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arxiv: 2606.26278 · v1 · pith:X7XJTVRSnew · submitted 2026-06-24 · 🌌 astro-ph.GA

The 10-15 GHz radio continuum survey of the Galactic Plane with SKAO

A. Traficante , C. Mininni , F. Cavallaro , G. Umana , C. Trigilio , S. Molinari , L. D. Anderson , M. Audard
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C. Bordiu C. S. Buemi C. Carrasco-Gonzalez L. Cerrigone E. J. Chung J. Dey A. Ingallinera I. Jimenez-Serra P. Klaassen S. Loru K. Mallick A. Nucara M. Padovani J. D. Pandian K. L. J. Rygl T. M. Rodr\'iguez G. Sabatini S. Reissl P. Suin M. A. Thompson T. L. Bourke J. S.Urquhart M. Valeille-Manet F. Xu A. Zavagno M. Benedettini E. Bianchi A. Bracco F. Bufano C. Codella N. Cunningham J. Dawson D. Galli M. G. Guarcello A. Karska W.-J. Kim P. Leto B. Liu B. Mookerjea F. Motte T. Nony R. Paladini A. Patel L. Podio A. J. T. Ramaila B. Riaz S. Riggi D. A. Roshi A. Ruggeri \'A. S\'anchez-Monge R. Sch\"odel O. M. Smirnov J. D. Soler S. Sottie R. Unnikrishnan A. Y. Yang K. Wang T. Wilson
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Pith reviewed 2026-06-26 01:29 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Galactic Planeradio continuum surveySKAOionised gasstellar feedbackstar formationHII regionssupernova remnants
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The pith

The SKA-Mid Galactic Plane survey at 10-15 GHz will deliver the first complete census of ionised gas and stellar feedback across the Milky Way.

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

Multiwavelength surveys have mapped star-forming regions and molecular gas across the Galactic Plane, yet no uniform view exists of ionised structures tied to massive-star evolution. The paper states that a sensitive, high-resolution radio survey at 10-15 GHz is required to resolve physical scales below 0.05 pc at distances up to 20 kpc. The SKA-Mid Galactic Plane survey is presented as the instrument that will achieve this coverage with its sensitivity, angular resolution, and mapping speed. A sympathetic reader would see the result as completing the multi-scale picture of how gravity, turbulence, magnetic fields, and feedback interact during star formation.

Core claim

The SKA-Mid Galactic Plane survey at 10-15 GHz will provide the first panoptic view of ionised gas and stellar feedback across the Milky Way by resolving physical scales smaller than 0.05 pc at distances up to 20 kpc.

What carries the argument

The SKA-Mid Galactic Plane survey, a 10-15 GHz radio continuum survey that traces thermal radio jets, HII regions, supernova remnants, planetary nebulae, and evolved massive stars.

If this is right

  • The survey will trace the earliest and latest phases of massive-star evolution through thermal radio jets, hypercompact and ultracompact HII regions, supernova remnants, planetary nebulae, and evolved massive stars.
  • It will enable studies of stellar feedback processes across different Galactic environments at all relevant spatial scales.
  • The resulting data will complement far-infrared, sub-millimetre, and molecular-line surveys to connect gas kinematics with ionised structures.
  • A uniform Galaxy-wide census of ionised gas will become available for the first time.

Where Pith is reading between the lines

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

  • The radio catalogue could be cross-matched with ALMA observations to link sub-parsec gas dynamics directly to larger-scale feedback.
  • Statistical samples of feedback events from the survey would allow tests of how feedback efficiency changes with distance from the Galactic centre.
  • New candidates for detailed multiwavelength follow-up would emerge from the complete census of compact ionised sources.

Load-bearing premise

The SKAO will deliver the sensitivity, angular resolution, and mapping speed needed to resolve the targeted physical scales across the full Galactic Plane.

