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arxiv: 2606.30307 · v1 · pith:Z5NCO7C2new · submitted 2026-06-29 · 🌌 astro-ph.GA

The SKA-VLBI Perspective on Radio-Quiet AGN

Francesca Panessa , Tao An , James Petley , Ailing Wang , Ranieri Diego Baldi , Ehud Behar , Emmanuel Bempong-Manful , Gabriele Bruni
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Ning Chang Sina Chen Lang Cui Filippo D'Ammando Marcello Giroletti Magdalena Kunert-Bajraszewska Sibasish Laha Ari Laor Ian McHardy Eileen Meyer Monica Orienti Miguel P\'erez-Torres Isabella Prandoni Claudio Ricci David R. A. Williams-Baldwin Zsolt Paragi
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Pith reviewed 2026-06-30 04:47 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords radio-quiet AGNSKAVLBIAGN feedbackradio emissionsupermassive black holesaccretiongalaxy evolution
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The pith

SKA-MID phased into global VLBI arrays will enable the first population-level census of radio-quiet AGN nuclei.

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

Radio-quiet AGN dominate the population yet their radio emission arises from several overlapping mechanisms that operate from host-galaxy scales down to the vicinity of the central black hole. The paper sets out how the Square Kilometre Array, once combined with VLBI, supplies the frequency coverage, sensitivity and angular resolution needed to isolate these contributions. A sympathetic reader would care because separating star formation, winds, free-free gas, weak jets and coronal emission bears directly on the accretion-ejection problem and on AGN feedback in galaxy evolution. At full AA4 deployment the phased SKA-MID is projected to reach sub-milliarcsecond imaging and microJy levels between 0.35 and 15 GHz, turning radio-quiet nuclei into a statistically accessible sample for the first time. Earlier array configurations are expected to permit initial studies of the brightest nearby objects.

Core claim

At the full AA4 deployment, the SKA-MID phased into global VLBI arrays will deliver sub-milliarcsecond imaging and μJy sensitivity over 0.35--15 GHz, enabling the first population-level census of radio-quiet AGN nuclei. Flux, spectral and polarisation monitoring will constrain dynamics and environmental coupling while mapping nuclear regions on sub-pc to kpc scales will disentangle compact cores from host emission and resolve the diversity of radio activity across accretion regimes and jet powers from the local Universe to cosmic dawn.

What carries the argument

SKA-MID phased into global VLBI arrays, which supplies the combination of wide frequency range, high sensitivity and sub-milliarcsecond resolution required to separate nuclear from host-galaxy emission.

If this is right

  • Flux, spectral and polarisation monitoring will constrain the dynamics and environmental coupling of the emission processes.
  • Mapping on sub-pc to kpc scales will separate compact cores from host-galaxy emission.
  • The diversity of radio activity across accretion regimes and jet powers can be resolved from the local Universe to cosmic dawn.
  • Earlier AA* operations will support pilot studies of the brightest nearby systems.

Where Pith is reading between the lines

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

  • Population statistics from such observations could be compared directly with multi-wavelength accretion indicators to test models of black-hole growth.
  • The same data sets might quantify how radio-quiet AGN contribute to the energy budget assumed in galaxy-formation simulations.
  • Practical limits on wide-field VLBI calibration could reduce the effective yield of faint sources below the nominal microJy threshold.

Load-bearing premise

The planned SKA-MID sensitivity, resolution and frequency coverage will be achieved on schedule and the resulting data will suffice to disentangle the listed radio-emission processes without major confusion from host-galaxy emission or calibration limits.

What would settle it

A sample of radio-quiet AGN observed at the projected μJy sensitivity and sub-milliarcsecond resolution in which the different emission components remain indistinguishable from one another would falsify the central claim.

