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arxiv: 2606.24802 · v1 · pith:Z6OP4WHLnew · submitted 2026-06-23 · 🌌 astro-ph.GA

Opening new parameter space windows on galaxy/AGN co-evolution with SKA radio continuum surveys

Isabella Prandoni , Mark T. Sargent , Matteo Bonato , Dharam V. Lal , Mahdiyar Mousavi-Sadr , Masoumeh Ghasemi-Nodehi , Nicholas Seymour , Fatemeh S. Tabatabaei
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Gianfranco De Zotti Ivano Baronchelli Elisabetta Liuzzo Nicola Marchili Marcella Massardi Rosita Paladino
This is my paper

Pith reviewed 2026-06-25 23:22 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy evolutionAGN co-evolutionradio continuum surveysSKAOmulti-frequency imagingextragalactic surveyssurvey synergies
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The pith

SKAO radio continuum reference surveys will advance galaxy and AGN co-evolution studies by revealing physical properties of sources and calibrating sparser radio observations.

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

The paper provides an overview of science enabled by the SKAO for understanding how galaxies and active galactic nuclei evolve together. It highlights planned radio continuum reference surveys, including tiered extragalactic designs at specific frequencies and complementary deep multi-frequency imaging over selected fields. These efforts are positioned to supply detailed information on emitting sources that current facilities cannot easily obtain. The multi-frequency component is presented as essential for calibrating observables from surveys that have less complete radio spectral coverage. The discussion also covers pathways to use the observatory from its early stages through to full baseline performance and notes synergies with other major facilities expected in the 2030s.

Core claim

The central claim is that SKAO radio continuum reference surveys, structured as tiered wedding-cake designs plus targeted multi-frequency imaging, will open new parameter space for galaxy/AGN co-evolution research by delivering key physical properties of radio-emitting sources and by providing calibration anchors for observables measured in surveys with sparser spectral coverage.

What carries the argument

Tiered radio continuum reference surveys combined with complementary multi-frequency imaging over extragalactic fields, which together supply spectral information needed to determine source physical properties.

If this is right

  • Radio data will constrain the physical mechanisms linking star formation and AGN activity across cosmic time.
  • Observables from single-frequency or sparsely sampled radio surveys will become more reliably interpreted through calibration against the multi-frequency reference data.
  • Joint coverage of extragalactic fields with other 2030s facilities will create high-value legacy datasets for multi-wavelength co-evolution studies.
  • Survey strategies can be adjusted from initial SKAO operations through to full baseline to maximize early science return.

Where Pith is reading between the lines

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

  • The emphasis on multi-frequency calibration could shift planning priorities for other radio arrays toward ensuring at least partial overlap with SKAO fields.
  • If the reference surveys succeed, they may enable population studies that test whether current models of AGN feedback over- or under-predict radio source counts at faint levels.
  • The described synergies suggest that coordinated field selection with optical and X-ray facilities could become a standard requirement for maximizing return on large radio survey investments.

Load-bearing premise

The SKAO will reach its planned baseline capabilities and that the described multi-frequency imaging over extragalactic fields will be obtained.

What would settle it

If the SKAO reference surveys fail to achieve the planned depths, frequency coverage, or area coverage, the expected gains in physical characterization and calibration for co-evolution studies would not materialize.

Figures

Figures reproduced from arXiv: 2606.24802 by Dharam V. Lal, Elisabetta Liuzzo, Fatemeh S. Tabatabaei, Gianfranco De Zotti, Isabella Prandoni, Ivano Baronchelli, Mahdiyar Mousavi-Sadr, Marcella Massardi, Mark T. Sargent, Masoumeh Ghasemi-Nodehi, Matteo Bonato, Nicholas Seymour, Nicola Marchili, Rosita Paladino.