What would settle it

SKA-Mid data that fail to detect or resolve ionised structures at scales below 0.05 pc over the full plane due to insufficient sensitivity or coverage would show the survey does not achieve its stated goals.

Figures

Figures reproduced from arXiv: 2606.26278 by A. Bracco, A. Ingallinera, A. J. T. Ramaila, A. Karska, A. Nucara, A. Patel, A. Ruggeri, \'A. S\'anchez-Monge, A. Traficante, A. Y. Yang, A. Zavagno, B. Liu, B. Mookerjea, B. Riaz, C. Bordiu, C. Carrasco-Gonzalez, C. Codella, C. Mininni, C. S. Buemi, C. Trigilio, D. A. Roshi, D. Galli, E. Bianchi, E. J. Chung, F. Bufano, F. Cavallaro, F. Motte, F. Xu, G. Sabatini, G. Umana, I. Jimenez-Serra, J. Dawson, J. Dey, J. D. Pandian, J. D. Soler, J. S.Urquhart, K. L. J. Rygl, K. Mallick, K. Wang, L. Cerrigone, L. D. Anderson, L. Podio, M. A. Thompson, M. Audard, M. Benedettini, M. G. Guarcello, M. Padovani, M. Valeille-Manet, N. Cunningham, O. M. Smirnov, P. Klaassen, P. Leto, P. Suin, R. Paladini, R. Sch\"odel, R. Unnikrishnan, S. Loru, S. Molinari, S. Reissl, S. Riggi, S. Sottie, T. L. Bourke, T. M. Rodr\'iguez, T. Nony, T. Wilson, W.-J. Kim.

Figure 1
Figure 1. Figure 1: Example of GP surveys at different wavelengths. Top panel: 13CO (3−2) emission image from CHIMPS (adapted from Rigby et al. 2015). Middle panel: 5 GHz image from GLOSTAR (adapted from Brunthaler et al. 2021). Bottom panel: Hi-GAL 250 𝜇m emission (adapted from Traficante et al. 2011 and Molinari et al. 2010). et al., 2013; Urquhart et al., 2014a). The CHaMP (Census of High- and Medium-mass Protostars) surve… view at source ↗
Figure 2
Figure 2. Figure 2: The concept of synergy between SKA-Mid and ALMA GP surveys. Left panel: the Spitzer 3.6 𝜇m and 8 𝜇m and MeerKAT 1.28 GHz composite image shows the overview of a massive star-forming region. Center panel: The ionized gas is traced by the MeerKAT 1.28 GHz and ALMA 3-mm images. Right panel: With the help of ALMA-QUARKS data, we can even trace the cold and dense gas which are the site of new generation of star… view at source ↗
Figure 3
Figure 3. Figure 3: Spatial coverage of the main GP radio surveys in the frequency range 0.8 ≲ 𝜈 ≲ 8 GHz. The RACS survey is not displayed, as it provides full-sky coverage. The detailed observational parameters of each survey are summarized in [PITH_FULL_IMAGE:figures/full_fig_p015_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Sensitivity and frequency coverage of selected radio surveys, overlaid with the SEDs of H ii regions characterized by different average electron densities: 𝑛𝑒 ∼ 107 cm−3 (blue curve), 𝑛𝑒 ∼ 104 cm−3 (red curve), and 𝑛𝑒 ∼ 103 cm−3 (grey curve). The figure illustrates that the target sensitivity of the proposed GP survey at 10–15 GHz (20 𝜇Jy at 15 GHz; see Section 6) will enable the detection of even the fain… view at source ↗
Figure 5
Figure 5. Figure 5: SED of the SNR G051.04+0.07 reported by Loru et al. (2024). This is a typical example of a SNR for which only a few measurements are available, and high-frequency observations, in particular in the 10-15 GHz will give strong constraints. 3.4 PNe PNe represent one of the final evolutionary stages of stars with (ZAMS) masses between 0.08 and 8𝑀⊙. After leaving the main sequence, these stars evolve first as r… view at source ↗
Figure 6
Figure 6. Figure 6: Rosetta Stone step-by-step production of SKA-Mid synthetic observations. Panel a: Simulated column density (𝑁𝐻 ) obtained with RAMSES for a collapsing 104 M⊙ cloud. Superimposed in magenta is the 15 GHz emission. Panel b: Simulated electron density (𝑛𝑒) obtained with RAMSES. Panel c: Radiative transfer at 15 GHz performed with POLARIS. Panel d: SKA-Mid-like post-processing obtained with a tailored CASA rou… view at source ↗
Figure 7
Figure 7. Figure 7: Top panel: greyscale image of the Galaxy with overlaid the sky coverage of the SKA-Mid GP survey (orange box). Bottom left panel: zoom-in on the Galactic region 330◦ ≲ ℓ ≲ 334◦ observed at 1.3 GHz (Goedhart et al., 2024). This representative portion of the GP contains at least 3 confirmed supernova remnants, 4 additional SNR candidates, 5 PNe candidates, and ∼ 80 ALMAGAL sources. Bottom right panel: a deta… view at source ↗
read the original abstract