Figures

Figures reproduced from arXiv: 2606.30307 by Ailing Wang, Ari Laor, Claudio Ricci, David R. A. Williams-Baldwin, Ehud Behar, Eileen Meyer, Emmanuel Bempong-Manful, Filippo D'Ammando, Francesca Panessa, Gabriele Bruni, Ian McHardy, Isabella Prandoni, James Petley, Lang Cui, Magdalena Kunert-Bajraszewska, Marcello Giroletti, Miguel P\'erez-Torres, Monica Orienti, Ning Chang, Ranieri Diego Baldi, Sibasish Laha, Sina Chen, Tao An, Zsolt Paragi.

Figure 1
Figure 1. Figure 1: VLBI evidence that a subset of RQ AGN launches relativistic jets, illustrated by Mrk 110 as a representative case (taken from Wang et al. (2025)). (a) VLBA 6.2 GHz images on 2021 December 31 (colour scale) and 2024 February 2 (contours), revealing a core offset of ∼ 1.6 mas. The image centre is set at the 2021 December peak position (R.A. 09:25:12.84781, Dec. +52:17:10.3862). (b) International LOFAR image … view at source ↗
read the original abstract

The accretion-ejection mechanism in Active Galactic Nuclei (AGN) remains a central open problem in astrophysics, tied to the role of AGN feedback in galaxy formation and evolution. Radio-quiet AGN dominate the observed AGN population. Lacking luminous jets, their radio emission traces a rich set of processes spanning the host galaxy kpc scales down to the vicinity of the supermassive black hole: star formation, AGN-driven winds and shocks, free-free emission from photo-ionized gas, low-power jets, and coronal activity close to the inner accretion disk. The Square Kilometre Array (SKA) will probe these processes across a wide frequency range with unprecedented sensitivity, wide-field survey capability, and, critically, high-resolution VLBI imaging. Flux, spectral, and polarization monitoring will constrain dynamics and environmental coupling, while mapping nuclear regions on sub-pc to kpc scales will disentangle compact cores from host emission, resolving the diversity of radio activity across accretion regimes and jet powers from the local Universe to the cosmic dawn. At the full AA4 deployment, the SKA-MID phased into global VLBI arrays will deliver sub-milliarcsecond imaging and $\mu$Jy sensitivity over 0.35--15\,GHz, enabling the first population-level census of radio-quiet AGN nuclei. Earlier AA$\ast$ operations will support pilot studies of the brightest nearby systems.

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 is a perspective article outlining the scientific potential of SKA-MID phased into global VLBI arrays for radio-quiet AGN studies. It reviews emission processes (star formation, winds, free-free, weak jets, coronal activity) across scales and argues that at full AA4 deployment the array will achieve sub-milliarcsecond resolution and μJy sensitivity from 0.35-15 GHz, enabling the first population-level census of radio-quiet AGN nuclei; earlier AA* operations are noted for pilot studies.

Significance. If the projected performance is realized, the perspective usefully synthesizes the case for high-resolution, wide-frequency VLBI observations to address accretion-ejection and feedback questions in the dominant AGN population. It correctly enumerates the relevant physical processes and ties them to SKA design goals, providing a forward-looking roadmap that could guide observing strategies.

major comments (1)
  1. [Abstract] Abstract (final sentence): The claim that SKA-MID VLBI 'will deliver sub-milliarcsecond imaging and μJy sensitivity over 0.35--15 GHz, enabling the first population-level census of radio-quiet AGN nuclei' is presented without quantitative support such as expected source counts, detection thresholds, or assessment of confusion from host-galaxy emission. This assumption is load-bearing for the central conclusion.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive assessment of the perspective's scope and for the constructive comment on the abstract. We address the point below and will incorporate revisions to strengthen the quantitative basis for the central claim.

read point-by-point responses

  1. Referee: [Abstract] Abstract (final sentence): The claim that SKA-MID VLBI 'will deliver sub-milliarcsecond imaging and μJy sensitivity over 0.35--15 GHz, enabling the first population-level census of radio-quiet AGN nuclei' is presented without quantitative support such as expected source counts, detection thresholds, or assessment of confusion from host-galaxy emission. This assumption is load-bearing for the central conclusion.

