pith. sign in

arxiv: 2606.24810 · v1 · pith:NQDLQHZLnew · submitted 2026-06-23 · 🌌 astro-ph.GA · astro-ph.IM

Measuring Magnetic Fields Near and Far with the SKA via the Zeeman Effect

Timothy Robishaw , Marta Nowotka , Tao-Chung Ching , James A. Green , Anita M. S. Richards , Sandra Etoka , Malcolm Gray , Susan E. Clark
show 2 more authors
Tyler L. Bourke Vincent Fish
This is my paper

Pith reviewed 2026-06-25 23:19 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.IM
keywords Zeeman effectmagnetic fieldsSKAOH masersdamped Lyman-alpha systemsradio recombination linesinterstellar mediumgalaxy evolution
0
0 comments X

The pith

The Square Kilometre Array will measure magnetic fields via Zeeman splitting across targets from solar-system comets to cosmological damped Lyman-alpha systems.

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

The paper shows how the SKA can detect Zeeman splitting in emission and absorption lines to obtain direct estimates of magnetic field strength and direction in gas at vastly different distances. It updates prior sensitivity calculations to indicate which goals are reachable with partial array builds such as AA4 or AA* and which require the full SKA. A reader would care because these measurements would supply in-situ field data in the neutral interstellar medium and in external galaxies, complementing rotation-measure programs and opening direct probes of magnetic roles in galaxy evolution.

Core claim

Zeeman splitting in spectral lines provides direct estimates of magnetic field strength and direction in magnetized gas; the SKA will enable such measurements in targets spanning cometary comas, Galactic molecular clouds, HI filaments, high-velocity clouds, the Fermi Bubbles, photodissociation regions via radio recombination lines, OH masers and megamasers in starburst galaxies, and cold neutral gas in damped Ly-alpha systems at high redshift, with specific capabilities available at Array Assembly 4, AA*, or full buildout.

What carries the argument

Zeeman splitting of spectral lines in emission and absorption, which directly yields magnetic field strength and direction when the splitting is resolved.

If this is right

  • SKA-Mid will enable Zeeman studies of OH kilomasers in nearby starburst systems.
  • The census of megamaser Zeeman detections will expand substantially beyond the Arecibo sky.
  • Magnetic fields in damped Lyman-alpha systems can be probed to field limits well below those currently achievable.
  • Stacking radio recombination lines across hundreds of transitions will extend Zeeman measurements to HII regions and photodissociation regions.
  • Zeeman data will complement Faraday rotation programs by supplying in-situ measurements in the warm and cold neutral interstellar medium.

Where Pith is reading between the lines

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

  • These Zeeman detections could directly constrain how magnetic fields shape gas dynamics during galaxy assembly at different epochs.
  • Combined Zeeman and rotation-measure maps of the same sightlines would test whether field orientations inferred from one method match those from the other.
  • Non-detections in high-velocity clouds or the Fermi Bubbles at the predicted sensitivities would indicate either weaker fields or additional depolarisation mechanisms not included in the calculations.

Load-bearing premise

The updated sensitivity calculations accurately predict detectable Zeeman signals in the listed targets without major unmodeled effects such as line blending, insufficient polarization, or source variability.

What would settle it

If SKA-Mid observations of OH kilomasers in a nearby starburst galaxy yield no detectable Zeeman splitting at the field strength the calculations predict should be visible, the reach claimed for that target class would be falsified.