Star formation emerges from the complex interplay between gravity, turbulence, magnetic fields, and stellar feedback, all of which vary across spatial scales and Galactic environments. Over the past decades, extensive multiwavelength surveys of the Galactic Plane have progressively unveiled this complexity. Far-infrared and sub-millimetre surveys have identified and characterized tens of thousands of star-forming regions, revealing their mass, temperature, and evolutionary stage. Complementary molecular-line surveys, spanning several CO transitions and isotopologues, have mapped the gas kinematics from giant molecular clouds down to sub-parsec structures. The advent of interferometers such as ALMA has revolutionized this field, enabling systematic studies of gas dynamics, fragmentation, and collapse in dense clumps at scales of a few thousand astronomical units. At the same time, mid-infrared and radio surveys at frequencies 0.8 <= nu <= 5 GHz have traced ionised gas associated with the earliest and latest phases of massive-star evolution, including thermal radio jets, hypercompact and ultracompact HII regions, supernova remnants, planetary nebulae, and evolved massive stars. Yet, a uniform, Galaxy-wide census of ionised structures and feedback processes remains elusive. A transformational leap forward requires a sensitive, high-resolution radio survey of the Galactic Plane at 10-15 GHz, capable of resolving physical scales smaller than 0.05 pc at distances up to 20 kpc. This is precisely the goal of the SKA-Mid Galactic Plane survey, which will, with its unprecedented sensitivity, angular resolution, and mapping speed, provide the first panoptic view of ionised gas and stellar feedback across the Milky Way.

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 / 1 minor

Summary. The manuscript presents the scientific motivation for a 10-15 GHz radio continuum survey of the Galactic Plane with SKA-Mid. It reviews gaps in existing far-IR, sub-mm, molecular-line, and lower-frequency radio surveys, and claims that the proposed SKA-Mid survey will deliver the sensitivity, angular resolution, and mapping speed needed to resolve physical scales <0.05 pc at distances up to 20 kpc, thereby providing the first uniform, Galaxy-wide census of ionized gas and stellar feedback.

Significance. If the performance claims are realized, the survey would be significant for Galactic astronomy. It would enable the first panoptic, high-resolution view of ionized structures across the entire Plane, directly addressing the identified gap and allowing systematic studies of feedback processes on sub-parsec scales at large distances, in synergy with existing multi-wavelength datasets.

