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arxiv: 2606.25580 · v1 · pith:2UZLCROXnew · submitted 2026-06-24 · 🌌 astro-ph.GA

The magnetic field in the Milky Way Galaxy: from large to small scales

Xiaohui Sun , Jennifer West , Marijke Haverkorn , Andrea Bracco , Anna Ordog , Sui Ann Mao , Yik Ki Ma , Wenhui Jing
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Thiem Hoang
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Pith reviewed 2026-06-25 20:44 UTC · model grok-4.3

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keywords magnetic fieldsMilky Wayrotation measureSKAgalactic magnetismpolarizationdiffuse emissionsouthern Galactic hemisphere
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The pith

SKA-Mid polarization survey will produce the most complete picture of the Milky Way's magnetic field in the southern Galactic hemisphere from large to small scales.

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

The Milky Way offers a unique laboratory for examining how magnetic fields form, change over time, and affect other galactic elements because observations can reach the smallest details. An SKA-Mid polarization survey is projected to create an all-sky rotation measure grid roughly 100 times denser than existing ones, reaching about 100 sources per square degree. It will also generate total intensity, polarized intensity, and RM images of diffuse emission that span scales starting from roughly 10 arcseconds when merged with single-dish data. These products together are expected to deliver the most complete view of the magnetic field structure across the southern Galactic hemisphere.

Core claim

The dense RM grid and images of diffuse emission will allow us to determine the most complete picture of the magnetic field in the southern Galactic hemisphere from large to small scales.

What carries the argument

The SKA-Mid polarization survey delivering an all-sky RM grid at ~100 sources per square degree together with multi-scale total intensity, polarized intensity, and RM images of diffuse emission.

If this is right

  • The survey data will address fundamental questions on how magnetic fields are generated and evolve in the Galaxy.
  • It will clarify how magnetic fields influence other components such as gas and cosmic rays.
  • The resulting maps will span the full range of spatial scales from large galactic structures to small interstellar features in the southern hemisphere.
  • This dataset can serve as a reference for modeling magnetic fields in external galaxies.

Where Pith is reading between the lines

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

  • Matching southern maps with existing or future northern hemisphere data could produce a full-sky model of the Milky Way's magnetic field.
  • The high source density may support statistical analyses of magnetic field fluctuations and turbulence on small scales.
  • The multi-scale images could test predictions from galactic dynamo simulations at both large and small scales.

Load-bearing premise

The SKA-Mid polarization survey will achieve an all-sky RM grid density of about 100 per square degree and produce total intensity, polarized intensity, and RM images of diffuse emission covering scales from about 10 arcseconds upward after combination with single-dish observations.

What would settle it

If the delivered RM grid density falls well below 100 sources per square degree or the combined images fail to recover the full range of spatial scales from 10 arcseconds upward, the claim of obtaining the most complete picture would not hold.

Figures

Figures reproduced from arXiv: 2606.25580 by Andrea Bracco, Anna Ordog, Jennifer West, Marijke Haverkorn, Sui Ann Mao, Thiem Hoang, Wenhui Jing, Xiaohui Sun, Yik Ki Ma.

Figure 1
Figure 1. Figure 1: All-sky RM grid surveys: LoTSS, POGS, VLASS, NVSS, SPICE-RACS, and POSSUM, showing 5 key parameters: sky coverage, sensitivity, FWHM of the RMSF, RM density, and resolution. For comparison, an SKA-Mid survey discussed in Sect. 3 is shown in each panel. The sensitivity and FWHM of the RMSF are displayed on logarithmic scales. There is no RMSF for NVSS because RMs were derived from two frequencies not able t… view at source ↗
Figure 2
Figure 2. Figure 2: Antenna layout for AA* and 𝑢𝑣 coverage and distributions for a 15 min observation of a source at 𝛿 = −60◦ at the central frequency of 1.31 GHz of SKA-Mid Band 2. The remote dish SKA-008 was excluded. layout for AA* and the 𝑢𝑣 distributions using the ska_ost_array_config2 package. Note that the simulations results are similar for AA4 if the 2 ′′ resolution is used. The frequency is 1.31 GHz which is the cen… view at source ↗
Figure 3
Figure 3. Figure 3: Image of the Galactic RM sky (Hutschenreuter et al., 2022) and RMs of extragalactic sources from NVSS (Taylor et al., 2009), POSSUM (Anderson et al., 2021), and MeerKAT (Loi et al., 2025) overlaid on the NVSS total intensity image at 1.4 GHz. 13 [PITH_FULL_IMAGE:figures/full_fig_p013_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: 𝑢𝑣 coverage, baseline distribution, and PSFs along the major and minor axes for uniform and natural weightings for a simulated 15 min observation with AA*, only using dishes within 5 km of baselines. The PSF sizes are displayed in the two bottom panels. and we extrapolated STAPS data assuming a spectral index for the combination. As can be seen, the combined image shows structures of scales from the EMU re… view at source ↗
Figure 5
Figure 5. Figure 5: Total intensity images from STAPS (Sun et al., 2025), ASKAP EMU (Hopkins et al., 2025), and the two combined. 16 [PITH_FULL_IMAGE:figures/full_fig_p016_5.png] view at source ↗
read the original abstract

