mnras/stad2087 16Kong et al

    Galbiati, M., Fumagalli, M., Fossati, M., et al. 2023, MNRAS, 524, 3474, doi: 10.1093/mnras/stad2087 16Kong et al. 9.5 10.0 10.5 11.0 11.5 logM* [M ] 2.25 2.00 1.75 1.50 1.25 1.00 0.75 0.50 D/Rvir-based D-based 1.4 1.6 1.8 2.0 z Figure B.The same as Figure 6, but additionally showingαobtained usingD/R vir binning (open symbols). The halo-scaled radial bin...

    work page doi:10.1093/mnras/stad2087 2023

  25. [25]

    L., Werk, J

    Garza, S. L., Werk, J. K., Berg, T. A. M., et al. 2025, ApJL, 978, L12, doi: 10.3847/2041-8213/ad9c69

    work page doi:10.3847/2041-8213/ad9c69 2025

  26. [26]

    2012, ApJ, 746, 94, doi: 10.1088/0004-637X/746/1/94

    Gaspari, M., Ruszkowski, M., & Sharma, P. 2012, ApJ, 746, 94, doi: 10.1088/0004-637X/746/1/94

    work page doi:10.1088/0004-637x/746/1/94 2012

  27. [27]

    C., Froning, C

    Green, J. C., Froning, C. S., Osterman, S., et al. 2012, ApJ, 744, 60, doi: 10.1088/0004-637X/744/1/6010.1086/141956

    work page doi:10.1088/0004-637x/744/1/6010.1086/141956 2012

  28. [28]

    2018, PyQSOFit: Python code to fit the spectrum of quasars, Astrophysics Source Code Library, record ascl:1809.008

    Guo, H., Shen, Y., & Wang, S. 2018, PyQSOFit: Python code to fit the spectrum of quasars, Astrophysics Source Code Library, record ascl:1809.008. http://ascl.net/1809.008

    2018

  29. [29]

    2020, MNRAS, 494, 3581, doi: 10.1093/mnras/staa902

    Hafen, Z., Faucher-Gigu` ere, C.-A., Angl´ es-Alc´ azar, D., et al. 2020, MNRAS, 494, 3581, doi: 10.1093/mnras/staa902

    work page doi:10.1093/mnras/staa902 2020

  30. [30]

    2022, MNRAS, 514, 5056, doi: 10.1093/mnras/stac1603

    Hafen, Z., Stern, J., Bullock, J., et al. 2022, MNRAS, 514, 5056, doi: 10.1093/mnras/stac1603

    work page doi:10.1093/mnras/stac1603 2022

  31. [31]

    , keywords =

    Hahn, C., Wilson, M. J., Ruiz-Macias, O., et al. 2023, AJ, 165, 253, doi: 10.3847/1538-3881/accff8

    work page doi:10.3847/1538-3881/accff8 2023

  32. [32]

    2026, ApJ, 998, 261, doi: 10.3847/1538-4357/ae1b88

    Stern, J. 2026, ApJ, 998, 261, doi: 10.3847/1538-4357/ae1b88

    work page doi:10.3847/1538-4357/ae1b88 2026

  33. [33]

    2025, ApJL, 986, L24, doi: 10.3847/2041-8213/addfd9

    Jia, C., Wang, E., Lyu, C., et al. 2025, ApJL, 986, L24, doi: 10.3847/2041-8213/addfd9

    work page doi:10.3847/2041-8213/addfd9 2025

  34. [34]

    2025, ApJ, 994, 220, doi: 10.3847/1538-4357/ae17c1

    Jiang, H., Wang, E., Wang, K., Ma, C., & Kong, X. 2025, ApJ, 994, 220, doi: 10.3847/1538-4357/ae17c1

    work page doi:10.3847/1538-4357/ae17c1 2025

  35. [35]

    G., Muzahid, S., Churchill, C

    Kacprzak, G. G., Muzahid, S., Churchill, C. W., Nielsen, N. M., & Charlton, J. C. 2015, ApJ, 815, 22, doi: 10.1088/0004-637X/815/1/22

    work page doi:10.1088/0004-637x/815/1/22 2015

  36. [36]

    G., Oppenheimer, B., Nielsen, N., et al

    Kacprzak, G. G., Oppenheimer, B., Nielsen, N., et al. 2025, PASA, 42, e128, doi: 10.1017/pasa.2025.10091

    work page doi:10.1017/pasa.2025.10091 2025

  37. [37]