read the original abstract

Zeeman splitting in spectral lines -- both in emission and absorption -- provides direct estimates of magnetic field strength and direction in magnetized gas in our own Milky Way and in external galaxies. We discuss the potential for using the Square Kilometre Array (SKA) to measure the Zeeman effect in targets spanning an enormous range of distance: from cometary comas in the solar system, through Galactic molecular clouds, HI filaments in the cold neutral medium, high-velocity clouds, the Fermi Bubbles, and photodissociation regions (PDRs) traced by radio recombination lines, to OH masers and megamasers in nearby and distant starburst galaxies, and to cold neutral gas in damped Ly-alpha absorbing systems at cosmological redshifts. We update the sensitivity calculations of Robishaw et al. (2015) and indicate, for each science goal, whether it will be achievable with Array Assembly 4 (AA4) of SKA-Mid, with the staged delivery of AA*, or only with the full SKA buildout. Zeeman measurements will probe the magnetic field in situ in the warm and cold neutral interstellar medium, complementing SKA Faraday rotation programs; radio recombination lines, stackable across hundreds of transitions, extend this reach to HII regions and PDRs. In external galaxies, SKA-Mid will enable Zeeman studies of OH kilomasers in nearby starburst systems, substantially expand the census of megamaser Zeeman detections beyond the Arecibo sky, and probe magnetic fields in damped Lyman-alpha systems to field limits well below those currently achievable, opening a new window on the role of magnetic fields in galaxy formation and cosmic 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 / 2 minor

Summary. The paper claims that the SKA (via AA4, AA*, and full buildout) will enable Zeeman-effect measurements of magnetic fields across scales from solar-system comae to cosmological damped Ly-alpha systems, updating the sensitivity calculations of Robishaw et al. (2015) to show which targets become accessible at each stage; this includes OH kilomasers in starbursts, expanded megamaser detections, and sub-current field limits in DLAs, complementing Faraday-rotation programs.

Significance. If the updated sensitivity calculations prove accurate, the work identifies a concrete path for direct in-situ B-field measurements in the neutral ISM and high-redshift absorbers that would complement existing SKA Faraday-rotation efforts and open new constraints on the role of magnetic fields in galaxy evolution.

major comments (1)
  1. [Abstract / sensitivity-update section] Abstract and sensitivity-update discussion: the central claim that SKA-Mid will reach the stated field limits in OH kilomasers and DLAs rests on the updated calculations correctly predicting detectable signals; however, it is unclear whether these calculations incorporate line blending in complex velocity fields, source variability on observing timescales, or realistic polarization fractions, all of which are flagged as potential degradations in the stress-test note and would directly affect the listed AA4/AA*/full-SKA reach statements.
minor comments (2)
  1. The manuscript would benefit from an explicit table or subsection listing the key assumptions (e.g., line width, polarization fraction, integration time) used in the updated sensitivity calculations for each target class.
  2. References to Robishaw et al. (2015) should include a brief recap of which parameters were revised and why, to allow readers to assess the magnitude of the update without consulting the earlier paper.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their detailed review and constructive feedback on our manuscript. We address the major comment point by point below.

read point-by-point responses

  1. Referee: [Abstract / sensitivity-update section] Abstract and sensitivity-update discussion: the central claim that SKA-Mid will reach the stated field limits in OH kilomasers and DLAs rests on the updated calculations correctly predicting detectable signals; however, it is unclear whether these calculations incorporate line blending in complex velocity fields, source variability on observing timescales, or realistic polarization fractions, all of which are flagged as potential degradations in the stress-test note and would directly affect the listed AA4/AA*/full-SKA reach statements.

    Authors: We thank the referee for this observation. The sensitivity calculations presented in the manuscript are updates to those in Robishaw et al. (2015) and are based on the same assumptions regarding line widths, polarization fractions, and signal detectability. The stress-test note in the manuscript explicitly identifies line blending due to complex velocity fields, source variability, and deviations from assumed polarization fractions as potential factors that could reduce the effective sensitivity. As such, the quoted field limits for the different array stages represent optimistic estimates under idealized conditions. We agree that this distinction should be made clearer in the abstract and sensitivity discussion. We will revise the manuscript to state explicitly that the calculations do not incorporate these degradations and to note that real-world observations may require longer integration times or may achieve somewhat weaker field limits. A full quantitative assessment of these effects for each target class would require detailed simulations tailored to individual sources, which is beyond the scope of the current work. revision: partial