The Milky Way is the galaxy in which we can study its magnetic field to the finest details, providing an ideal laboratory to understand the fundamental questions: how magnetic field is generated and evolves, and how it influences other components in the Galaxy. An SKA-Mid polarization survey will produce an all-sky rotation measure (RM) grid with a density of about 100 per square degree, which is approximately two orders of magnitude larger than what is currently available, and produce total intensity, polarized intensity, and RM all-sky images of diffuse emission covering scales from about 10 arcseconds upward after combination with single-dish observations. The dense RM grid and images of diffuse emission will allow us to determine the most complete picture of the magnetic field in the southern Galactic hemisphere from large to small scales.

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 is a forward-looking perspective that describes the anticipated products of an SKA-Mid polarization survey and their implications for Milky Way magnetic-field studies. It states that the survey will deliver an all-sky RM grid at a density of ~100 sources per square degree (two orders of magnitude above current catalogs) together with total-intensity, polarized-intensity, and RM images of diffuse emission on scales from ~10 arcsec upward once combined with single-dish data. These products are projected to yield the most complete picture of the magnetic field in the southern Galactic hemisphere from large to small scales.

Significance. If the quoted survey specifications are realized, the resulting RM grid and diffuse-emission maps would provide a step-change in data density and angular-scale coverage for Galactic magnetism, enabling tighter constraints on field generation, evolution, and coupling to other ISM components across the southern sky. The manuscript correctly aligns its projections with publicly documented SKA survey plans and does not introduce new derivations or fitted parameters.

minor comments (1)
  1. [Abstract] Abstract: the quoted RM density and resolution figures would benefit from an explicit citation to the relevant SKA survey design documents or white papers so that readers can directly verify the numbers.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive review of the manuscript and their recommendation to accept. The report contains no major comments requiring a point-by-point response.

Circularity Check

0 steps flagged

No circularity; forward-looking survey projection with no derivations

full rationale

The paper is a perspective piece describing anticipated SKA-Mid survey capabilities and their expected scientific impact on mapping the Galactic magnetic field. It contains no equations, no fitted parameters, no predictions derived from data, and no self-citations used to justify load-bearing claims. The central statement about obtaining the 'most complete picture' is an explicit forward-looking expectation, not a result obtained by reducing inputs to outputs via any chain. No steps match any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No free parameters, axioms, or invented entities are introduced; the document is a review of observational prospects rather than a theoretical or empirical derivation.

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Works this paper leans on

92 extracted references · 90 canonical work pages · 3 internal anchors

  1. [1]

    doi: 10.1017/pasa.2021.4. B. D. Ball et al.MNRAS, 524(1):1396–1421, Sept

    work page doi:10.1017/pasa.2021.4 2021

  2. [2]

    doi: 10.1093/mnras/stad1953. B. D. Ball et al.ApJ, 988(1):75, July

    work page doi:10.1093/mnras/stad1953

  3. [3]

    doi: 10.3847/1538-4357/addc63. R. Beck and B. M. Gaensler.New Astron. Rev., 48(11-12):1289–1304, Dec

    work page doi:10.3847/1538-4357/addc63

  4. [4]

