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arxiv: 2606.25901 · v1 · pith:JAP3ORJCnew · submitted 2026-06-24 · 🌌 astro-ph.GA

Spectroscopic surveys with the SKA probing the ionized and molecular Milky Way

A. Karska , J.R. Dawson , A.M. Jacob , T.V. Wenger , J.S. Urquhart , D. Colombo , L.D. Anderson , V.S. Veena
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M. Rugel M.A. Thompson P.D. Klaassen H. Beuther M.P. Busch A. Traficante G. Sabatini
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Pith reviewed 2026-06-25 19:57 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords SKAMilky Wayinterstellar mediummolecular cloudsradio recombination linesstar formationOHH2CO
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The pith

SKA spectroscopic surveys will map small molecules and ionized gas across the Milky Way to trace star formation conditions.

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

The paper argues that radio line surveys with the SKA can observe OH, CH, H2CO, and radio recombination lines in both the inner and outer Galactic disk. These observations would reveal how molecular clouds form, how warm ionized gas is distributed, and how CO-dark molecular gas affects star formation across varying densities and metallicities. A sympathetic reader would see this as using the Milky Way as a detailed template for understanding the interstellar medium and star formation in other galaxies. The work focuses on the unique wide-field and sensitivity capabilities that allow such deep surveys for the first time.

Core claim

Deep, wide-field SKA observations of small molecules and recombination lines toward the inner and outer Galaxy will constrain the processes forming molecular clouds, the structure of HII regions, and the role of CO-dark gas in star formation, providing a local template for galaxy evolution studies.

What carries the argument

Spectroscopic surveys of small molecules (OH, CH, H2CO) and radio recombination lines, which probe the transition from atomic to molecular phases and the properties of ionized gas across density and metallicity gradients.

If this is right

  • OH and CH surveys would directly measure the formation rate of molecular clouds in low-density regimes.
  • Radio recombination line maps would trace the large-scale structure of ionized gas and HII regions throughout the disk.
  • H2CO observations would quantify the contribution of CO-dark gas to the total molecular reservoir and its link to star formation efficiency.
  • The combined dataset would calibrate relations between ISM phases and star formation rates that can be applied to distant galaxies.

Where Pith is reading between the lines

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

  • Such surveys could test whether the Milky Way's metallicity gradient produces measurable changes in molecular formation pathways compared to metal-poor systems.
  • The same line data might allow kinematic separation of spiral arm and inter-arm gas on scales not previously accessible at these frequencies.
  • If successful, the approach would prioritize SKA time allocation toward wide shallow fields rather than deep targeted pointings for ISM studies.

Load-bearing premise

The SKA will achieve the sensitivity, angular resolution, and wide-field coverage needed to detect these lines in sufficient numbers across the full Galactic disk.

What would settle it

If SKA observations of the proposed fields detect far fewer OH or H2CO lines than predicted by current models of cloud formation, or fail to map recombination lines at the expected spatial scales, the case for unique new insights into ISM conditions would not hold.

Figures

Figures reproduced from arXiv: 2606.25901 by A. Karska, A.M. Jacob, A. Traficante, D. Colombo, G. Sabatini, H. Beuther, J.R. Dawson, J.S. Urquhart, L.D. Anderson, M.A. Thompson, M.P. Busch, M. Rugel, P.D. Klaassen, T.V. Wenger, V.S. Veena.