Circularity Check

0 steps flagged

Minor self-citation to prior sensitivity calculations; no load-bearing circular derivations or self-defined predictions.

full rationale

The paper updates sensitivity calculations from Robishaw et al. (2015) (with author overlap) to assess SKA reach for Zeeman measurements across targets, but contains no equations, fitted parameters, or derivation chains that reduce to inputs by construction. Claims rely on standard sensitivity methods and external literature without internal circularity; the self-citation is not load-bearing for any 'prediction' that is statistically forced or self-definitional.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The paper rests on the standard domain assumption that Zeeman splitting directly yields magnetic field strength and direction. No free parameters, invented entities, or additional axioms are stated in the abstract.

axioms (1)
  • domain assumption Zeeman splitting in spectral lines provides direct estimates of magnetic field strength and direction in magnetized gas
    This premise is stated in the opening sentence and underpins all listed science goals.

pith-pipeline@v0.9.1-grok · 5878 in / 1292 out tokens · 21967 ms · 2026-06-25T23:19:37.739284+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

89 extracted references · 86 canonical work pages

  1. [1]

    doi: 10.22323/1.215.0093. L. D. Anderson et al.ApJSS, 254(2):28, June

    work page doi:10.22323/1.215.0093

  2. [2]

    M.K.Argoetal.MNRAS,402(4):2703–2714,Mar.2010

    doi: 10.3847/1538-4365/abef65. M.K.Argoetal.MNRAS,402(4):2703–2714,Mar.2010. doi: 10.1111/j.1365-2966.2009.16100.x. D. S. Balser.Science China Physics, Mechanics, and Astronomy, 65(12):129707, Dec

    work page doi:10.3847/1538-4365/abef65 2010

  3. [3]

    doi: 10.1007/s11433-022-2038-7. D. S. Balser et al.ApJ, 816(1):22, Jan

    work page doi:10.1007/s11433-022-2038-7 2038

  4. [4]

    doi: 10.3847/0004-637X/816/1/22. S. K. Betti et al.ApJ, 871(2):215, Feb

    work page doi:10.3847/0004-637x/816/1/22

  5. [5]

    doi: 10.3847/1538-4357/aaf886. T. L. Bourke et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.3847/1538-4357/aaf886

  6. [6]

    , keywords =

    arXiv search: Report number AASKAII/Bourke01. S.L.Breen,S.P.Ellingsen,J.L.Caswell,andB.E.Lewis.MNRAS,401(4):2219–2244,Feb.2010. doi: 10.1111/j.1365-2966.2009.15831.x. S. L. Breen et al.MNRAS, 435(1):524–530, Oct

    work page doi:10.1111/j.1365-2966.2009.15831.x 2010

  7. [7]

    doi: 10.1093/mnras/stt1315. K. J. Brooks and J. B. Whiteoak.MNRAS, 291(3):395–402, Nov

    work page doi:10.1093/mnras/stt1315

  8. [8]

    doi: 10.1093/mnras/291. 3.395. J. C. Brown et al.ApJ, 663(1):258–266, July

    work page doi:10.1093/mnras/291

  9. [9]

    doi: 10.1086/518499. M. P. Busch.ApJ, 967(2):148, June

    work page doi:10.1086/518499

  10. [10]

    doi: 10.3847/1538-4357/ad3af6. E. Carretti et al.Nature, 493(7430):66–69, Jan

    work page doi:10.3847/1538-4357/ad3af6

  11. [11]

    doi: 10.1038/nature11734. P. Castangia et al.A&A, 529:A150, May

    work page doi:10.1038/nature11734

  12. [12]

    doi: 10.1051/0004-6361/201016403. S. Chandrasekhar and E. Fermi.ApJ, 118:113, July

    work page doi:10.1051/0004-6361/201016403

  13. [13]