    Drgoňa et al

    doi: 10.1016/j. newar.2004.09.013. R. Beck, A. Shukurov, D. Sokoloff, and R. Wielebinski.A&A, 411:99–107, Nov

    work page doi:10.1016/j 2004

  5. [5]

    doi: 10.1051/0004-6361:20031101. A. Berger et al.A&A, 693:A202, Jan

    work page doi:10.1051/0004-6361:20031101

  6. [6]

    doi: 10.1051/0004-6361/202245733. F. Boulanger et al.JCAP, 2018(8):049, Aug

    work page doi:10.1051/0004-6361/202245733 2018

  7. [7]

    doi: 10.1088/1475-7516/2018/08/049. A. Bracco, M. Padovani, and D. Galli.A&A, 686:A52, June

    work page doi:10.1088/1475-7516/2018/08/049 2018

  8. [8]

    doi: 10.1051/0004-6361/ 202449625. A. Brandenburg and E. Ntormousi.ARA&A, 61:561–606, Aug

    work page doi:10.1051/0004-6361/

  9. [9]

    M.A.BrentjensandA.G.deBruyn.A&A,441(3):1217–1228,Oct.2005

    doi: 10.1146/ annurev-astro-071221-052807. M.A.BrentjensandA.G.deBruyn.A&A,441(3):1217–1228,Oct.2005. doi: 10.1051/0004-6361: 20052990. J. C. Brown and A. R. Taylor.ApJL, 563(1):L31–L34, Dec

    work page doi:10.1051/0004-6361: 2005

  10. [10]

    doi: 10.1086/338358. B. J. Burn.MNRAS, 133:67, Jan

    work page doi:10.1086/338358

  11. [11]

    doi: 10.1093/mnras/133.1.67. E. Carretti et al.MNRAS, 489(2):2330–2354, Oct

    work page doi:10.1093/mnras/133.1.67

  12. [12]

    doi: 10.1093/mnras/stz806. A. P. Curtin, J. M. Weisberg, and J. M. Rankin.ApJ, 975(2):217, Nov

    work page doi:10.1093/mnras/stz806

  13. [13]

    doi: 10.3847/1538-4357/ac94ce. A. Erceg et al.A&A, 663:A7, July

    work page doi:10.3847/1538-4357/ac94ce

  14. [14]

    doi: 10.1051/0004-6361/202142244. K. Ferrière and P. Terral.A&A, 561:A100, Jan

    work page doi:10.1051/0004-6361/202142244

  15. [15]

    doi: 10.1051/0004-6361/201322966. B. M. Gaensler et al.ApJ, 549(2):959–978, Mar

    work page doi:10.1051/0004-6361/201322966

  16. [16]

    doi: 10.1086/319468. B. M. Gaensler et al.Nature, 478(7368):214–217, Oct

    work page doi:10.1086/319468

  17. [17]

    doi: 10.1038/nature10446. B. M. Gaensler et al.PASA, 42:e091, June

    work page doi:10.1038/nature10446

  18. [18]

    doi: 10.1017/pasa.2025.10031. J. L. Han.ARA&A, 55(1):111–157, Aug

    work page doi:10.1017/pasa.2025.10031 2025

  19. [19]

    doi: 10.1146/annurev-astro-091916-055221. J. L. Han, R. N. Manchester, and G. J. Qiao.MNRAS, 306(2):371–380, June

    work page doi:10.1146/annurev-astro-091916-055221

  20. [20]

    1365-2966.2003.07017.x

    doi: 10.1046/j. 1365-8711.1999.02544.x. J. L. Han, R. N. Manchester, W. van Straten, and P. Demorest.ApJSS, 234(1):11, Jan

    work page doi:10.1046/j 1999

  21. [21]

    M.Haverkorn

    doi: 10.3847/1538-4365/aa9c45. M.Haverkorn. InA.Lazarian,E.M.deGouveiaDalPino,andC.Melioli,editors,MagneticFields in Diffuse Media, volume 407 ofAstrophysics and Space Science Library, page 483, Jan

    work page doi:10.3847/1538-4365/aa9c45

  22. [22]

    doi: 10.1007/978-3-662-44625-6_17. M. Haverkorn, P. Katgert, and A. G. de Bruyn.A&A, 356:L13–L16, Apr

    work page doi:10.1007/978-3-662-44625-6_17

  23. [23]

    doi: 10.48550/ arXiv.astro-ph/0003260. M. Haverkorn, J. C. Brown, B. M. Gaensler, and N. M. McClure-Griffiths.ApJ, 680(1):362–370, June