Figure 2
Figure 2. Figure 2: Upper panel: Sky density of AGN populations in the T-RECS simulation (Bonaldi et al., 2023), as a function of their predicted median flux density at 1.4 GHz. Horizontal error bars span the interquartile range (25-75%) of the fluxes tabulated in the T-RECS catalog for a given AGN sub-sample. AGN populations are binned by redshift (and drawn from a ∼1 Gyr interval centred on the reference redshifts listed in… view at source ↗
Figure 3
Figure 3. Figure 3: As in [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: SKA-Mid Band 2 and Band 5 reference surveys, as defined in [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Top row: LOFAR images obtained at various angular resolutions and integration times. From left to right: resolution improvement from the standard 6′′ provided by NL baselines, to 1.5, 0.7 and 0.4′′ when including international stations, with different weightings. With international stations one can de-blend the source into three different components. Bottom: J-band Euclid image from the Quick Release 1 (Q1… view at source ↗
Figure 6
Figure 6. Figure 6: Panels 1–3: Band-by-band observing times (𝑡obs), angular resolution (FWHMbm) and sky coverage (Asky) for a roughly beam-matched, multi-band AA4 survey with flat spectral response (red lines) or 𝜈 −0.7 scaling (blue). All three quantities are normalised to B2 (scales on left-hand y-axis). For beam sizes and sky areas, which are independent of observing time, an absolute scale is shown on the right. SKA-Low … view at source ↗
Figure 7
Figure 7. Figure 7: Integration time per sq. degree as a function of angular resolution from the SKAO Sensitivity Calculator (Decl. = −45◦ , Elevation = 45◦ ). Different colors refer to different frequencies: Band 1/0.8 GHz; Band 2/1.4 GHz; Band 5a/6.6 GHz; Band 5b/11.9 GHz. Different lines refer to different tiers: Wide (solid); Deep (dotted); Ultra-deep (dot-dashed). Thick (thin) lines refer to AA4 (AA∗ ). Band 1 and 2 (Ban… view at source ↗
Figure 8
Figure 8. Figure 8: Cumulative number density predictions for different classes of radio continuum sources from T-RECS (Bonaldi et al. 2023), compared with WST capabilities. left-hand y-axis – number of sources in a 1 deg2 field; right-hand y-axis – number of sources in the WST field of view. The black horizontal lines indicate the number of fibres available for WST (30k for low resolution spectroscopy). The filled histograms… view at source ↗
Figure 9
Figure 9. Figure 9: Simulated ALMA WSU spectral profile of a molecular transition (e.g. CO 𝐽=3–2). The model consists of a narrow core component (rotating disk; Gaussian FWHM ∼90 km s−1 ; peak ∼3 mJy) plus a broad, blueshifted outflow wing (peak ∼0.3 mJy; width ∼200 km s−1 ). The black trace shows the noisy realization (added Gaussian RMS = 0.04 mJy); the dotted horizontal line marks a conceptual 5𝜎 threshold for the chosen i… view at source ↗
read the original abstract

In this chapter we provide an overview of the science enabled by the SKAO, focusing on galaxy/AGN co-evolution studies. In particular we discuss a number of radio continuum `reference' surveys with the SKAO, highlighting the role they can play in advancing this research field with respect to the pre-SKAO era. Alongside well-explored scenarios for wedding cake-like, tiered extragalactic surveys at specific frequencies, we also address the scope for complementary efforts to obtain deep multi-frequency imaging over parts of (an) extragalactic field(s). In addition to providing key information on the physical properties of the emitting sources, such multi-frequency imaging will make important contributions to the calibration of observables from surveys with sparser radio spectral coverage. In this context, we explore possible pathways that can fully exploit the SKAO from initial (AA*) to baseline capabilities (AA4). Finally, we highlight observational synergies with other major facilities -- for wide field and targeted follow-up science -- that will be operational in the 2030s, and for which joint coverage of extragalactic fields will generate significant legacy value

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. The manuscript provides an overview of science enabled by the SKAO for galaxy/AGN co-evolution studies via radio continuum reference surveys. It covers tiered 'wedding cake' extragalactic surveys at specific frequencies, the value of complementary deep multi-frequency imaging over extragalactic fields for source physical properties and calibration of sparser-coverage observables, pathways to exploit the observatory from initial (AA*) to baseline (AA4) capabilities, and synergies with other 2030s facilities for legacy value.