    doi: 10.1086/145731. X. Chen et al.AJ, 169(3):158, Mar

    work page doi:10.1086/145731

  14. [14]

    doi: 10.3847/1538-3881/ada8aa. T.-C. Ching et al.Nature, 601(7891):49–52, Jan

    work page doi:10.3847/1538-3881/ada8aa

  15. [15]

    doi: 10.1038/s41586-021-04159-x. P. Colom, J. Crovisier, N. Biver, and D. Bockelée-Morvan. InEPSC-DPS Joint Meeting 2011, volume 2011, page 837, Oct

    work page doi:10.1038/s41586-021-04159-x 2011

  16. [16]

    doi: 10.1088/2041-8205/792/1/L2. M. A. Cordiner et al.ApJ, 953(1):59, Aug

    work page doi:10.1088/2041-8205/792/1/l2 2041

  17. [17]

    doi: 10.3847/1538-4357/ace0bc. R. M. Crocker and F. Aharonian.Phys. Rev. Let., 106(10):101102, Mar

    work page doi:10.3847/1538-4357/ace0bc

  18. [18]

    doi: 10.3389/fspas.2019.00066. R. M. Crutcher et al.ApJ, 407:175, Apr

    work page doi:10.3389/fspas.2019.00066 2019

  19. [19]

    doi: 10.1086/172503. R. M. Crutcher et al.ApJ, 725(1):466–479, Dec

    work page doi:10.1086/172503

  20. [20]

    doi: 10.1088/0004-637X/725/1/466. R. D. Davies. In F. J. Kerr and S. C. Simonson, editors,Galactic Radio Astronomy, volume 60 of IAU Symposium, page 275, Jan

    work page doi:10.1088/0004-637x/725/1/466

  21. [21]

    doi: 10.1051/0004-6361/200913387. D. Despois, E. Gérard, J. Crovisier, and I. Kazès.A&A, 99:320–340, June

    work page doi:10.1051/0004-6361/200913387

  22. [22]

    doi: 10.1088/1538-3873/128/969/115006. S. P. Ellingsen.MNRAS, 377(2):571–583, May

    work page doi:10.1088/1538-3873/128/969/115006

  23. [23]

    doi: 10.1111/j.1365-2966.2007.11615.x. S. Etoka and P. Diamond.MNRAS, 348(1):34–45, Feb

    work page doi:10.1111/j.1365-2966.2007.11615.x 2007

  24. [24]

    doi: 10.1111/j.1365-2966.2004. 07370.x. 16 Zeeman Measurements Near and Far Robishaw et al. S. Etoka and P. J. Diamond.MNRAS, 406(4):2218–2234, Aug

    work page doi:10.1111/j.1365-2966.2004 2004

  25. [25]

    2012.21704.x

    doi: 10.1111/j.1365-2966. 2010.16840.x. S. Etoka et al. In S. J. Murphy and M. S. Bessell, editors,The Eighth Pacific Rim Conference on StellarAstrophysics: ATributetoKam-ChingLeung,volume404ofAstronomicalSocietyofthe Pacific Conference Series, page 311, Aug

    work page doi:10.1111/j.1365-2966 2010

  26. [26]

    doi: 10.22323/1.215.0125. S. Etoka et al.MNRAS, 468(2):1703–1716, June

    work page doi:10.22323/1.215.0125

  27. [27]

    doi: 10.1093/mnras/stx448. V. L. Fish, M. J. Reid, A. L. Argon, and K. M. Menten.ApJ, 596(1):328–343, Oct

    work page doi:10.1093/mnras/stx448

  28. [28]

    doi: 10.1086/377081. V. L. Fish, M. J. Reid, A. L. Argon, and X.-W. Zheng.ApJSS, 160(1):220–271, Sept

    work page doi:10.1086/377081

  29. [29]

    doi: 10.1086/431669. A. J. Fox et al.ApJL, 816(1):L11, Jan

    work page doi:10.1086/431669

  30. [30]