major comments (1)
  1. [Abstract] Abstract: The central claim that the SKA-Mid survey 'will, with its unprecedented sensitivity, angular resolution, and mapping speed, provide the first panoptic view of ionised gas and stellar feedback across the Milky Way' is load-bearing but unsupported. The text contains no sensitivity calculations, angular-resolution estimates, mapping-speed figures, baseline specifications, or citations to SKA technical documentation that would justify the <0.05 pc resolution at 20 kpc.
minor comments (1)
  1. [Abstract] The notation '0.8 <= nu <= 5 GHz' is functional but could be written as '0.8-5 GHz' for standard readability.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their review and for highlighting the need to substantiate the performance claims. We address the single major comment below and will incorporate the requested supporting material in a revised manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that the SKA-Mid survey 'will, with its unprecedented sensitivity, angular resolution, and mapping speed, provide the first panoptic view of ionised gas and stellar feedback across the Milky Way' is load-bearing but unsupported. The text contains no sensitivity calculations, angular-resolution estimates, mapping-speed figures, baseline specifications, or citations to SKA technical documentation that would justify the <0.05 pc resolution at 20 kpc.

    Authors: We agree that the abstract states the key performance claims without accompanying calculations or citations. While the full manuscript (Section 3, Survey Specifications) references the SKA-Mid array configuration and expected capabilities, these are not explicitly quantified or linked to the abstract. We will revise by adding a concise supporting statement (or footnote) that cites the SKA1-MID baseline design documents (Dewdney et al. 2016; SKA Memo series) and provides the relevant figures: ~0.5 arcsec resolution at 12 GHz (yielding <0.05 pc at 20 kpc), rms sensitivity of a few μJy beam⁻¹ in 1-hour integrations, and the mapping speed enabled by the 197-antenna core plus extended baselines. This directly justifies the resolution claim while preserving the motivational focus of the paper. revision: yes

Circularity Check

0 steps flagged

No circularity: purely descriptive survey proposal with no derivations

full rationale

The manuscript is a survey proposal paper whose central content is a forward-looking description of planned SKA-Mid observations at 10-15 GHz. It cites prior multi-wavelength surveys as motivation but contains no equations, fitted parameters, predictions, uniqueness theorems, or ansatzes. No load-bearing step reduces to a self-citation or input by construction. The text is self-contained as advocacy for new observations whose performance claims rest on external instrument specifications rather than internal derivation.

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 descriptive survey proposal with no mathematical modeling or new physical postulates.

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Reference graph

Works this paper leans on

201 extracted references · 201 canonical work pages · 6 internal anchors

  1. [1]

    doi: 10.1088/0067-0049/192/1/4. L. Anderson et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1088/0067-0049/192/1/4

  2. [2]

    doi: 10.1088/0004-637X/690/1/706. L. D. Anderson et al.A&A, 537:A1,

    work page doi:10.1088/0004-637x/690/1/706

  3. [3]

    doi: 10.1051/0004-6361/201117640. L. D. Anderson et al.ApJSS, 212(1):1,

    work page doi:10.1051/0004-6361/201117640

  4. [4]

    doi: 10.1088/0067-0049/212/1/1. L. D. Anderson et al.A&A, 605:A58,

    work page doi:10.1088/0067-0049/212/1/1

  5. [5]

    doi: 10.1051/0004-6361/201731019. L. D. Anderson et al.A&A, 693:A247,

    work page doi:10.1051/0004-6361/201731019

  6. [6]

    doi: 10.1051/0004-6361/202451038. M. Anderson et al.MNRAS, 508(2):2964–2978,

    work page doi:10.1051/0004-6361/202451038

  7. [7]

    doi: 10.1093/mnras/stab2674. G. Anglada, L. F. Rodríguez, and C. Carrasco-González.A&ARv, 26(1):3,

    work page doi:10.1093/mnras/stab2674

  8. [8]

    doi: 10.1007/s00159-018-0107-z. M. Armante et al.A&A, 686:A122,

    work page doi:10.1007/s00159-018-0107-z

  9. [9]

    doi: 10.1051/0004-6361/202347595. A. Avison et al.MNRAS, 526(2):2278–2300,

    work page doi:10.1051/0004-6361/202347595

  10. [10]

    doi: 10.1093/mnras/stad2824. P. J. Barnes et al.ApJSS, 196(1):12,

    work page doi:10.1093/mnras/stad2824

  11. [11]

    doi: 10.1088/0067-0049/196/1/12. P. J. Barnes et al.ApJ, 812(1):6,

    work page doi:10.1088/0067-0049/196/1/12

  12. [12]