Significance. If realized, the described surveys would supply physical-property constraints and calibration support that advance co-evolution studies beyond the pre-SKAO era. As a forward-looking synthesis rather than a source of new empirical results or derivations, the manuscript's primary contribution is to frame the observational strategy and its conditional scientific payoff.

minor comments (1)
  1. [Abstract] Abstract: the acronyms AA* and AA4 are introduced without definition or reference; a parenthetical gloss or citation to SKAO documentation would aid readers.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of our manuscript and their recommendation to accept. No major comments were raised.

Circularity Check

0 steps flagged

No significant circularity; overview of future surveys with no derivations or fitted predictions

full rationale

The manuscript is an overview chapter discussing planned SKAO reference surveys and their potential role in galaxy/AGN co-evolution studies. It contains no mathematical derivations, equations, fitted parameters, or predictions that could reduce to self-referential inputs. All claims are explicitly conditional on future observatory performance (AA4 capabilities and complementary multi-frequency imaging) and are scoped as forward-looking science cases rather than empirical results derived from the paper's own content. No self-citation chains, ansatzes, or uniqueness theorems are invoked as load-bearing elements. The central argument stands as self-contained planning discussion without internal reduction to its own assumptions.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is an overview paper with no mathematical derivations, new models, or empirical claims; no free parameters, axioms, or invented entities are introduced.

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Works this paper leans on

63 extracted references · 60 canonical work pages · 1 internal anchor

  1. [1]

    InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026

    J.Afonsoetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Afonso.1. H. S. B. Algera et al.ApJ, 903(2):139, Nov

    2026

  2. [2]

    doi: 10.3847/1538-4357/abb77a. H. S. B. Algera et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.3847/1538-4357/abb77a

  3. [3]

    ALMA Observatory

    arXiv search: Report number AASKAII/Algera.1. ALMA Observatory. ALMA WSU Factsheet and WSU Program docu- mentation.https://www.almaobservatory.org/en/alma-development/ alma-2030-wideband-sensitivity-upgrade/, 2024a. Accessed 2024-2025. ALMA Observatory. ALMA WSU science case summaries.https://www.almaobservatory. org/en/alma-development/alma-2030-wideband...

    2030

  4. [4]

    doi: 10.1117/12.3018093. O. S. Bait et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1117/12.3018093

  5. [5]

    doi: 10.1111/j.1365-2966.2007.11937.x. P. N. Best et al.MNRAS, 523(2):1729–1755, Aug

    work page doi:10.1111/j.1365-2966.2007.11937.x 2007

  6. [6]

    doi: 10.1093/mnras/stad1308. A. Bonaldi et al.MNRAS, 524(1):993–1007, Sept

    work page doi:10.1093/mnras/stad1308

  7. [7]

    doi: 10.1093/mnras/stad1913. M. Bonato et al.MNRAS, 469(2):1912–1923, Aug

    work page doi:10.1093/mnras/stad1913 1912

  8. [8]

    doi: 10.1093/mnras/stx974. R. G. Bower et al.MNRAS, 370(2):645–655, Aug

    work page doi:10.1093/mnras/stx974

  9. [9]

    Hydrodynamic models , author =

    doi: 10.1111/j.1365-2966.2006.10519.x. R.Braunetal. SKA1Science(Level0)Requirements. TechnicalReportSKA-TEL-SKO-0000007 Rev 2, SKA Organisation,

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

  10. [10]

    arXiv e-prints , keywords =

    URLhttps://www.skao.int/sites/default/files/ documents/d1_v2-SKA-TEL-SKO-0000007-02-SKA1_Science_Requirements.pdf. R.Braunetal.arXive-prints,art.arXiv:1912.12699,Dec.2019. doi: 10.48550/arXiv.1912.12699. J.Carpenteretal. TheALMA2030WidebandSensitivityUpgrade,Nov2022. ALMAMemo621. J. J. Condon.Annual Review of Astronomy and Astrophysics, 30:575–611,

    work page doi:10.48550/arxiv.1912.12699 1912

  11. [11]