Figure 1
Figure 1. Figure 1: The primary scientific goals of this work are illustrated here, highlighting the multi-scale and multi-physics impact of spectral line surveys. from the Galactic center to the inner and outer Galaxy (𝑅Gal > 8.2 kpc; GRAVITY Collaboration et al. 2019). In particular, the gradual decrease in metallicity (e.g., Méndez-Delgado et al., 2022) results in reduced abundances of dust and molecules heavier than H2 in… view at source ↗
Figure 2
Figure 2. Figure 2: Schematic illustrating the lifecycle of baryonic material in the ISM, tracing its evolution from diffuse atomic gas to molecular clouds, the collapse into dense star-forming regions, the birth and evolution of massive stars, and their eventual return of enriched material back to the ISM. 2.1 From cold atomic to molecular gas In the interests of clarity, we will begin by defining terminology. The term ‘cold… view at source ↗
Figure 3
Figure 3. Figure 3: Radial distribution of CO-dark molecular gas column density in the plane of the Milky Way as traced by varied tracers including [C ii] (pink diamonds), CH (blue circles), and OH (orange circles) alongside the total H2 column density as traced by CO (gray squares). The spiral arm crossings, typically encountered along the line of sight toward a background continuum source in the fourth Galactic quadrant, ar… view at source ↗
Figure 4
Figure 4. Figure 4: Galactic longitude, latitude, and LSR velocity (𝑉LSR) distribution of 2,582 spectroscopic ionized gas measurements associated with 2,351 Galactic H ii regions in the WISE Catalog of Galactic H ii Regions (Anderson et al., 2014). An additional 21 measurements with |𝑉LSR| > 150 km s−1 toward 20 nebulae (one at a Galactic longitude near ℓ = 7.70◦ , the rest near ℓ = 358.75◦ ) are excluded for clarity. Along s… view at source ↗
Figure 5
Figure 5. Figure 5: Galactic environments spanning the metallicity and dynamical diversity of the Milky Way, so far observed only in the CO-bright gas, forming the target sample for the proposed SKA line survey. Clockwise from top-left: high-velocity gas stream tracing bar-driven inflow in the Central Molecular Zone (Veena et al., 2024); an HVC toward the northern lobe of the nuclear outflow (Noon et al., 2023); the G195.722-… view at source ↗
Figure 6
Figure 6. Figure 6: Simulated detection rate for OH absorption over a 600 square-degree SKA survey of the Galactic Plane. The simulated data is generated as described in the text. This treatment considers only the brightest position toward a simulated source, and is in that sense a lower limit. For extended bright sources, mul￾tiple/resolved detections are likely; for extended weak sources, integrating spatially to improve se… view at source ↗
Figure 7
Figure 7. Figure 7: Schematic showing the RRLs within the SKA Bands 2 and 5b. The blue and red lines show the frequencies of the H𝛼 and H𝛽 lines respectively. There are 36 H𝛼 RRLs in Band 2 (beige shaded region) and 17 H𝛼 RRLs in band 5b (pink shaded region). The sensitivities in Band 2 can be improved by stacking RRLs ( [PITH_FULL_IMAGE:figures/full_fig_p023_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Left Panel: Predicted flux densities for the three most compact H ii region stages. The solid and dashed lines show the continuum and RRL fluxes respectively. The bright magenta and cyan bars show the sensitivity to RRLs estimated from the SKA sensitivity calculator assuming a 600 second integration, robust weighting of 1 and channel width of ∼3.5 and 4.5 km s−1 . The pale magenta and cyan bars show the im… view at source ↗
read the original abstract

Radio spectroscopic surveys provide us with a comprehensive picture of the Milky Way across many physical and chemical regimes. Spectral lines primarily probe the multi-phase gaseous interstellar medium (ISM) from its ionized to atomic and molecular phases, and constrain both local and galaxy-scale kinematics and structure through Doppler shifts. By investigating the physical and chemical properties and distribution of the ISM, the processes driving star formation and galaxy evolution can be studied in detail. This motivates line surveys of our Galaxy that allow us to use the range of physical conditions found in the Milky Way as a template for understanding star formation in extragalactic environments. In this chapter, we describe the science enabled by the spectroscopy of small molecules and radio recombination lines of atoms toward a range of Galactic environments with the SKA. We address questions concerning the processes that dictate the formation of molecular clouds (OH, CH), the properties of warm, ionized gas and the potential of HII regions in understanding the structure of the Galaxy (radio recombination lines), and the impact of CO-dark molecular gas across various density regimes on star formation and galaxy evolution (OH, H2CO). We propose a survey that includes the inner and outer Galaxy disk, characterized by a broad range of densities, temperatures, and metallicities. Deep, wide-field observations of small molecules will be uniquely accessible with SKA, providing key insights on the condition of interstellar medium in galaxies and its impact on star formation.

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

2 major / 1 minor

Summary. The manuscript presents a forward-looking science case for radio spectroscopic surveys with the Square Kilometre Array (SKA) targeting small molecules (OH, CH, H2CO) and radio recombination lines across the inner and outer Milky Way disk. It argues that such observations will probe molecular cloud formation, properties of warm ionized gas and HII regions, the role of CO-dark molecular gas, and their collective impact on star formation, using the Milky Way's range of conditions as a template for extragalactic environments. The central claim is that deep, wide-field observations of these tracers will be uniquely accessible with the SKA.