    Authors: We agree this is a valid criticism: the abstract statement is forward-looking and would be strengthened by explicit quantitative grounding. As a perspective article the manuscript synthesizes existing literature rather than presenting new calculations, but we will revise by (i) adding order-of-magnitude source-count estimates extrapolated from current surveys (e.g., FIRST, NVSS, and VLASS) to SKA-MID VLBI sensitivities at 0.35–15 GHz, (ii) tabulating expected detection thresholds using the published SKA-MID system-equivalent flux density and integration-time scaling, and (iii) including a brief discussion of host-galaxy confusion limits based on typical kpc-scale radio surface-brightness distributions. These additions will be placed in a new short subsection and referenced from the abstract. The revised text will retain the perspective tone while making the load-bearing claim quantitatively defensible. revision: yes

Circularity Check

0 steps flagged

No derivation chain; perspective paper on planned capabilities

full rationale

The manuscript is a forward-looking perspective article. It describes planned SKA-MID VLBI performance (sub-mas resolution, μJy sensitivity, 0.35-15 GHz) and lists target emission processes (star formation, winds, free-free, jets, coronal activity) without presenting equations, parameter fits, or any derivation that reduces to its own inputs. No self-citations are invoked to support a uniqueness theorem or ansatz. The central claim is a projection of instrument specifications rather than a calculated result, so no circularity is present.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a perspective paper with no mathematical derivations, data fits, or new physical postulates; the ledger is therefore empty.

pith-pipeline@v0.9.1-grok · 5886 in / 1217 out tokens · 36910 ms · 2026-06-30T04:47:20.742468+00:00 · methodology

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Works this paper leans on

82 extracted references · 82 canonical work pages · 3 internal anchors

  1. [1]

    doi: 10.1111/j.1365-2966.2009.15829.x. D. M. Alexander et al.New Astron. Rev., 101:101733, Dec

    work page doi:10.1111/j.1365-2966.2009.15829.x 2009

  2. [2]

    doi: 10.1016/j.newar.2025. 101733. T. An.ApJL, 1004(1):L5, June

    work page doi:10.1016/j.newar.2025 2025

  3. [3]

    doi: 10.3847/2041-8213/ae6cde. T. An et al.Nature Communications, 11:143, Jan

    work page doi:10.3847/2041-8213/ae6cde 2041

  4. [4]

    doi: 10.1038/s41467-019-14093-2. T. An et al.MNRAS, 519(3):4047–4055, Mar

    work page doi:10.1038/s41467-019-14093-2

  5. [5]

    doi: 10.1093/mnras/stac3774. E. Bañados et al.ApJ, 804(2):118, May

    work page doi:10.1093/mnras/stac3774

  6. [6]

    13 AGN accretion and ejection Panessa et al

    doi: 10.1088/0004-637X/804/2/118. 13 AGN accretion and ejection Panessa et al. R. D. Baldi, E. Behar, A. Laor, and A. Horesh.MNRAS, 454(4):4277–4281, Dec

    work page doi:10.1088/0004-637x/804/2/118

  7. [7]

    doi: 10.1093/mnras/stv2284. R. D. Baldi et al.MNRAS, 508(2):2019–2038, Dec

    work page doi:10.1093/mnras/stv2284 2019

  8. [8]

    doi: 10.1093/mnras/stab2613. R. D. Baldi et al.MNRAS, 510(1):1043–1058, Feb

    work page doi:10.1093/mnras/stab2613

  9. [9]

    doi: 10.1093/mnras/stab3445. L. Barcos-Muñoz et al.ApJL, 853(2):L28, Feb

    work page doi:10.1093/mnras/stab3445

  10. [10]

    doi: 10.3847/2041-8213/aaa28d. E. Behar et al.MNRAS, 451(1):517–526, July

    work page doi:10.3847/2041-8213/aaa28d 2041

  11. [11]

    doi: 10.1093/mnras/stv988. E. Behar et al.MNRAS, 478(1):399–406, July

    work page doi:10.1093/mnras/stv988

  12. [12]

    doi: 10.1093/mnras/sty850. S. Belladitta et al.A&A, 635:L7, Mar

    work page doi:10.1093/mnras/sty850

  13. [13]

    doi: 10.1051/0004-6361/201937395. S. Belladitta et al.A&A, 669:A134, Jan

    work page doi:10.1051/0004-6361/201937395

  14. [14]

    doi: 10.1051/0004-6361/202243855. E. Bempong-Manful et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202243855