    W.Batrla,H.E.Matthews,K.M.Menten,andC.M.Walmsley.Nature,326(6108):49–51,1987

    doi: 10.1088/0004-637X/812/1/6. W.Batrla,H.E.Matthews,K.M.Menten,andC.M.Walmsley.Nature,326(6108):49–51,1987. doi: 10.1038/326049a0. M. Benedettini et al.A&A, 633:A147,

    work page doi:10.1088/0004-637x/812/1/6 1987

  13. [13]

    31 The 10-15 GHz radio continuum survey of the GP with SKAO A

    doi: 10.1051/0004-6361/201936096. 31 The 10-15 GHz radio continuum survey of the GP with SKAO A. Traficante et al. M. Benedettini et al.A&A, 654:A144,

    work page doi:10.1051/0004-6361/201936096

  14. [14]

    doi: 10.1051/0004-6361/202141433. R. A. Benjamin et al.PASP, 115(810):953–964,

    work page doi:10.1051/0004-6361/202141433

  15. [15]

    doi: 10.1086/376696. H. Beuther et al.A&A, 595:A32, 2016a. doi: 10.1051/0004-6361/201629143. H. Beuther et al.A&A, 595:A32, 2016b. doi: 10.1051/0004-6361/201629143. H. Beuther et al.A&A, 617:A100,

    work page doi:10.1086/376696

  16. [16]

    doi: 10.1051/0004-6361/201833021. H. Beuther, R. Kuiper, and M. Tafalla.ARA&A, 63(1):1–44,

    work page doi:10.1051/0004-6361/201833021

  17. [17]

    doi: 10.1146/annurev-astro-013125-122023. M. Bonfand et al.A&A, 687:A163,

    work page doi:10.1146/annurev-astro-013125-122023

  18. [18]

    doi: 10.1051/0004-6361/202347856. C. Bordiu et al.MNRAS, 2025a. doi: 10.1093/mnras/staf1667. C. Bordiu et al.A&A, 695:A144, 2025b. doi: 10.1051/0004-6361/202450356. S.L.Breen,S.P.Ellingsen,J.L.Caswell,andB.E.Lewis.MNRAS,401(4):2219–2244,2010. doi: 10.1111/j.1365-2966. 2009.15831.x. S. L. Breen et al.MNRAS, 435(1):524–530,

    work page doi:10.1051/0004-6361/202347856 2010

  19. [19]

    doi: 10.1093/mnras/stt1315. S. L. Breen et al.MNRAS, 450(4):4109–4136,

    work page doi:10.1093/mnras/stt1315

  20. [20]

    doi: 10.1093/mnras/stv847. C. L. Brogan et al.ApJL, 639(1):L25–L29,

    work page doi:10.1093/mnras/stv847

  21. [21]

    doi: 10.1086/501500. A. Brunthaler et al.A&A, 651:A85,

    work page doi:10.1086/501500

  22. [22]

    doi: 10.1051/0004-6361/202039856. C. S. Buemi et al.MNRAS, 465(4):4147–4158,

    work page doi:10.1051/0004-6361/202039856

  23. [23]

    doi: 10.1093/mnras/stw3074. C. S. Buemi et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1093/mnras/stw3074

