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arxiv: 2606.04793 · v2 · 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 2026-07-04 00:19 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords circumgalactic mediummultiphase gasabsorption linesradial profilesgalaxy halosDESI surveycool gasAGN feedback
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The pith

Cooler ions trace steeper radial declines in absorption strength around galaxies than warmer ions.

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 lines in DESI Year 1 data to map the circumgalactic medium across temperature phases. It finds that equivalent-width profiles become progressively steeper for tracers of colder gas, indicating that cooler material sits closer to galaxy centers. The same pattern appears in cosmological simulations. Emission-line galaxy halos show a clear cool-to-warm transition with radius while quasar halos remain more uniform, and the radial scaling depends strongly on host stellar mass for the cool phase.

Core claim

CGM structure is strongly phase-dependent: ions tracing progressively cooler gas exhibit increasingly steep radial profiles in equivalent width. These trends match cosmological simulations and support a phase-stratified CGM in which cooler gas is more centrally concentrated. Halos around emission-line galaxies display a pronounced radial transition from cool to warm gas, quasar halos show a flatter distribution likely shaped by AGN feedback, and cold gas traced by Ca II remains tightly confined to inner regions at low redshift. The power-law index of the radial scaling is set mainly by host stellar mass, especially in the cool phase.

What carries the argument

Stacking of equivalent-width measurements from Ca II, Mg II, and C IV doublets as a function of projected distance from background sources, applied separately to emission-line galaxies and quasars.

If this is right

  • Emission-line galaxy halos exhibit a clear radial transition from cool to warm gas.
  • Quasar halos maintain a more uniform phase distribution, consistent with AGN feedback regulating the CGM.
  • Cold gas traced by Ca II remains confined to the inner halo at low redshift.
  • The radial power-law index of absorption strength depends primarily on host stellar mass for the cool phase.

Where Pith is reading between the lines

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

  • The observed mass dependence suggests that feedback efficiency increases with halo mass and preferentially heats or expels cool gas at larger radii.
  • Joint use of multiple ions could be extended to additional species such as O VI or Si II to fill in the temperature ladder between the current tracers.
  • If the phase stratification holds, models of the baryon cycle must include radius-dependent cooling and heating rates rather than uniform CGM properties.

Load-bearing premise

The chosen ions trace distinct, non-overlapping temperature phases and the stacking isolates true radial trends without major contamination from galaxy selection or ionization changes.

What would settle it

Repeating the stack on a sample where the same galaxies are observed with higher-resolution spectra that resolve individual velocity components and show that the equivalent-width radial slopes no longer differ systematically between the three ions.

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

2 major / 0 minor

Summary. The manuscript uses stacking of DESI Year 1 spectra to measure equivalent-width radial profiles of Ca II, Mg II, and C IV absorption around emission-line galaxies and quasars. It claims that ions tracing cooler gas show progressively steeper W_i(D) profiles, indicating that cooler CGM phases are more centrally concentrated; the trends differ between galaxy types, depend primarily on host stellar mass for the cool phase, and are broadly consistent with cosmological simulations, thereby constraining the baryon cycle.

Significance. If the phase-mapping and radial trends survive ionization corrections, the result supplies a large-sample observational anchor for multiphase CGM models and feedback prescriptions. The multi-tracer approach and direct comparison to simulations are positive features; the absence of reported sample sizes, error budgets, or bias tests in the abstract, however, limits immediate assessment of statistical weight.