    doi: 10.3847/2041-8205/816/1/L11. B. M. Gaensler et al.Science, 307(5715):1610–1612, Mar

    work page doi:10.3847/2041-8205/816/1/l11 2041

  31. [31]

    doi: 10.1126/science.1108832. Z. Gan-Baruch, R. Wegmann, A. Eviatar, and H. U. Schmidt.J. Geophys. Res., 103(A10):23639– 23652, Oct

    work page doi:10.1126/science.1108832

  32. [32]

    doi: 10.1029/97JA02651. E. Gérard.A&A, 146(1):1–10, May

    work page doi:10.1029/97ja02651

  33. [33]

    doi: 10.1016/S0032-0633(97) 00197-9. J. F. Gómez et al.MNRAS, 461(3):3259–3273, Sept

    work page doi:10.1016/s0032-0633(97

  34. [34]

    doi: 10.1093/mnras/stw1536. A. A. Goodman and C. Heiles.ApJ, 424:208, Mar

    work page doi:10.1093/mnras/stw1536

  35. [35]

    doi: 10.1086/173884. J. A. Green et al.MNRAS, 392(2):783–794, Jan

    work page doi:10.1086/173884

  36. [36]

    BH scaling relations and the AGN luminosity function

    doi: 10.1111/j.1365-2966.2008.14091.x. J.A.Greenetal.MNRAS,425(4):2530–2547,Oct.2012. doi: 10.1111/j.1365-2966.2012.21722.x. J. A. Green et al.MNRAS, 440(4):2988–2996, June

    work page doi:10.1111/j.1365-2966.2008.14091.x 2008

  37. [37]

    doi: 10.1093/mnras/stu429. J. A. Green, J. L. Caswell, and N. M. McClure-Griffiths.MNRAS, 451(1):74–92, July 2015a. doi: 10.1093/mnras/stv936. J. A. Green et al.Highlights of Astronomy, 16:402–402, Mar. 2015b. doi: 10.1017/ S1743921314011715. J. A. Green et al. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 119, Apr. 2015c. doi: ...

    work page doi:10.1093/mnras/stu429

  38. [38]

    doi: 10.1088/0004-637X/756/2/181. J. L. Han and J. S. Zhang.A&A, 464(2):609–614, Mar

    work page doi:10.1088/0004-637x/756/2/181

  39. [39]

    doi: 10.1051/0004-6361:20065801. G. Heald et al.Galaxies, 8(3):53, July

    work page doi:10.1051/0004-6361:20065801

  40. [40]

    doi: 10.3390/galaxies8030053. C. Heiles.ApJ, 324:321, Jan

    work page doi:10.3390/galaxies8030053

  41. [41]

    doi: 10.1086/165897. C. Heiles.ApJ, 336:808, Jan

    work page doi:10.1086/165897

  42. [42]

    doi: 10.1086/167051. C. Heiles.ApJ, 466:224, July

    work page doi:10.1086/167051

  43. [43]

    doi: 10.1086/177504. C. Heiles.ApJSS, 111(1):245–288, July

    work page doi:10.1086/177504

  44. [44]

    doi: 10.1086/313010. C. Heiles and T. H. Troland.ApJL, 260:L23–L26, Sept

    work page doi:10.1086/313010

  45. [45]

    doi: 10.1086/183862. C. Heiles and T. H. Troland.ApJSS, 151(2):271–297, Apr

    work page doi:10.1086/183862

  46. [46]

    doi: 10.1086/381753. C. Heiles and T. H. Troland.ApJ, 624(2):773–793, May

    work page doi:10.1086/381753

  47. [47]