  15. [15]

    2012.21704.x

    arXiv search: Report number AASKAII/Bempong-Manful01. P.N.BestandT.M.Heckman.MNRAS,421(2):1569–1582,Apr.2012. doi: 10.1111/j.1365-2966. 2012.20414.x. P.N.Bestetal.MNRAS,523(2):1729–1755,2023. ISSN13652966. doi: 10.1093/mnras/stad1308. URLhttps://ui.adsabs.harvard.edu/abs/2023MNRAS.523.1729B/abstract. Pub- lisher: Oxford University Press. R. D. Blandford a...

    work page doi:10.1111/j.1365-2966 2012

  16. [16]

    doi: 10.1093/mnras/179.3

    work page doi:10.1093/mnras/179.3

  17. [17]

    doi: 10.1093/mnras/stad2289. S. Chen et al.ApJ, 979(2):241, Feb

    work page doi:10.1093/mnras/stad2289

  18. [18]

    doi: 10.3847/1538-4357/ada142. X. Cheng et al.ApJSS, 277(2):56, Apr

    work page doi:10.3847/1538-4357/ada142

  19. [19]

    doi: 10.3847/1538-4365/adba4c. J. J. Condon.ARA&A, 30:575–611, Jan

    work page doi:10.3847/1538-4365/adba4c

  20. [20]

    S.M.Croometal.MNRAS,399(4):1755–1772,Nov.2009

    doi: 10.1146/annurev.aa.30.090192.003043. S.M.Croometal.MNRAS,399(4):1755–1772,Nov.2009. doi: 10.1111/j.1365-2966.2009.15398. x. S. del Palacio et al.A&A, 701:A41, Sept

    work page doi:10.1146/annurev.aa.30.090192.003043 2009

  21. [21]

    doi: 10.1051/0004-6361/202554936. C.-A. Faucher-Giguère and E. Quataert.MNRAS, 425(1):605–622, Sept

    work page doi:10.1051/0004-6361/202554936

  22. [22]

    1365-2966.2012.21512.x

    doi: 10.1111/j. 1365-2966.2012.21512.x. S. Frey et al.A&A, 531:L5, July

    work page doi:10.1111/j 2012

  23. [23]

    doi: 10.1051/0004-6361/201117341. S. Frey et al.A&A, 681:L12, Jan

    work page doi:10.1051/0004-6361/201117341

  24. [24]

    doi: 10.1051/0004-6361/202348602. J. F. Gallimore, S. A. Baum, C. P. O’Dea, and A. Pedlar.ApJ, 458:136, Feb

    work page doi:10.1051/0004-6361/202348602

  25. [25]

    doi: 10.1086/504593. G. Ghisellini et al.MNRAS, 438(3):2694–2700, Mar

    work page doi:10.1086/504593

  26. [26]

    doi: 10.1093/mnras/stt2394. M. Giroletti and F. Panessa.ApJL, 706(2):L260–L264, Dec

    work page doi:10.1093/mnras/stt2394

  27. [27]

    doi: 10.1088/0004-637X/706/ 2/L260. K. Gültekin et al.MNRAS, 516(4):6123–6131, Nov

    work page doi:10.1088/0004-637x/706/

  28. [28]

    doi: 10.1093/mnras/stac2608. C. L. Hale et al.MNRAS, 536(3):2187–2211, Jan

    work page doi:10.1093/mnras/stac2608

  29. [29]

    , keywords =

    doi: 10.1093/mnras/stae2528. M.J.Hardcastleetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Hardcastle01. C.M.Harrison,D.M.Alexander,J.R.Mullaney,andA.M.Swinbank.MNRAS,441(4):3306–3347, July

    work page doi:10.1093/mnras/stae2528 2026

  30. [30]