Significance. If the SKA realizes the required sensitivity, resolution, and wide-field survey speed, the proposed observations could deliver new constraints on multi-phase ISM physics and star-formation processes that are difficult to obtain with existing facilities, thereby strengthening the Milky Way as a local benchmark for galaxy evolution studies.

major comments (2)
  1. [Abstract] Abstract: the assertion that deep, wide-field observations of small molecules 'will be uniquely accessible with SKA' is load-bearing for the central claim yet is unsupported by any quantitative comparison of SKA sensitivity, survey speed, or resolution against current or planned instruments (e.g., MeerKAT, ngVLA, or ALMA).
  2. [Full text (survey proposal section)] Science-case description: no survey parameters (integration time per field, total sky coverage, expected line sensitivities, or detection-rate estimates) are supplied for the proposed inner- and outer-disk observations, leaving the feasibility of the 'deep, wide-field' program unquantified.
minor comments (1)
  1. The manuscript would benefit from a concise table listing the key transitions (rest frequencies, critical densities) of OH, CH, H2CO, and the recombination lines discussed.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the positive overall assessment and the specific comments, which help strengthen the presentation of the science case. We address each major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that deep, wide-field observations of small molecules 'will be uniquely accessible with SKA' is load-bearing for the central claim yet is unsupported by any quantitative comparison of SKA sensitivity, survey speed, or resolution against current or planned instruments (e.g., MeerKAT, ngVLA, or ALMA).

    Authors: We agree that the uniqueness claim benefits from explicit quantitative support. In the revised manuscript we will insert a short paragraph (or table) in the abstract or introduction that compares SKA1-MID expected line sensitivities, survey speed, and field-of-view at the relevant frequencies (1–10 GHz) against MeerKAT, ngVLA, and ALMA for the OH, CH, and H2CO transitions, thereby grounding the statement. revision: yes

  2. Referee: [Full text (survey proposal section)] Science-case description: no survey parameters (integration time per field, total sky coverage, expected line sensitivities, or detection-rate estimates) are supplied for the proposed inner- and outer-disk observations, leaving the feasibility of the 'deep, wide-field' program unquantified.

    Authors: The chapter is written as a high-level science motivation rather than a technical proposal. We nevertheless accept that indicative numbers improve credibility. We will add a concise new subsection that supplies order-of-magnitude estimates for integration time per pointing, total area, 5-sigma line sensitivities, and rough detection-rate expectations derived from SKA1-MID specifications and existing pilot data. revision: yes

Circularity Check

0 steps flagged

No circularity: descriptive proposal with no derivations or equations

full rationale

The document is a forward-looking science-case proposal chapter. It contains no equations, derivations, fitted parameters, predictions, or load-bearing self-citations. Claims rest on anticipated SKA instrument performance rather than any internal chain that reduces to its own inputs. No steps meet the criteria for circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the domain assumption that SKA performance will enable the described observations and that the listed spectral lines will yield the stated physical insights; no free parameters or invented entities are introduced.

axioms (1)
  • domain assumption SKA will enable unique deep wide-field observations of small molecules and recombination lines
    Invoked when stating that such observations will be uniquely accessible and provide key ISM insights.

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Works this paper leans on

188 extracted references · 186 canonical work pages · 2 internal anchors

  1. [1]

    doi: 10.1051/0004-6361/200913474. W. S. Adams. ApJ, 93:11, Jan

    work page doi:10.1051/0004-6361/200913474

  2. [2]

    doi: 10.1086/144237. R. J. Allen, M. Ivette Rodríguez, J. H. Black, and R. S. Booth. AJ, 143(4):97, Apr

    work page doi:10.1086/144237

  3. [3]

    doi: 10.1088/0004-6256/143/ 4/97. R. J. Allen, D. E. Hogg, and P. D. Engelke. AJ, 149(4):123, Apr

    work page doi:10.1088/0004-6256/143/

  4. [4]

    doi: 10.1088/0004-6256/149/4/123. K. R. Anantharamaiah.Journal of Astrophysics and Astronomy, 7(3):131–139, Sept

    work page doi:10.1088/0004-6256/149/4/123

  5. [5]

    doi: 10.1007/BF02714206. L. D. Anderson and T. M. Bania. ApJ, 690:706–719, Jan

    work page doi:10.1007/bf02714206

  6. [6]

    doi: 10.1088/0004-637X/690/1/706. L. D. Anderson, T. M. Bania, D. S. Balser, and R. T. Rood. ApJ, 754:62, July

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

  7. [7]

    doi: 10.1088/0004-637X/754/1/62. L. D. Anderson et al. ApJS, 212:1, May

    work page doi:10.1088/0004-637x/754/1/62

  8. [8]

    doi: 10.1088/0067-0049/212/1/1. L. D. Anderson et al. ApJS, 221:26, Dec. 2015a. doi: 10.1088/0067-0049/221/2/26. L. D. Anderson et al. ApJ, 810:42, Sept. 2015b. doi: 10.1088/0004-637X/810/1/42. L. D. Anderson et al. ApJS, 254(2):28, June