    C.Heiles,A.A.Goodman,C.F.McKee,andE.G.Zweibel

    doi: 10.1086/428896. C.Heiles,A.A.Goodman,C.F.McKee,andE.G.Zweibel. InE.H.LevyandJ.I.Lunine,editors, Protostars and Planets III, page 279, Jan

    work page doi:10.1086/428896

  48. [48]

    doi: 10.1088/0004-637X/777/1/55. L. G. Hou and X. Y. Gao.MNRAS, 495(4):4326–4333, July

    work page doi:10.1088/0004-637x/777/1/55

  49. [49]

    doi: 10.1093/mnras/staa1461. Z. Hu, B. D. Wibking, and M. R. Krumholz.MNRAS, 521(4):5604–5615, June

    work page doi:10.1093/mnras/staa1461

  50. [50]

    , keywords =

    doi: 10.1093/mnras/stad931. IAU.InG.ContopoulosandA.Jappel,editors,TransactionsoftheIAU,Vol.XVB1973,Proceedings of the Fifteenth General Assembly, pages 165–167, Dordrecht,

    work page doi:10.1093/mnras/stad931

  51. [51]

    IEEE.IEEE Standard for Definitions of Terms for Radio Wave Propagation, IEEE Std

    Reidel. IEEE.IEEE Standard for Definitions of Terms for Radio Wave Propagation, IEEE Std. 211-2018,

    2018

  52. [52]

    doi: 10.1117/12.3020829. P. Jagannathan, S. Bhatnagar, U. Rau, and A. R. Taylor.AJ, 154(2):56, Aug

    work page doi:10.1117/12.3020829

  53. [53]

    , keywords =

    doi: 10.3847/1538-4357/ab672b. M.Johnston-Hollittetal. InAdvancingAstrophysicswiththeSquareKilometreArray(AASKA14), page 92, Apr

    work page doi:10.3847/1538-4357/ab672b

  54. [54]

    doi: 10.22323/1.215.0092. D. Li and P. F. Goldsmith.ApJ, 585(2):823–839, Mar

    work page doi:10.22323/1.215.0092

  55. [55]

    doi: 10.1086/346227. D. J. Linville et al.ApJ, 959(2):110, Dec

    work page doi:10.1086/346227

  56. [56]

    F.J.LockmanandN.M.McClure-Griffiths.ApJ,826(2):215,Aug.2016

    doi: 10.3847/1538-4357/acfc39. F.J.LockmanandN.M.McClure-Griffiths.ApJ,826(2):215,Aug.2016. doi: 10.3847/0004-637X/ 826/2/215. Y.K.Maetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Ma01. S. A. Mao et al.ApJ, 688(2):1029–1049, Dec

    work page doi:10.3847/1538-4357/acfc39 2016

  57. [57]

    doi: 10.1086/590546. J. McBride and C. Heiles.ApJ, 763(1):8, Jan

    work page doi:10.1086/590546

  58. [58]

    doi: 10.1088/0004-637X/763/1/8. J. McBride, E. Quataert, C. Heiles, and A. Bauermeister.ApJ, 780(2):182, Jan

    work page doi:10.1088/0004-637x/763/1/8

  59. [59]

    doi: 10.1088/0004-637X/780/2/182. J. McBride et al.MNRAS, 447(2):1103–1111, Feb

    work page doi:10.1088/0004-637x/780/2/182

  60. [60]

    doi: 10.1093/mnras/stu2489. N. M. McClure-Griffiths et al.ApJ, 652(2):1339–1347, Dec

    work page doi:10.1093/mnras/stu2489

  61. [61]

    doi: 10.1086/508706. V. Minier, S. P. Ellingsen, R. P. Norris, and R. S. Booth.A&A, 403:1095–1100, June

    work page doi:10.1086/508706

  62. [62]

    doi: 10.1051/0004-6361:20030465. Y. Mizuguchi, M. Akagawa, and H. Yokoi.Electronics Communications of Japan, 61:58–66, Mar

    work page doi:10.1051/0004-6361:20030465

  63. [63]

    doi: 10.1086/429559. P. C. Myers and V. K. Khersonsky.ApJ, 442:186, Mar

    work page doi:10.1086/429559

  64. [64]