    29 A new radio window on galaxy/AGN co-evolution I

    doi: 10.1146/ annurev.aa.30.090192.003043. 29 A new radio window on galaxy/AGN co-evolution I. Prandoni, M. Sargent, M. Bonato et al. R. T. Coogan et al.MNRAS, 479(1):703–729, Sept

    arXiv

  12. [12]

    doi: 10.1093/mnras/sty1446. R. T. Coogan et al.MNRAS, 525(3):3413–3438, Nov

    work page doi:10.1093/mnras/sty1446

  13. [13]

    doi: 10.1093/mnras/stad2469. L. Costantin et al.ApJ, 946(2):71, Apr

    work page doi:10.1093/mnras/stad2469

  14. [14]

    doi: 10.3847/1538-4357/acb926. D. J. Croton.MNRAS, 369(4):1808–1812, July

    work page doi:10.3847/1538-4357/acb926

  15. [15]

    doi: 10.1111/j.1365-2966.2006.10429.x. E. Daddi et al.ApJL, 846(2):L31, Sept

    work page doi:10.1111/j.1365-2966.2006.10429.x 2006

  16. [16]

    doi: 10.3847/2041-8213/aa8808. I. Delvecchio et al.A&A, 602:A3, June

    work page doi:10.3847/2041-8213/aa8808 2041

  17. [17]

    C.Dickinsonetal.NewAstronomyReviews,80:1–28,May2018.doi: 10.1016/j.newar.2018.04.001

    doi: 10.1051/0004-6361/201629367. C.Dickinsonetal.NewAstronomyReviews,80:1–28,May2018.doi: 10.1016/j.newar.2018.04.001. S. Duivenvoorden et al.MNRAS, 462(1):277–289, Oct

    work page doi:10.1051/0004-6361/201629367 2018

  18. [18]

    doi: 10.1093/mnras/stw1466. J. S. Dunlop et al.MNRAS, 466(1):861–883, Apr

    work page doi:10.1093/mnras/stw1466

  19. [19]

    doi: 10.1093/mnras/stw3088. G. Erfanianfar et al.MNRAS, 455(3):2839–2851, Jan

    work page doi:10.1093/mnras/stw3088

  20. [20]

    Euclid Collaboration et al.A&A,

    doi: 10.1093/mnras/stv2485. Euclid Collaboration et al.A&A,

    work page doi:10.1093/mnras/stv2485

  21. [21]

    URLhttps: //doi.org/10.1051/0004-6361/202554610

    doi: 10.1051/0004-6361/202554610. URLhttps: //doi.org/10.1051/0004-6361/202554610. M. Gaspari et al.ApJ, 884(2):169, Oct

    work page doi:10.1051/0004-6361/202554610

  22. [22]

    M.J.Hardcastleetal

    doi: 10.3847/1538-4357/ab3c5d. M.J.Hardcastleetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Hardcastle.1. H. Hassani et al.MNRAS, 510(1):11–31, Feb

    work page doi:10.3847/1538-4357/ab3c5d 2026

  23. [23]

    doi: 10.1093/mnras/stab3202. T. M. Heckman.ApJ, 268:628–631, May

    work page doi:10.1093/mnras/stab3202

  24. [24]

    doi: 10.1086/160984. T. M. Heckman and P. N. Best.ARA&A, 52:589–660, Aug

    work page doi:10.1086/160984

  25. [25]

    2025, PASA, 42, e071, doi: 10.1017/pasa.2025.10042

    doi: 10.1017/pasa.2025.10042. P.F.Hopkinsetal.MNRAS,427(2):968–978,Dec.2012. doi: 10.1111/j.1365-2966.2012.21981.x. M. Jarvis et al. InMeerKAT Science: On the Pathway to the SKA, page 6, Jan

    work page doi:10.1017/pasa.2025.10042 2025

  26. [26]

    doi: 10.22323/1.277.0006. E. F. Jiménez-Andrade et al.A&A, 625:A114, May

    work page doi:10.22323/1.277.0006

  27. [27]

    doi: 10.1051/0004-6361/201935178. E. F. Jiménez-Andrade et al.ApJ, 972(1):89, Sept

    work page doi:10.1051/0004-6361/201935178

  28. [28]

    doi: 10.3847/1538-4357/ad5b5c. W. C. Keel.ApJ, 282:75–84, July

    work page doi:10.3847/1538-4357/ad5b5c

  29. [29]

    doi: 10.1086/162177. R. Kondapally et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1086/162177