    Pith/arXiv arXiv

  24. [24]

    doi: 10.1086/587165. M. Haverkorn et al. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 96, Apr

    work page doi:10.1086/587165

  25. [25]

    doi: 10.22323/1.215.0096. G. Heald et al.Galaxies, 8(3):53, July

    work page doi:10.22323/1.215.0096

  26. [26]

    Galaxies , keywords =

    doi: 10.3390/galaxies8030053. 20 Magnetic field in the Milky Way Galaxy Sun et al. T. Hoang and A. Lazarian.ApJ, 831(2):159, Nov

    work page doi:10.3390/galaxies8030053

  27. [27]

    doi: 10.3847/0004-637X/831/2/159. T. Hoang and B. Truong.ApJ, 965(2):183, Apr

    work page doi:10.3847/0004-637x/831/2/159

  28. [28]

    doi: 10.3847/1538-4357/ad2a56. A. Hopkins et al.PASA, 42:e071, May

    work page doi:10.3847/1538-4357/ad2a56

  29. [29]

    doi: 10.1017/pasa.2025.10042. S. Hutschenreuter et al.A&A, 657:A43, Jan

    work page doi:10.1017/pasa.2025.10042 2025

  30. [30]

    doi: 10.1051/0004-6361/202140486. T. R. Jaffe.Galaxies, 7(2):52, Apr

    work page doi:10.1051/0004-6361/202140486

  31. [31]

    doi: 10.3390/galaxies7020052. T. R. Jaffe et al.MNRAS, 401(2):1013–1028, Jan

    work page doi:10.3390/galaxies7020052

  32. [32]

    doi: 10.1111/j.1365-2966.2009.15745.x. R. Jansson and G. R. Farrar.ApJL, 761(1):L11, Dec

    work page doi:10.1111/j.1365-2966.2009.15745.x 2009

  33. [33]

    doi: 10.1088/2041-8205/761/1/L11. S. Jiao et al.Science China Physics, Mechanics, and Astronomy, 65(9):299511, Sept

    work page doi:10.1088/2041-8205/761/1/l11 2041

  34. [34]

    M.Johnston-Hollittetal

    doi: 10.1007/s11433-021-1902-3. M.Johnston-Hollittetal. InAdvancingAstrophysicswiththeSquareKilometreArray(AASKA14), page 92, Apr

    work page doi:10.1007/s11433-021-1902-3 1902

  35. [35]

    doi: 10.22323/1.215.0092. A. Khadir et al.ApJ, 977(2):276, Dec

    work page doi:10.22323/1.215.0092

  36. [36]

    doi: 10.3847/1538-4357/ad8ddf. J. Koda et al.PASP, 131(999):054505, May

    work page doi:10.3847/1538-4357/ad8ddf

  37. [37]

    doi: 10.1088/1538-3873/ab047e. M. Krause et al.A&A, 639:A112, July

    work page doi:10.1088/1538-3873/ab047e

  38. [38]

    doi: 10.1051/0004-6361/202037780. M. Lacy et al.PASP, 132(1009):035001, Mar

    work page doi:10.1051/0004-6361/202037780

  39. [39]

    doi: 10.1088/1538-3873/ab63eb. A. Lazarian, K. H. Yuen, and D. Pogosyan.ApJ, 974(2):237, Oct

    work page doi:10.1088/1538-3873/ab63eb

  40. [41]

    doi: 10.3847/1538-4357/ac09e4. D. Li et al.IEEE Microwave Magazine, 19(3):112–119, Apr

    work page doi:10.3847/1538-4357/ac09e4

  41. [42]

    doi: 10.1109/MMM.2018. 2802178. F. Loi et al.A&A, 694:A125, Feb

    work page doi:10.1109/mmm.2018 2018

  42. [43]

    doi: 10.1051/0004-6361/202451711. Y. K. Ma et al.MNRAS, 487(3):3432–3453, Aug

    work page doi:10.1051/0004-6361/202451711

  43. [44]

    doi: 10.1093/mnras/stz1325. Y. K. Ma, S. A. Mao, A. Ordog, and J. C. Brown.MNRAS, 497(3):3097–3117, Sept

    work page doi:10.1093/mnras/stz1325

  44. [45]

    doi: 10.1093/mnras/staa2105. Y. K. Ma et al.MNRAS, 541(1):306–336, July

    work page doi:10.1093/mnras/staa2105

  45. [46]