    doi: 10.1086/175434. M. Nowotka et al.ApJ, 992(1):129, Oct

    work page doi:10.1086/175434

  65. [65]

    doi: 10.3847/1538-4357/adff52. C. S. Ogbodo et al.MNRAS, 493(1):199–233, Mar

    work page doi:10.3847/1538-4357/adff52

  66. [66]

    doi: 10.1093/mnras/staa167. R. Oonk et al. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 139, Apr

    work page doi:10.1093/mnras/staa167

  67. [67]

    doi: 10.22323/1.215.0139. X.-J. Ouyang et al.ApJL, 964(2):L18, Apr

    work page doi:10.22323/1.215.0139

  68. [68]

    doi: 10.3847/2041-8213/ad3338. M. R. Pestalozzi, V. Minier, and R. S. Booth.A&A, 432(2):737–742, Mar

    work page doi:10.3847/2041-8213/ad3338 2041

  69. [69]

    18 Zeeman Measurements Near and Far Robishaw et al

    doi: 10.3847/0004-637X/817/1/37. 18 Zeeman Measurements Near and Far Robishaw et al. M. J. Reid and E. M. Silverstein.ApJ, 361:483, Oct

    work page doi:10.3847/0004-637x/817/1/37

  70. [70]

    doi: 10.1086/169212. A. M. S. Richards et al.MNRAS, 364(2):353–366, Dec

    work page doi:10.1086/169212

  71. [71]

    doi: 10.1111/j.1365-2966.2005. 09588.x. T. Robishaw.Magnetic Fields Near and Far: Galactic and Extragalactic Single-Dish Radio Observations of the Zeeman Effect. PhD thesis, University of California, Berkeley, May

    work page doi:10.1111/j.1365-2966.2005 2005

  72. [72]

    doi: 10.1086/588031. T. Robishaw et al. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 110, Apr

    work page doi:10.1086/588031

  73. [73]

    doi: 10.22323/1.215.0110. N. X. Roth et al.ApJ, 921(1):14, Nov

    work page doi:10.22323/1.215.0110

  74. [74]

    doi: 10.3847/1538-4357/ac0441. K. L. J. Rygl et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.3847/1538-4357/ac0441

  75. [75]

    P.Salas etal

    arXiv search: Report number AASKAII/Rygl01. P.Salas etal. InAdvancingAstrophysics withthe SKA–II (AASKAII).2026. arXiv search: Report number AASKAII/Salas01. K. C. Sarkar.A&ARv, 32(1):1, Mar

    2026

  76. [76]

    A.SetaandN.M.McClure-Griffiths.MNRAS,539(2):1024–1039,May2025

    doi: 10.1007/s00159-024-00152-1. A.SetaandN.M.McClure-Griffiths.MNRAS,539(2):1024–1039,May2025. doi: 10.1093/mnras/ staf520. A. J. Smith et al.Planet. Sci. J., 2(4):123, Aug

    work page doi:10.1007/s00159-024-00152-1

  77. [77]

    doi: 10.3847/PSJ/abfec7. X. Sun et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.3847/psj/abfec7

  78. [78]

    doi: 10.1051/0004-6361: 200810858. M. Tahani et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361:

  79. [79]

    doi: 10.1093/mnras/stv1133. T. H. Troland and C. Heiles.ApJ, 252:179–192, Jan. 1982a. doi: 10.1086/159544. T. H. Troland and C. Heiles.ApJL, 260:L19–L22, Sept. 1982b. doi: 10.1086/183861. C. L. Van Eck et al.ApJ, 728(2):97, Feb

    work page doi:10.1093/mnras/stv1133

  80. [80]

    doi: 10.1088/0004-637X/728/2/97. G. L. Verschuur.ApJ, 339:163, Apr

    work page doi:10.1088/0004-637x/728/2/97

Showing first 80 references.