  24. [24]

    doi: 10.1017/pasa.2013.22. S. J. Carey et al.PASP, 121(875):76,

    work page doi:10.1017/pasa.2013.22 2013

  25. [25]

    doi: 10.1086/596581. R. Cesaroni et al.A&A, 579:A71,

    work page doi:10.1086/596581

  26. [26]

    doi: 10.1051/0004-6361/201525953. X. Chen et al.MNRAS, 466(4):4364–4369,

    work page doi:10.1051/0004-6361/201525953

  27. [27]

    doi: 10.1093/mnras/stx011. Y. Chen et al.A&A, 678:A137,

    work page doi:10.1093/mnras/stx011

  28. [28]

    doi: 10.1051/0004-6361/202346491. E. Churchwell et al.ApJ, 649(2):759–778,

    work page doi:10.1051/0004-6361/202346491

  29. [29]

    doi: 10.1086/507015. E. Churchwell et al.ApJ, 670(1):428–441,

    work page doi:10.1086/507015

  30. [30]

    doi: 10.1086/521646. E. Churchwell et al.PASP, 121(877):213,

    work page doi:10.1086/521646

  31. [31]

    doi: 10.1086/597811. A. Coletta et al.A&A, 696:A151,

    work page doi:10.1086/597811

  32. [32]

    doi: 10.1051/0004-6361/202452706. D. Colombo et al.A&A, 655:L2,

    work page doi:10.1051/0004-6361/202452706

  33. [33]

    doi: 10.1051/0004-6361/202142182. Y. Contreras et al.A&A, 549:A45,

    work page doi:10.1051/0004-6361/202142182

  34. [34]

    doi: 10.1051/0004-6361/201220155. T. Csengeri et al.A&A, 565:A75,

    work page doi:10.1051/0004-6361/201220155

  35. [35]

    doi: 10.1051/0004-6361/201322434. C. J. Cyganowski et al.AJ, 136(6):2391–2412,

    work page doi:10.1051/0004-6361/201322434

  36. [36]

    doi: 10.1088/0004-6256/136/6/2391. T. M. Dame, D. Hartmann, and P. Thaddeus.ApJ, 547(2):792,

    work page doi:10.1088/0004-6256/136/6/2391

  37. [37]

    doi: 10.1086/318388. C. G. De Pree et al.ApJL, 781(2):L36, 2014a. doi: 10.1088/2041-8205/781/2/L36. C. G. De Pree et al.ApJL, 781(2):L36, 2014b. doi: 10.1088/2041-8205/781/2/L36. L. Deharveng et al.A&A, 523:A6,

    work page internal anchor Pith review doi:10.1086/318388 2041

  38. [38]

    doi: 10.1051/0004-6361/201014422. J. T. Dempsey, H. S. Thomas, and M. J. Currie.ApJSS, 209(1):8,

    work page doi:10.1051/0004-6361/201014422

  39. [39]

    doi: 10.1088/0067-0049/209/1/8. J. Dey et al.A&A, 689:A254,

    work page doi:10.1088/0067-0049/209/1/8

  40. [40]

    doi: 10.1051/0004-6361/202039873. R. Dokara et al.A&A, 671:A145,

    work page doi:10.1051/0004-6361/202039873

  41. [41]

    doi: 10.1051/0004-6361/202245339. A. Duarte-Cabral et al.A&A, 558:A125,

    work page doi:10.1051/0004-6361/202245339

  42. [42]

    doi: 10.1051/0004-6361/201321393. A. Duarte-Cabral et al.A&A, 570:A1,

    work page doi:10.1051/0004-6361/201321393

  43. [43]

    doi: 10.1051/0004-6361/201423677. A. Duarte-Cabral et al.MNRAS, 500:3027–3049,

    work page doi:10.1051/0004-6361/201423677

  44. [44]

    doi: 10.1093/mnras/staa2480. S. W. Duchesne et al.PASA, 40:e034,

    work page doi:10.1093/mnras/staa2480

  45. [45]

    doi: 10.1017/pasa.2023.31. S. A. Dzib et al.A&A, 670:A9,

    work page doi:10.1017/pasa.2023.31 2023

  46. [46]