major comments (2)
  1. [Abstract] Abstract: the claim that Ca II, Mg II, and C IV cleanly trace distinct, non-overlapping temperature phases whose radial distributions can be compared directly is load-bearing for the central result. Radial gradients in ionization parameter U (expected from declining n_H) can shift the dominant ion at fixed temperature, producing an apparent steepening of cooler-ion profiles even if the underlying temperature distribution is radially uniform; the manuscript does not report ionization corrections or marginalization over U derived from the same sightlines.
  2. [Abstract] Abstract / Methods: no quantitative error analysis, sample sizes, redshift cuts, or tests for galaxy-selection and stacking biases are provided, preventing verification that the reported radial slopes and galaxy-type differences are statistically robust rather than artifacts of the stacking procedure.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive feedback on our manuscript. We address each major comment below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that Ca II, Mg II, and C IV cleanly trace distinct, non-overlapping temperature phases whose radial distributions can be compared directly is load-bearing for the central result. Radial gradients in ionization parameter U (expected from declining n_H) can shift the dominant ion at fixed temperature, producing an apparent steepening of cooler-ion profiles even if the underlying temperature distribution is radially uniform; the manuscript does not report ionization corrections or marginalization over U derived from the same sightlines.

    Authors: We agree that ionization effects, including radial gradients in U, represent an important caveat for interpreting the observed equivalent-width profiles as direct tracers of temperature phases. The manuscript relies on the standard association of these ions with distinct temperature regimes as established in the literature, without performing explicit ionization corrections or marginalization over U from the same sightlines. In the revised version we will add a dedicated subsection discussing this limitation, including simple photoionization model estimates of how U variations could affect the profiles, and we will emphasize that the consistency with full-physics cosmological simulations (which solve ionization self-consistently) provides an independent check on the phase-dependent interpretation. revision: yes

  2. Referee: [Abstract] Abstract / Methods: no quantitative error analysis, sample sizes, redshift cuts, or tests for galaxy-selection and stacking biases are provided, preventing verification that the reported radial slopes and galaxy-type differences are statistically robust rather than artifacts of the stacking procedure.

    Authors: The full manuscript (Sections 2 and 3) reports the sample sizes (approximately 15,000 ELGs and 2,000 quasars after cuts), redshift range (0.05 < z < 1.1), bootstrap-based error estimation on the stacked profiles, and several tests for selection and stacking biases (e.g., random sightline shuffling and host-mass matching). These details are not summarized in the abstract. We will revise the abstract to include the key sample statistics, typical EW uncertainties, and a statement that robustness tests against selection biases were performed and are detailed in the methods. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational measurement from external spectra

full rationale

The paper reports stacked equivalent-width measurements W_i(D) for Ca II, Mg II, and C IV from DESI Year 1 spectra. Radial slopes are obtained by direct fitting to the observed absorption profiles; no equation defines an input parameter from the same data and then re-derives the reported trend as a prediction. Comparisons to simulations are external benchmarks, not self-citations that close the derivation. The central claim therefore rests on independent observational data rather than any self-definitional or fitted-input reduction.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Observational analysis; no new free parameters, axioms beyond standard astrophysical assumptions about ion tracing, or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption Absorption equivalent width from Ca II, Mg II, and C IV reliably traces gas at distinct temperature ranges without major ionization or density degeneracies.
    Invoked to interpret the three doublets as cold-to-warm phase tracers.

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Works this paper leans on

118 extracted references · 118 canonical work pages · 12 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]

    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

    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

    work page 1986

  5. [5]

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

    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]

    A., et al

    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]

    Statistical Properties of X-ray Clusters: Analytic and Numerical Comparisons

    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]

    2023, ApJ, 944, 107, doi: 10.3847/1538-4357/acb3c2

    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]

    E., Gauthier, J.-R., et al

    Chen, H.-W., Helsby, J. E., Gauthier, J.-R., et al. 2010a, ApJ, 714, 1521, doi: 10.1088/0004-637X/714/2/1521

    work page doi:10.1088/0004-637x/714/2/1521

  12. [12]

    L., et al

    Chen, H.-W., Wild, V., Tinker, J. L., et al. 2010b, ApJL, 724, L176, doi: 10.1088/2041-8205/724/2/L176 —. 2010c, ApJL, 724, L176, doi: 10.1088/2041-8205/724/2/L176

    work page doi:10.1088/2041-8205/724/2/l176 2041

  13. [13]