    2024, NIST Atomic Spectra Database (version 5.12), Online, doi: 10.18434/T4W30F

    Kramida, A., Ralchenko, Y., Reader, J., et al. 2024, NIST Atomic Spectra Database (version 5.12), Online, doi: 10.18434/T4W30F

    work page doi:10.18434/t4w30f 2024

  38. [38]

    2020, ApJ, 897, 97, doi: 10.3847/1538-4357/ab989a

    Lan, T.-W. 2020, ApJ, 897, 97, doi: 10.3847/1538-4357/ab989a

    work page doi:10.3847/1538-4357/ab989a 2020

  39. [39]

    2017, ApJ, 850, 156, doi: 10.3847/1538-4357/aa93eb

    Lan, T.-W., & Fukugita, M. 2017, ApJ, 850, 156, doi: 10.3847/1538-4357/aa93eb

    work page doi:10.3847/1538-4357/aa93eb 2017

  40. [40]

    2018, ApJ, 866, 36, doi: 10.3847/1538-4357/aadc08

    Lan, T.-W., & Mo, H. 2018, ApJ, 866, 36, doi: 10.3847/1538-4357/aadc08

    work page doi:10.3847/1538-4357/aadc08 2018

  41. [41]

    X., Aguilar, J., et al

    Lan, T.-W., Prochaska, J. X., Aguilar, J., et al. 2025, arXiv e-prints, arXiv:2511.03195, doi: 10.48550/arXiv.2511.03195

    work page doi:10.48550/arxiv.2511.03195 2025

  42. [42]

    W., & Mykytyn, D

    Lang, D., Hogg, D. W., & Mykytyn, D. 2016, The Tractor: Probabilistic astronomical source detection and measurement, Astrophysics Source Code Library, record ascl:1604.008

    2016

  43. [43]

    The Dark Energy Spectroscopic Instrument (DESI)

    Levi, M., Allen, L. E., Raichoor, A., et al. 2019, in Bulletin of the American Astronomical Society, Vol. 51, 57, doi: 10.48550/arXiv.1907.10688

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1907.10688 2019

  44. [44]

    2021, MNRAS, 500, 1038, doi: 10.1093/mnras/staa3322

    Li, F., Rahman, M., Murray, N., et al. 2021, MNRAS, 500, 1038, doi: 10.1093/mnras/staa3322

    work page doi:10.1093/mnras/staa3322 2021

  45. [45]

    2025, MNRAS, 543, 1878, doi: 10.1093/mnras/staf1594

    Li, H., Chen, Y., Wang, H., & Mo, H. 2025, MNRAS, 543, 1878, doi: 10.1093/mnras/staf1594

    work page doi:10.1093/mnras/staf1594 2025

  46. [46]

    J., Kravtsov, A

    Liang, C. J., Kravtsov, A. V., & Agertz, O. 2016, MNRAS, 458, 1164, doi: 10.1093/mnras/stw375

    work page doi:10.1093/mnras/stw375 2016

  47. [47]

    J., & Remming, I

    Liang, C. J., & Remming, I. 2020, MNRAS, 491, 5056, doi: 10.1093/mnras/stz3403

    work page doi:10.1093/mnras/stz3403 2020

  48. [48]

    2019, ApJ, 877, 4, doi: 10.3847/1538-4357/ab184e

    Schaye, J. 2019, ApJ, 877, 4, doi: 10.3847/1538-4357/ab184e

    work page doi:10.3847/1538-4357/ab184e 2019

  49. [49]

    2025, ApJL, 981, L6, doi: 10.3847/2041-8213/adb4ed

    Lyu, C., Wang, E., Zhang, H., et al. 2025, ApJL, 981, L6, doi: 10.3847/2041-8213/adb4ed

    work page doi:10.3847/2041-8213/adb4ed 2025

  50. [50]

    2026, ApJL, 1000, L3, doi: 10.3847/2041-8213/ae48ee

    Lyu, C., Yu, H., Wang, E., et al. 2026, ApJL, 1000, L3, doi: 10.3847/2041-8213/ae48ee

    work page doi:10.3847/2041-8213/ae48ee 2026

  51. [51]