    14 AGN accretion and ejection Panessa et al

    doi: 10.1093/mnras/stu515. 14 AGN accretion and ejection Panessa et al. C.M.Harrisonetal.NatureAstronomy,2:198–205,Feb.2018. doi: 10.1038/s41550-018-0403-6. T. M. Heckman and P. N. Best.ARA&A, 52:589–660, Aug

    work page doi:10.1093/mnras/stu515 2018

  31. [31]

    doi: 10.1088/0004-6256/144/4/105. L. Ighina et al.A&A, 647:L11, Mar

    work page doi:10.1088/0004-6256/144/4/105

  32. [32]

    doi: 10.1051/0004-6361/202140362. Y. Inoue and A. Doi.ApJ, 869(2):114, Dec

    work page doi:10.1051/0004-6361/202140362

  33. [33]

    doi: 10.3847/1538-4357/aaeb95. M. Janssen et al.A&A, 626:A75, June

    work page doi:10.3847/1538-4357/aaeb95

  34. [34]

    doi: 10.1051/0004-6361/201935181. M. E. Jarvis et al.MNRAS, 485(2):2710–2730, May

    work page doi:10.1051/0004-6361/201935181

  35. [35]

    doi: 10.1093/mnras/stz556. L. Jiang et al.ApJ, 656(2):680–690, Feb

    work page doi:10.1093/mnras/stz556

  36. [36]

    doi: 10.1086/510831. P. M. Keller et al.MNRAS, 528(4):5692–5702, Mar

    work page doi:10.1086/510831

  37. [37]

    doi: 10.1093/mnras/stae418. K. I. Kellermann et al.AJ, 98:1195, Oct

    work page doi:10.1093/mnras/stae418

  38. [38]

    doi: 10.1086/115207. P. Kharb and S. Silpa.Galaxies, 11(1):27, Feb

    work page doi:10.1086/115207

  39. [39]

    doi: 10.3390/galaxies11010027. P. Kharb et al.ApJ, 652(1):177–188, Nov

    work page doi:10.3390/galaxies11010027

  40. [40]

    doi: 10.1086/507945. J.-S. Kim et al.A&A, 690:A129, Oct

    work page doi:10.1086/507945

  41. [41]

    doi: 10.1051/0004-6361/202449663. R. Kondapally et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202449663

  42. [42]

    Y.Kudohetal

    doi: 10.1088/0004-6256/149/2/61. Y.Kudohetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Kudoh01. A.LaorandE.Behar.MNRAS,390(2):847–862,Oct.2008. doi: 10.1111/j.1365-2966.2008.13806. x. Y.Lietal. VLBIwithSKA:Possiblearraysandastrometricscience,

    work page doi:10.1088/0004-6256/149/2/61 2026

  43. [43]

    org/abs/2404.14663

    URLhttp://arxiv. org/abs/2404.14663. Y. Liu et al.ApJ, 929(1):69, Apr. 2022a. doi: 10.3847/1538-4357/ac5c50. Y. Liu et al.ApJL, 939(1):L5, Nov. 2022b. doi: 10.3847/2041-8213/ac98b2. Y. Liu et al.A&A, 685:A111, May

    work page doi:10.3847/1538-4357/ac5c50 2041

  44. [44]

    doi: 10.1051/0004-6361/202449394. A. P. Lobanov.A&A, 330:79–89, Feb

    work page doi:10.1051/0004-6361/202449394

  45. [45]

    doi: 10.48550/arXiv.astro-ph/9712132. P. Madau and M. Dickinson.ARA&A, 52:415–486, Aug

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9712132

  46. [46]

    doi: 10.1093/mnras/stt201. J. C. McKinney, A. Tchekhovskoy, and R. D. Blandford.MNRAS, 423(4):3083–3117, July

    work page doi:10.1093/mnras/stt201

  47. [47]