  30. [30]

    doi: 10.1088/0004-6256/149/2/61. D. V. Lal, P. Shastri, and D. C. Gabuzda.ApJ, 731(1):68, Apr

    work page doi:10.1088/0004-6256/149/2/61

  31. [32]

    doi: 10.3847/1538-4357/adf6dc. S. K. Leslie et al.ApJ, 899(1):58, Aug

    work page doi:10.3847/1538-4357/adf6dc

  32. [33]

    K., Schinnerer, E., Liu, D., et al

    doi: 10.3847/1538-4357/aba044. F.M.Maccagnietal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Maccagni.1. C. Macfarlane et al.MNRAS, 506(4):5888–5907, Oct

    work page doi:10.3847/1538-4357/aba044 2026

  33. [34]

    doi: 10.1093/mnras/stab1998. M. Magliocchetti.A&ARv, 30(1):6, Dec

    work page doi:10.1093/mnras/stab1998

  34. [35]

    doi: 10.1007/s00159-022-00142-1. M. Magliocchetti et al.MNRAS, 464(3):3271–3280, Jan

    work page doi:10.1007/s00159-022-00142-1

  35. [36]

    doi: 10.1093/mnras/stw2541. F. Mazoochi et al.ApJ, 997(1):31, Jan

    work page doi:10.1093/mnras/stw2541

  36. [37]

    doi: 10.3847/1538-4357/ae1b93. G. Mazzolari et al.A&A, 687:A120, July

    work page doi:10.3847/1538-4357/ae1b93

  37. [38]

    L.McKayetal.arXive-prints,art.arXiv:2509.11846,Sept.2025.doi: 10.48550/arXiv.2509.11846

    doi: 10.1051/0004-6361/202348072. L.McKayetal.arXive-prints,art.arXiv:2509.11846,Sept.2025.doi: 10.48550/arXiv.2509.11846. 30 A new radio window on galaxy/AGN co-evolution I. Prandoni, M. Sargent, M. Bonato et al. J. Moldon et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202348072 2025

  38. [39]

    doi: 10.1051/0004-6361/201834559. C. G. Mundell, P. Ferruit, N. Nagar, and A. S. Wilson.ApJ, 703(1):802–815, Sept

    work page doi:10.1051/0004-6361/201834559

  39. [40]

    E.Murphyetal

    doi: 10.1088/0004-637X/703/1/802. E.Murphyetal. InAdvancingAstrophysicswiththeSquareKilometreArray(AASKA14),page85, Apr

    work page doi:10.1088/0004-637x/703/1/802

  40. [41]

    doi: 10.22323/1.215.0085. E. J. Murphy et al.The Astrophysical Journal, 737(2):67, Aug

    work page doi:10.22323/1.215.0085

  41. [42]

    doi: 10.1088/0004-637X/ 737/2/67. T. W. B. Muxlow et al.MNRAS, 495(1):1188–1208, June

    work page doi:10.1088/0004-637x/

  42. [43]

    doi: 10.1093/mnras/staa1279. N. M. Nagar, H. Falcke, A. S. Wilson, and J. S. Ulvestad.A&A, 392:53–82, Sept

    work page doi:10.1093/mnras/staa1279

  43. [44]

    doi: 10.1051/0004-6361:20020874. N. M. Nagar, H. Falcke, and A. S. Wilson.A&A, 435(2):521–543, May

    work page doi:10.1051/0004-6361:20020874

  44. [45]

    doi: 10.3847/1538-4357/aaf38a. R. P. Norris et al.PASA, 28(3):215–248, Aug

    work page doi:10.3847/1538-4357/aaf38a

  45. [46]

    doi: 10.1071/AS11021. R. P. Norris et al.PASA, 38:e046, Sept

    work page doi:10.1071/as11021

  46. [47]

    doi: 10.1017/pasa.2021.42. F. Panessa et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1017/pasa.2021.42 2021