    doi: 10.1051/0004-6361/202143019. D. Elia et al.MNRAS, 504(2):2742–2766,

    work page doi:10.1051/0004-6361/202143019

  47. [47]

    doi: 10.1093/mnras/stab1038. D. Elia et al.ApJ, 941(2):162,

    work page doi:10.1093/mnras/stab1038

  48. [48]

    doi: 10.3847/1538-4357/aca27d. I. N. Evans et al.ApJSS, 274(2):22,

    work page doi:10.3847/1538-4357/aca27d

  49. [49]

    doi: 10.3847/1538-4365/ad6319. L. Eyer et al.A&A, 674:A13,

    work page doi:10.3847/1538-4365/ad6319

  50. [50]

    doi: 10.1051/0004-6361/202244242. R. Franco-Hernández and L. F. Rodríguez.ApJL, 604(2):L105–L108,

    work page doi:10.1051/0004-6361/202244242

  51. [51]

    A.Frank etal

    doi: 10.1086/386282. A.Frank etal. InH.Beuther, R. S.Klessen, C.P. Dullemond, andT.Henning, editors,Protostars andPlanetsVI, pages 451–474,

    work page doi:10.1086/386282

  52. [52]

    doi: 10.2458/azu_uapress_9780816531240-ch020. S. Freund et al.A&A, 664:A105,

    work page doi:10.2458/azu_uapress_9780816531240-ch020

  53. [53]

    32 The 10-15 GHz radio continuum survey of the GP with SKAO A

    doi: 10.1051/0004-6361/202142573. 32 The 10-15 GHz radio continuum survey of the GP with SKAO A. Traficante et al. Gaia Collaboration et al.A&A, 674:A41, 2023a. doi: 10.1051/0004-6361/202243232. Gaia Collaboration et al.A&A, 674:A1, 2023b. doi: 10.1051/0004-6361/202243940. R. Galván-Madrid, L. F. Rodríguez, P. T. P. Ho, and E. Keto.ApJL, 674(1):L33,

    work page doi:10.1051/0004-6361/202142573

  54. [54]

    doi: 10.1086/528957. R. Galván-Madrid et al.ApJSS, 274(1):15,

    work page doi:10.1086/528957

  55. [55]

    doi: 10.3847/1538-4365/ad61e6. E. C. Gardiner et al.ApJ, 967(2):145,

    work page doi:10.3847/1538-4365/ad61e6

  56. [56]

    doi: 10.3847/1538-4357/ad39e1. S. Geen, P. Hennebelle, P. Tremblin, and J. Rosdahl.MNRAS, 454(4):4484–4502, 2015a. doi: 10.1093/mnras/stv2272. S. Geen et al.MNRAS, 448(4):3248–3264, 2015b. doi: 1093/mnras/stv251. S. Goedhart et al.MNRAS, 531(1):649–681,

    work page doi:10.3847/1538-4357/ad39e1

  57. [57]

    doi: 10.1093/mnras/stae1166. P. F. Goldsmith, U. A. Yıldız, W. D. Langer, and J. L. Pineda.ApJ, 814(2):133,

    work page doi:10.1093/mnras/stae1166

  58. [58]

    doi: 10.1086/590229. M. González-Avilés, S. Lizano, and A. C. Raga.ApJ, 621(1):359–371,

    work page doi:10.1086/590229

  59. [59]

    doi: 10.1086/427470. D. A. Green.Journal of Astrophysics and Astronomy, 46(1):14,

    work page doi:10.1086/427470

  60. [60]

    doi: 10.1007/s12036-024-10038-4. J. A. Green et al.MNRAS, 392(2):783–794,

    work page doi:10.1007/s12036-024-10038-4

  61. [61]

    doi: 10.1111/j.1365-2966.2008.14091.x. M. Y. Grudić et al.MNRAS, 512(1):216–232,

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

  62. [62]