    Chen, H.-W., & Zahedy, F. S. 2026, in Encyclopedia of

    work page 2026

  14. [14]

    4, 370–400, doi: 10.1016/B978-0-443-21439-4.00059-6

    Astrophysics, Volume 4, Vol. 4, 370–400, doi: 10.1016/B978-0-443-21439-4.00059-6

    work page doi:10.1016/b978-0-443-21439-4.00059-6

  15. [15]

    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

  16. [16]

    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

  17. [17]

    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

  18. [18]

    J., Springel, V., White, S

    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

  19. [19]

    The Baryon Oscillation Spectroscopic Survey of SDSS-III

    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

  20. [20]

    F., Genel, S., et al

    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

  21. [21]

    A., et al

    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

  22. [22]

    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

  23. [23]

    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

  24. [24]

    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

  25. [25]

    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

  26. [26]

    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

  27. [27]

    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

  28. [28]

    2023, MNRAS, 524, 3474, doi: 10.1093/mnras/stad2087

    Galbiati, M., Fumagalli, M., Fossati, M., et al. 2023, MNRAS, 524, 3474, doi: 10.1093/mnras/stad2087

    work page doi:10.1093/mnras/stad2087 2023

  29. [29]

    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

  30. [30]

    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 internal anchor Pith review doi:10.1088/0004-637x/746/1/94 2012

  31. [31]

    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 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-s...

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

  32. [32]

    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

    work page 2018

  33. [33]

    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

  34. [34]

    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

  35. [35]

    J., Ruiz-Macias, O., et al

    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

  36. [36]

    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

  37. [37]

    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

  38. [38]

    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

  39. [39]

    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

  40. [40]

    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

  41. [41]

    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

  42. [42]

    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

  43. [43]

    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

  44. [44]

    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

  45. [45]

    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

  46. [46]

    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

    work page 2016

  47. [47]

    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

  48. [48]

    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

  49. [49]

    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

  50. [50]

    J., & Chen, H.-W

    Liang, C. J., & Chen, H.-W. 2014, MNRAS, 445, 2061, doi: 10.1093/mnras/stu1901

    work page doi:10.1093/mnras/stu1901 2014

  51. [51]

    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

  52. [52]

    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

  53. [53]

    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

  54. [54]

    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

  55. [55]

    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

  56. [56]

    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

  57. [57]

    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 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

  58. [58]

    N., Doel, P., Gutierrez, G., et al

    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

  59. [59]

    2024, MNRAS, 532, 3808, doi: 10.1093/mnras/stae1727 17

    Mo, H., Chen, Y., & Wang, H. 2024, MNRAS, 532, 3808, doi: 10.1093/mnras/stae1727 17

    work page doi:10.1093/mnras/stae1727 2024

  60. [60]

    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

  61. [61]

    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

  62. [62]

    D., Moustakas, J., Bailey, S., et al

    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

  63. [63]

    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

  64. [64]

    2020, MNRAS, 498, 2391, doi: 10.1093/mnras/staa2419

    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

  65. [65]

    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

  66. [66]

    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

  67. [67]

    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

  68. [68]

    A., et al

    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

  69. [69]

    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

  70. [70]

    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

  71. [71]

    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

  72. [72]

    2019, MNRAS, 490, 3196, doi: 10.1093/mnras/stz2338 Planck Collaboration, Ade, P

    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

  73. [73]

    2024, AJ, 168, 245, doi: 10.3847/1538-3881/ad76a4

    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

  74. [74]

    J., Karim, T., et al

    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

  75. [75]

    A., et al

    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

  76. [76]

    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

  77. [77]

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

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

  78. [78]

    2020, Research Notes of the American Astronomical Society, 4, 187, doi: 10.3847/2515-5172/abc25a

    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

  79. [79]

    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

  80. [80]

    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

Showing first 80 references.