    2024, ApJL, 971, L14, doi: 10.3847/2041-8213/ad675f

    Ma, C., Wang, K., Wang, E., et al. 2024, ApJL, 971, L14, doi: 10.3847/2041-8213/ad675f

    work page doi:10.3847/2041-8213/ad675f 2024

  52. [52]

    P., O’Leary, R., & Madigan, A.-M

    McCourt, M., Oh, S. P., O’Leary, R., & Madigan, A.-M. 2018, MNRAS, 473, 5407, doi: 10.1093/mnras/stx2687 17 M´ enard, B., Wild, V., Nestor, D., et al. 2011, Monthly Notices of the Royal Astronomical Society, 417, 801

    work page doi:10.1093/mnras/stx2687 2018

  53. [53]

    , keywords =

    Miller, T. N., Doel, P., Gutierrez, G., et al. 2024, AJ, 168, 95, doi: 10.3847/1538-3881/ad45fe

    work page doi:10.3847/1538-3881/ad45fe 2024

  54. [54]

    2024, MNRAS, 532, 3808, doi: 10.1093/mnras/stae1727

    Mo, H., Chen, Y., & Wang, H. 2024, MNRAS, 532, 3808, doi: 10.1093/mnras/stae1727

    work page doi:10.1093/mnras/stae1727 2024

  55. [55]

    2024, MNRAS, 532, 32, doi: 10.1093/mnras/stae1418

    Blomqvist, M. 2024, MNRAS, 532, 32, doi: 10.1093/mnras/stae1418

    work page doi:10.1093/mnras/stae1418 2024

  56. [56]

    P., Naab, T., & White, S

    Moster, B. P., Naab, T., & White, S. D. M. 2013, MNRAS, 428, 3121, doi: 10.1093/mnras/sts261

    work page internal anchor Pith review doi:10.1093/mnras/sts261 2013

  57. [57]

    , keywords =

    Myers, A. D., Moustakas, J., Bailey, S., et al. 2023, AJ, 165, 50, doi: 10.3847/1538-3881/aca5f9

    work page doi:10.3847/1538-3881/aca5f9 2023

  58. [58]

    D., et al

    Napolitano, L., Pandey, A., Myers, A. D., et al. 2023, AJ, 166, 99, doi: 10.3847/1538-3881/ace62c

    work page doi:10.3847/1538-3881/ace62c 2023

  59. [59]

    doi:10.1093/mnras/staa2419 , eprint =

    Nelson, D., Sharma, P., Pillepich, A., et al. 2020, MNRAS, 498, 2391, doi: 10.1093/mnras/staa2419

    work page doi:10.1093/mnras/staa2419 2020

  60. [60]

    The Synthetic Absorption Line Spectral Almanac (SALSA)

    Nelson, D., Peroux, C., Richter, P., et al. 2025, arXiv e-prints, arXiv:2510.19904, doi: 10.48550/arXiv.2510.19904

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2510.19904 2025

  61. [61]

    V., Lan, T.-W., Prochaska, J

    Ng, Y. V., Lan, T.-W., Prochaska, J. X., et al. 2025, ApJ, 993, 92, doi: 10.3847/1538-4357/ae0613

    work page doi:10.3847/1538-4357/ae0613 2025

  62. [62]

    L., et al

    Olivares, V., Salom´ e, P., Hamer, S. L., et al. 2022, A&A, 666, A94, doi: 10.1051/0004-6361/202142475

    work page doi:10.1051/0004-6361/202142475 2022

  63. [63]

    M., Fender, R

    Oppenheimer, B. D., & Dav´ e, R. 2006, MNRAS, 373, 1265, doi: 10.1111/j.1365-2966.2006.10989.x

    work page doi:10.1111/j.1365-2966.2006.10989.x 2006

  64. [64]

    D., Schaye, J., Crain, R

    Oppenheimer, B. D., Schaye, J., Crain, R. A., Werk, J. K., & Richings, A. J. 2018, MNRAS, 481, 835, doi: 10.1093/mnras/sty2281

    work page doi:10.1093/mnras/sty2281 2018

  65. [65]

    2024, arXiv e-prints, arXiv:2411.07988, doi: 10.48550/arXiv.2411.07988 P´ eroux, C., Nelson, D., van de Voort, F., et al