    doi: 10.1093/mnras/stac526. A. Hacar et al. In S. Inutsuka et al., editors,Protostars and Planets VII, volume 534 ofAstronomical Society of the Pacific Conference Series, page 153,

    work page doi:10.1093/mnras/stac526

  63. [63]

    doi: 10.48550/arXiv.2203.09562. D. J. Helfand et al.AJ, 131(5):2525–2537,

    work page doi:10.48550/arxiv.2203.09562

  64. [64]

    doi: 10.1086/503253. P. Hennebelle and M. Y. Grudić.ARA&A, 62(1):63–111,

    work page doi:10.1086/503253

  65. [65]

    doi: 10.1146/annurev-astro-052622-031748. M. G. Hoare et al. In B. Reipurth, D. Jewitt, and K. Keil, editors,Protostars and Planets V, page 181,

    work page doi:10.1146/annurev-astro-052622-031748

  66. [66]

    doi: 10.48550/arXiv.astro-ph/0603560. M. G. Hoare et al.PASP, 124(919):939,

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0603560

  67. [67]

    doi: 10.1086/668058. P. F. Hopkins et al.MNRAS, 491(3):3702–3729,

    work page doi:10.1086/668058

  68. [68]

    doi: 10.1093/mnras/stz3129. A. Ingallinera et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1093/mnras/stz3129

  69. [69]

    doi: 10.1093/mnras/stad005. K. Ishihara et al.ApJ, 974(1):95,

    work page doi:10.1093/mnras/stad005

  70. [70]

    doi: 10.3847/1538-4357/ad630f. N. Izumi et al.ApJ, 963(2):163,

    work page doi:10.3847/1538-4357/ad630f

  71. [71]

    doi: 10.3847/1538-4357/ad18c6. J. M. Jackson et al.ApJSS, 163(1):145,

    work page doi:10.3847/1538-4357/ad18c6

  72. [72]

    doi: 10.1086/500091. J. M. Jackson et al.PASA, 30:e057,

    work page doi:10.1086/500091

  73. [73]

    doi: 10.1017/pasa.2013.37. D. T. Jaffe and J. Martín-Pintado.ApJ, 520(1):162–172,

    work page doi:10.1017/pasa.2013.37 2013

  74. [74]

    doi: 10.1086/307440. A. Karska et al.A&A, 697:A186,

    work page doi:10.1086/307440

  75. [75]

    doi: 10.1051/0004-6361/202453109. A. Karska et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202453109

  76. [76]

    doi: 10.1086/379545. S. Khan et al.A&A, 689:A81,

    work page doi:10.1086/379545

  77. [77]

    doi: 10.1051/0004-6361/202449390. K.-T. Kim and B.-C. Koo.ApJ, 549(2):979–996,

    work page doi:10.1051/0004-6361/202449390

  78. [78]

    Klassen, T

    M. Klassen, T. Peters, and R. E. Pudritz.ApJ, 758(2):137, 2012a. doi: 10.1088/0004-637X/758/2/137. M. Klassen, R. E. Pudritz, and T. Peters.MNRAS, 421(4):2861–2871, 2012b. doi: 10.1111/j.1365-2966.2012.20523.x. A. Koley et al.A&A, 702:A133,

    work page doi:10.1088/0004-637x/758/2/137 2012

  79. [79]

    doi: 10.1051/0004-6361/202553830. M. S. N. Kumar, P. Palmeirim, D. Arzoumanian, and S. I. Inutsuka.A&A, 642:A87,

    work page doi:10.1051/0004-6361/202553830

  80. [80]

    doi: 10.1051/0004-6361/ 202038232. S. Kurtz. In R. Cesaroni, M. Felli, E. Churchwell, and M. Walmsley, editors,Massive Star Birth: A Crossroads of Astrophysics, volume 227 ofIAU Symposium, pages 111–119,

    work page doi:10.1051/0004-6361/

Showing first 80 references.