    Beutler, C

    doi: 10.1111/j.1365-2966.2012.21074.x. A.MerloniandS.Heinz.MNRAS,388(3):1011–1030,Aug.2008. doi: 10.1111/j.1365-2966.2008. 13472.x. A. Merloni, S. Heinz, and T. di Matteo.MNRAS, 345(4):1057–1076, Nov

    work page doi:10.1111/j.1365-2966.2012.21074.x 2012

  48. [48]

    1365-2966.2003.07017.x

    doi: 10.1046/j. 1365-2966.2003.07017.x. A. Mesinger, B. Greig, and E. Sobacchi.MNRAS, 459(3):2342–2353, July

    work page doi:10.1046/j 2003

  49. [49]

    doi: 10.1007/s00159-007-0008-z. B. Mingo et al.MNRAS, 511(3):3250–3271, Apr

    work page doi:10.1007/s00159-007-0008-z

  50. [50]

    doi: 10.1093/mnras/stac140. E. Momjian et al.ApJ, 861(2):86, July

    work page doi:10.1093/mnras/stac140

  51. [51]

    15 AGN accretion and ejection Panessa et al

    doi: 10.3847/1538-4357/aac76f. 15 AGN accretion and ejection Panessa et al. R. Morganti et al.A&A, 580:A1, Aug

    work page doi:10.3847/1538-4357/aac76f

  52. [52]

    doi: 10.1051/0004-6361/201525860. D. Mukherjee et al.MNRAS, 479(4):5544–5566, Oct

    work page internal anchor Pith review doi:10.1051/0004-6361/201525860

  53. [53]

    doi: 10.1093/mnras/sty1776. I. M. Mutie et al.MNRAS, 539(2):808–819, May

    work page internal anchor Pith review doi:10.1093/mnras/sty1776

  54. [54]

    doi: 10.1093/mnras/staf524. N. M. Nagar, H. Falcke, A. S. Wilson, and J. S. Ulvestad.A&A, 392:53–82, Sept

    work page doi:10.1093/mnras/staf524

  55. [55]

    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

  56. [56]

    doi: 10.1086/176343. K. Nyland et al.MNRAS, 458(2):2221–2268, May

    work page doi:10.1086/176343

  57. [57]

    doi: 10.1093/mnras/stw391. C. P. O’Dea.PASP, 110(747):493–532, May

    work page doi:10.1093/mnras/stw391

  58. [58]

    doi: 10.1086/316162. P. Padovani.A&ARv, 24(1):13, Sept

    work page doi:10.1086/316162

  59. [59]

    doi: 10.1007/s00159-016-0098-6. P. Padovani et al.A&ARv, 25(1):2, Aug. 2017a. doi: 10.1007/s00159-017-0102-9. P. Padovani et al.A&ARv, 25(1):2, Aug. 2017b. doi: 10.1007/s00159-017-0102-9. F. Panessa and M. Giroletti.MNRAS, 432(2):1138–1143, June

    work page doi:10.1007/s00159-016-0098-6

  60. [60]

    doi: 10.1093/mnras/stt547. F. Panessa et al.Nature Astronomy, 3:387–396, Apr

    work page doi:10.1093/mnras/stt547

  61. [61]

    doi: 10.1038/s41550-019-0765-4. F. Panessa et al.MNRAS, 510(1):718–724, Feb

    work page doi:10.1038/s41550-019-0765-4

  62. [62]

    doi: 10.1093/mnras/stab3426. K. Perger, S. Frey, K. É. Gabányi, and L. V. Tóth.Frontiers in Astronomy and Space Sciences, 4: 9, Aug

    work page doi:10.1093/mnras/stab3426

  63. [63]

    doi: 10.3389/fspas.2017.00009. P. O. Petrucci et al.A&A, 678:L4, Oct

    work page doi:10.3389/fspas.2017.00009 2017

  64. [64]

    R.M.Plotkinetal.MNRAS,419(1):267–286,Jan.2012

    doi: 10.1051/0004-6361/202347495. R.M.Plotkinetal.MNRAS,419(1):267–286,Jan.2012. doi: 10.1111/j.1365-2966.2011.19689.x. I. Prandoni et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202347495 2012