    Y.K.Maetal

    doi: 10.1093/mnras/staf1000. Y.K.Maetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Ma01. E. Maconi et al.A&A, 698:A84, June

    work page doi:10.1093/mnras/staf1000 2026

  46. [47]

    doi: 10.1051/0004-6361/202451477. S. A. Mao et al.ApJ, 714(2):1170–1186, May

    work page doi:10.1051/0004-6361/202451477

  47. [48]

    doi: 10.1088/0004-637X/714/2/1170. S. A. Mao et al.ApJ, 755(1):21, Aug

    work page doi:10.1088/0004-637x/714/2/1170

  48. [49]

    doi: 10.1088/0004-637X/755/1/21. S. A. Mao et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1088/0004-637x/755/1/21

  49. [50]

    doi: 10.1093/mnrasl/ slv176. A. H. Minter and S. R. Spangler.ApJ, 458:194, Feb

    work page doi:10.1093/mnrasl/

  50. [51]

    doi: 10.1086/176803. S. K. Ocker and J. M. Cordes.arXiv e-prints, art. arXiv:2602.11838, Feb

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/176803

  51. [52]

    doi: 10.48550/ arXiv.2602.11838. A. Ordog, J. C. Brown, R. Kothes, and T. L. Landecker.A&A, 603:A15, July

    Pith/arXiv arXiv

  52. [53]

    doi: 10.3847/1538-3881/adc929. A. Ordog et al.ApJSS, 282(2):53, Feb

    work page doi:10.3847/1538-3881/adc929

  53. [54]

    doi: 10.3847/1538-4365/ae2471. S. P. O’Sullivan et al.MNRAS, 519(4):5723–5742, Mar

    work page doi:10.3847/1538-4365/ae2471

  54. [55]

    doi: 10.1093/mnras/stac3820. L. S. Oswald et al.MNRAS, 540(3):2112–2130, July

    work page doi:10.1093/mnras/stac3820

  55. [56]

    21 Magnetic field in the Milky Way Galaxy Sun et al

    doi: 10.1093/mnras/staf645. 21 Magnetic field in the Milky Way Galaxy Sun et al. A. Pandhi et al.ApJ, 982(2):146, Apr

    work page doi:10.1093/mnras/staf645

  56. [57]

    K.Pattleetal

    doi: 10.3847/1538-4357/adb8e3. K.Pattleetal. InS.Inutsukaetal.,editors,ProtostarsandPlanetsVII,volume534ofAstronomical Society of the Pacific Conference Series, page 193, July

    work page doi:10.3847/1538-4357/adb8e3

  57. [58]

    doi: 10.48550/arXiv.2203.11179. V. Pelgrims, J. F. Macías-Pérez, and F. Ruppin.A&A, 652:A130, Aug

    work page doi:10.48550/arxiv.2203.11179

  58. [59]

    doi: 10.1051/0004-6361/201528033. A. Plunkett et al.PASP, 135(1045):034501, Mar

    work page doi:10.1051/0004-6361/201528033

  59. [60]

    doi: 10.1088/1538-3873/acb9bd. I. Prandoni and N. Seymour. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 67, Apr

    work page doi:10.1088/1538-3873/acb9bd

  60. [61]

    C.R.Purcelletal.RM-Tools: Rotationmeasure(RM)synthesisandStokesQU-fitting.Astrophysics Source Code Library, record ascl:2005.003, May

    doi: 10.22323/1.215.0067. C.R.Purcelletal.RM-Tools: Rotationmeasure(RM)synthesisandStokesQU-fitting.Astrophysics Source Code Library, record ascl:2005.003, May

    work page doi:10.22323/1.215.0067 2005

  61. [62]

    doi: 10.1051/0004-6361/202348993. U. Rau, N. Naik, and T. Braun.AJ, 158(1):3, July

    work page doi:10.1051/0004-6361/202348993

  62. [63]

    doi: 10.3847/1538-3881/ab1aa7. C. J. Riseley et al.PASA, 37:e029, July

    work page doi:10.3847/1538-3881/ab1aa7

  63. [64]

    doi: 10.1017/pasa.2020.20. L. Rudnick and F. N. Owen.ApJ, 785(1):45, Apr

    work page doi:10.1017/pasa.2020.20 2020

  64. [65]

    doi: 10.1088/0004-637X/785/1/45. D. H. F. M. Schnitzeler.MNRAS, 409(1):L99–L103, Nov