  47. [48]

    doi: 10.22323/1.215.0067. I. Prandoni et al.The Messenger, 193:14–19, Sep

    work page doi:10.22323/1.215.0067

  48. [49]

    doi: 10.18727/0722-6691/5361. J. F. Radcliffe et al.A&A, 649:L9, May 2021a. doi: 10.1051/0004-6361/202140791. J. F. Radcliffe et al.A&A, 649:A27, May 2021b. doi: 10.1051/0004-6361/202038591. J. Rhodes et al.ApJSS, 233(2):21, Dec

    work page doi:10.18727/0722-6691/5361

  49. [50]

    doi: 10.3847/1538-4365/aa96b0. J. Sabater et al.A&A, 622:A17, Feb

    work page doi:10.3847/1538-4365/aa96b0

  50. [51]

    doi: 10.1051/0004-6361/201833883. M. Shuntov et al.A&A, 664:A61, Aug

    work page doi:10.1051/0004-6361/201833883

  51. [52]

    doi: 10.1051/0004-6361/202243136. J. Silk and G. A. Mamon.Research in Astronomy and Astrophysics, 12(8):917–946, Aug

    work page doi:10.1051/0004-6361/202243136

  52. [53]

    doi: 10.1088/1674-4527/12/8/004. R. S. Somerville and R. Davé.ARA&A, 53:51–113, Aug

    work page doi:10.1088/1674-4527/12/8/004

  53. [54]

    doi: 10.1146/ annurev-astro-082812-140951. F. Tabatabaei et al. In F. Tabatabaei, B. Barbuy, and Y.-S. Ting, editors,Early Disk-Galaxy FormationfromJWSTtotheMilkyWay,volume377ofIAUSymposium,pages43–47,Jan.2024. doi: 10.1017/S1743921323001680. F. Tabatabaei et al.ApJ, 989(1):44, Aug

    work page doi:10.1017/s1743921323001680 2024

  54. [55]

    doi: 10.3847/1538-4357/ade233. F. S. Tabatabaei et al.ApJ, 836(2):185, Feb

    work page doi:10.3847/1538-4357/ade233

  55. [56]

    doi: 10.3847/1538-4357/836/2/185. F. S. Tabatabaei, P. Minguez, M. A. Prieto, and J. A. Fernández-Ontiveros.Nature Astronomy, 2: 83–89, Nov

    work page doi:10.3847/1538-4357/836/2/185

  56. [57]

    F.S.Tabatabaeietal

    doi: 10.1038/s41550-017-0298-7. F.S.Tabatabaeietal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Tabatabaei.1. L. J. Tacconi, R. Genzel, and A. Sternberg.ARA&A, 58:157–203, Aug

    work page doi:10.1038/s41550-017-0298-7 2026

  57. [58]

    31 A new radio window on galaxy/AGN co-evolution I

    doi: 10.3847/1538-4357/ab32e7. 31 A new radio window on galaxy/AGN co-evolution I. Prandoni, M. Sargent, M. Bonato et al. C. M. Urry and P. Padovani.PASP, 107:803, Sept

    work page doi:10.3847/1538-4357/ab32e7

  58. [59]

    doi: 10.1086/133630. S. D. van Dyk and L. C. Ho. In J. A. Zensus, G. B. Taylor, and J. M. Wrobel, editors,IAU Colloquium 164: Radio Emission from Galactic and Extragalactic Compact Sources, volume 144 ofAstronomical Society of the Pacific Conference Series, page 205, Jan

    work page internal anchor Pith review doi:10.1086/133630

  59. [60]

    doi: 10.1093/mnras/stx2486. J. R. Weaver et al.A&A, 677:A184, Sept

    work page doi:10.1093/mnras/stx2486

  60. [61]

    doi: 10.1051/0004-6361/202245581. R. H. Wechsler and J. L. Tinker.ARA&A, 56:435–487, Sept

    work page doi:10.1051/0004-6361/202245581

  61. [62]

    doi: 10.1093/mnras/stac2140. G. Zasowski et al.arXiv e-prints, art. arXiv:2505.10574, May

    work page doi:10.1093/mnras/stac2140

  62. [63]

    doi: 10.48550/arXiv.2505. 10574. S. Zhang, B. Liu, and V. Bromm.MNRAS, 528(1):180–197, Feb

    work page doi:10.48550/arxiv.2505

  63. [64]

    doi: 10.1093/mnras/ stad3986. 32

    work page doi:10.1093/mnras/