  65. [65]

    doi: 10.1051/0004-6361/202038591. C. Ricci et al.ApJL, 952(2):L28, Aug

    work page doi:10.1051/0004-6361/202038591

  66. [66]

    doi: 10.3847/2041-8213/acda27. I. Ruffa et al.MNRAS, 522(4):6170–6195, July

    work page doi:10.3847/2041-8213/acda27 2041

  67. [67]

    doi: 10.1093/mnras/stad1119. P. Saikia, E. Körding, and S. Dibi.MNRAS, 477(2):2119–2127, June

    work page doi:10.1093/mnras/stad1119

  68. [68]

    doi: 10.1093/mnras/ sty754. M. T. Sargent et al.ApJSS, 186(2):341–377, Feb

    work page doi:10.1093/mnras/

  69. [69]

    doi: 10.1088/0067-0049/186/2/341. T. Sbarrato et al.MNRAS, 426(1):L91–L95, Oct

    work page doi:10.1088/0067-0049/186/2/341

  70. [70]

    doi: 10.1111/j.1745-3933.2012.01332.x. B. Sebastian et al.MNRAS, 499(1):334–354, Nov

    work page doi:10.1111/j.1745-3933.2012.01332.x 2012

  71. [71]

    doi: 10.1093/mnras/staa2473. E. Shablovinskaya et al.A&A, 690:A232, Oct

    work page doi:10.1093/mnras/staa2473

  72. [72]

    doi: 10.1051/0004-6361/202450133. M. Sikora, Ł. Stawarz, and J.-P. Lasota.ApJ, 658(2):815–828, Apr

    work page doi:10.1051/0004-6361/202450133

  73. [73]

    doi: 10.1086/511972. S. Silpa et al.MNRAS, 507(1):991–1001, Oct. 2021a. doi: 10.1093/mnras/stab1870. S. Silpa et al.MNRAS, 507(2):2550–2561, Oct. 2021b. doi: 10.1093/mnras/stab2110. S. Silpa et al.MNRAS, 513(3):4208–4223, July

    work page doi:10.1086/511972

  74. [74]

    doi: 10.1093/mnras/stac1044. C. Spingola et al.A&A, 643:L12, Nov

    work page doi:10.1093/mnras/stac1044

  75. [75]

    doi: 10.1051/0004-6361/202039458. C. Spingola et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202039458

  76. [76]

    doi: 10.1111/j.1745-3933.2011.01147.x. J. S. Ulvestad and L. C. Ho.ApJ, 558(2):561–577, Sept

    work page doi:10.1111/j.1745-3933.2011.01147.x 2011

  77. [77]

    doi: 10.1086/322307. J. S. Ulvestad and A. S. Wilson.ApJ, 285:439–452, Oct

    work page doi:10.1086/322307

  78. [78]

    J.S.Ulvestad,R.R.J.Antonucci,andR.W.Goodrich.AJ,109:81,Jan.1995

    doi: 10.1086/162520. J.S.Ulvestad,R.R.J.Antonucci,andR.W.Goodrich.AJ,109:81,Jan.1995. doi: 10.1086/117258. 16 AGN accretion and ejection Panessa et al. M. Volonteri, M. Sikora, and J.-P. Lasota.ApJ, 667(2):704–713, Oct

    work page doi:10.1086/162520 1995

  79. [79]

    doi: 10.1086/521186. A. Wang et al.MNRAS, 504(3):3823–3830, July

    work page doi:10.1086/521186

  80. [80]

    doi: 10.1093/mnras/stab587. A. Wang et al.MNRAS, 518(1):39–53, Jan. 2023a. doi: 10.1093/mnras/stac3091. A. Wang et al.MNRAS, 523(1):L30–L34, July 2023b. doi: 10.1093/mnrasl/slad051. A. Wang et al.MNRAS, 525(4):6064–6083, Nov. 2023c. doi: 10.1093/mnras/stad2651. A. Wang et al.ApJL, 987(2):L26, July

    work page doi:10.1093/mnras/stab587

Showing first 80 references.