    work page doi:10.1088/0004-637x/785/1/45

  65. [66]

    doi: 10.1111/j.1745-3933.2010. 00957.x. D. H. F. M. Schnitzeler et al.MNRAS, 485(1):1293–1309, May

    work page doi:10.1111/j.1745-3933.2010 2010

  66. [67]

    doi: 10.1093/mnras/stz092. A. Seta and C. Federrath.MNRAS, 499(2):2076–2086, Dec

    work page doi:10.1093/mnras/stz092 2076

  67. [68]

    doi: 10.1093/mnras/staa2978. A. Seta and C. Federrath.MNRAS, 502(2):2220–2237, Apr

    work page doi:10.1093/mnras/staa2978

  68. [69]

    doi: 10.1093/mnras/stab128. A. M. Shukurov and K. Subramanian.Astrophysical Magnetic Fields: From Galaxies to the Early Universe

    work page doi:10.1093/mnras/stab128

  69. [70]

    D.D.Sokoloffetal.MNRAS,299(1):189–206,Aug.1998.doi: 10.1046/j.1365-8711.1998.01782.x

    doi: 10.1017/9781139046657. D.D.Sokoloffetal.MNRAS,299(1):189–206,Aug.1998.doi: 10.1046/j.1365-8711.1998.01782.x. J. M. Stil, A. R. Taylor, and C. Sunstrum.ApJ, 726(1):4, Jan

    work page doi:10.1017/9781139046657 1998

  70. [71]

    doi: 10.1088/0004-637X/726/ 1/4. K. Subramanian.Reports on Progress in Physics, 79(7):076901, July

    work page doi:10.1088/0004-637x/726/

  71. [72]

    X.Sunetal

    doi: 10.1051/0004-6361/202453326. X.H.SunandW.Reich.A&A,507(2):1087–1105,Nov.2009.doi: 10.1051/0004-6361/200912539. X. H. Sun et al.A&A, 463(3):993–1007, Mar

    work page doi:10.1051/0004-6361/202453326 2009

  72. [73]

    doi: 10.1051/0004-6361:20066001. X. H. Sun, W. Reich, A. Waelkens, and T. A. Enßlin.A&A, 477(2):573–592, Jan

    work page doi:10.1051/0004-6361:20066001

  73. [74]

    doi: 10.1051/0004-6361:20078671. X. H. Sun et al.ApJ, 811(1):40, Sept. 2015a. doi: 10.1088/0004-637X/811/1/40. X. H. Sun et al.AJ, 149(2):60, Feb. 2015b. doi: 10.1088/0004-6256/149/2/60. X.-H. Sun et al.Research in Astronomy and Astrophysics, 22(12):125011, Dec

    work page doi:10.1051/0004-6361:20078671

  74. [75]

    doi: 10.1088/1674-4527/ac9d27. M. Tahani et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1088/1674-4527/ac9d27

  75. [76]

    doi: 10.1093/mnras/stae169. A. J. M. Thomson et al.PASA, 40:e040, Aug

    work page doi:10.1093/mnras/stae169

  76. [77]

    doi: 10.1017/pasa.2023.38. A. J. M. Thomson et al.arXiv e-prints, art. arXiv:2605.16917, May

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pasa.2023.38 2023

  77. [78]

    The Rapid ASKAP Continuum Survey VII: Spectra and Polarisation In Cutouts of Extragalactic Sources (SPICE-RACS) Second Data Release -- Unveiling the Magnetised Sky

    doi: 10.48550/arXiv. 22 Magnetic field in the Milky Way Galaxy Sun et al. 2605.16917. L. N. Tram and T. Hoang.Frontiers in Astronomy and Space Sciences, 9:923927, Oct

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

  78. [79]

    doi: 10.3389/fspas.2022.923927. B. Truong and T. Hoang.ApJ, 981(1):83, Mar

    work page doi:10.3389/fspas.2022.923927 2022

  79. [80]

    doi: 10.3847/1538-4357/adb423. M. Unger and G. R. Farrar.ApJ, 970(1):95, July

    work page doi:10.3847/1538-4357/adb423

  80. [81]

    doi: 10.3847/1538-4357/ad4a54. C. L. Van Eck et al.ApJ, 728(2):97, Feb

    work page doi:10.3847/1538-4357/ad4a54

Showing first 80 references.