    Peroux, C., & Nelson, D. 2024, arXiv e-prints, arXiv:2411.07988, doi: 10.48550/arXiv.2411.07988 P´ eroux, C., Nelson, D., van de Voort, F., et al. 2020, MNRAS, 499, 2462, doi: 10.1093/mnras/staa2888

    work page doi:10.48550/arxiv.2411.07988 2024

  66. [66]

    M., Mortonson, M

    Pieri, M. M., Mortonson, M. J., Frank, S., et al. 2014, MNRAS, 441, 1718, doi: 10.1093/mnras/stu577

    work page doi:10.1093/mnras/stu577 2014

  67. [67]

    First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time , volume=

    Pillepich, A., Nelson, D., Springel, V., et al. 2019, MNRAS, 490, 3196, doi: 10.1093/mnras/stz2338 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2016, A&A, 594, A13, doi: 10.1051/0004-6361/201525830

    work page doi:10.1093/mnras/stz2338 2019

  68. [68]

    , keywords =

    Poppett, C., Tyas, L., Aguilar, J., et al. 2024, AJ, 168, 245, doi: 10.3847/1538-3881/ad76a4

    work page doi:10.3847/1538-3881/ad76a4 2024

  69. [69]

    Research Notes of the American Astronomical Society , keywords =

    Raichoor, A., Eisenstein, D. J., Karim, T., et al. 2020, Research Notes of the American Astronomical Society, 4, 180, doi: 10.3847/2515-5172/abc078

    work page doi:10.3847/2515-5172/abc078 2020

  70. [70]

    , keywords =

    Raichoor, A., Moustakas, J., Newman, J. A., et al. 2023, AJ, 165, 126, doi: 10.3847/1538-3881/acb213

    work page doi:10.3847/1538-3881/acb213 2023

  71. [71]

    J., & Ostriker, J

    Rees, M. J., & Ostriker, J. P. 1977, MNRAS, 179, 541, doi: 10.1093/mnras/179.4.541

    work page doi:10.1093/mnras/179.4.541 1977

  72. [72]

    Murphy, M. T. 2011, A&A, 528, A12, doi: 10.1051/0004-6361/201015566

    work page doi:10.1051/0004-6361/201015566 2011

  73. [73]

    Research Notes of the American Astronomical Society , keywords =

    Ruiz-Macias, O., Zarrouk, P., Cole, S., et al. 2020, Research Notes of the American Astronomical Society, 4, 187, doi: 10.3847/2515-5172/abc25a

    work page doi:10.3847/2515-5172/abc25a 2020

  74. [74]

    L., Rennehan, D., et al

    Saeedzadeh, V., Jung, S. L., Rennehan, D., et al. 2023, MNRAS, 525, 5677, doi: 10.1093/mnras/stad2637

    work page doi:10.1093/mnras/stad2637 2023

  75. [75]

    C., Wakker, B

    Sameer, Charlton, J. C., Wakker, B. P., et al. 2024, MNRAS, 530, 3827, doi: 10.1093/mnras/stae962

    work page doi:10.1093/mnras/stae962 2024

  76. [76]

    N., Werk, J

    Sanchez, N. N., Werk, J. K., Tremmel, M., et al. 2019, ApJ, 882, 8, doi: 10.3847/1538-4357/ab3045

    work page doi:10.3847/1538-4357/ab3045 2019

  77. [77]

    A., Bower, R

    Schaye, J., Crain, R. A., Bower, R. G., et al. 2015, MNRAS, 446, 521, doi: 10.1093/mnras/stu2058

    work page doi:10.1093/mnras/stu2058 2015

  78. [78]

    , keywords =

    Schlafly, E. F., Kirkby, D., Schlegel, D. J., et al. 2023, AJ, 166, 259, doi: 10.3847/1538-3881/ad0832

    work page doi:10.3847/1538-3881/ad0832 2023

  79. [79]

    J., Ferraro, S., Aldering, G., et al

    Schlegel, D. J., Ferraro, S., Aldering, G., et al. 2022, arXiv e-prints, arXiv:2209.03585, doi: 10.48550/arXiv.2209.03585

    work page doi:10.48550/arxiv.2209.03585 2022

  80. [80]

    2025, MNRAS, 541, 2471, doi: 10.1093/mnras/staf1066

    Shah, H., van de Voort, F., Seta, A., & Federrath, C. 2025, MNRAS, 541, 2471, doi: 10.1093/mnras/staf1066

    work page doi:10.1093/mnras/staf1066 2025

Showing first 80 references.