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

  9. [9]

    doi: 10.3847/1538-4365/abef65. P. André et al. In H. Beuther, R. S. Klessen, C. P. Dullemond, and T. Henning, editors,Protostars and Planets VI, page 27, Jan

    work page doi:10.3847/1538-4365/abef65

  10. [10]

    doi: 10.2458/azu\_uapress\_9780816531240-ch002. E. M. Arnal and W. M. Goss. A&A, 145:369–376, Apr

    work page doi:10.2458/azu

  11. [11]

    doi: 10.1051/0004-6361/201116596. A. Asensio Ramos and M. Elitzur. A&A, 616:A131, Sept

    work page doi:10.1051/0004-6361/201116596

  12. [12]

    doi: 10.1051/0004-6361/201731943. E. Audit and P. Hennebelle. A&A, 433(1):1–13, Apr

    work page doi:10.1051/0004-6361/201731943

  13. [13]

    doi: 10.1051/0004-6361:20041474. T. M. Bania et al. ApJ, 972(2):192, Sept

    work page doi:10.1051/0004-6361:20041474

  14. [14]

    doi: 10.3847/1538-4357/ad5f8b. J. E. Barnes, K. Wood, A. S. Hill, and L. M. Haffner. MNRAS, 447:559–566, Feb

    work page doi:10.3847/1538-4357/ad5f8b

  15. [15]

    L.Barriault,G.Joncas,F.J.Lockman,andP.G.Martin.MNRAS,407:2645–2659,Oct.2010.doi: 10.1111/j.1365-2966

    doi: 10.1093/mnras/stu2454. L.Barriault,G.Joncas,F.J.Lockman,andP.G.Martin.MNRAS,407:2645–2659,Oct.2010.doi: 10.1111/j.1365-2966. 2010.17105.x. E. Bellomi et al. A&A, 643:A36, Nov

    work page doi:10.1093/mnras/stu2454 2010

  16. [16]

    doi: 10.1051/0004-6361/202038593. H. Beuther et al. A&A, 595:A32, Oct

    work page doi:10.1051/0004-6361/202038593

  17. [17]

    doi: 10.1051/0004-6361/201629143. H. Beuther et al. A&A, 628:A90, Aug

    work page doi:10.1051/0004-6361/201629143

  18. [18]

    doi: 10.1051/0004-6361/201935936. S. Bialy, B. Burkhart, and A. Sternberg. ApJ, 843(2):92, July

    work page doi:10.1051/0004-6361/201935936

  19. [19]

    doi: 10.3847/1538-4357/aa7854. T. G. Bisbas, P. P. Papadopoulos, and S. Viti. ApJ, 803(1):37, Apr

    work page doi:10.3847/1538-4357/aa7854

  20. [20]

    doi: 10.1088/0004-637X/803/1/37. L. Blitz and E. Rosolowsky. ApJ, 650:933–944, Oct

    work page doi:10.1088/0004-637x/803/1/37

  21. [21]

    doi: 10.1086/505417. J. B. G. M. Bloemen. ApJ, 317:L15, June

    work page doi:10.1086/505417

  22. [22]

    doi: 10.1086/184904. T. L. Bourke et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1086/184904

  23. [23]

    org/abs/1912.12699

    URLhttps://arxiv. org/abs/1912.12699. L. Bronfman et al. ApJ, 324:248, Jan

    arXiv 1912

  24. [24]

    doi: 10.1086/165892. C. Brown, J. M. Dickey, J. R. Dawson, and N. M. McClure-Griffiths. ApJS, 211(2):29, Apr

    work page doi:10.1086/165892

  25. [25]

    doi: 10.1086/344796. A. Brunthaler et al. A&A, 651:A85, July

    work page doi:10.1086/344796

  26. [26]

    doi: 10.1051/0004-6361/202039856. M. P. Busch.ApJ, 967:148, 5

    work page doi:10.1051/0004-6361/202039856

  27. [27]

    doi: 10.3847/1538-4357/AD3AF6

    ISSN 0004-637X. doi: 10.3847/1538-4357/AD3AF6. URL https://iopscience.iop.org/article/10.3847/1538-4357/ad3af6https://iopscience.iop.org/ article/10.3847/1538-4357/ad3af6/meta. M. P. Busch et al. ApJ, 883(2):158, Oct

    work page doi:10.3847/1538-4357/ad3af6

  28. [28]

    doi: 10.3847/1538-4357/ab3a4b. M. P. Busch, P. D. Engelke, R. J. Allen, and D. E. Hogg. ApJ, 914(1):72, June

    work page doi:10.3847/1538-4357/ab3a4b

  29. [29]

    doi: 10.3847/1538-4357/abf832. E. Cappellazzo et al. ApJ, 996(1):15, Jan

    work page doi:10.3847/1538-4357/abf832

  30. [30]

    doi: 10.3847/1538-4357/ae1970. M. Chevance et al. MNRAS, 494(4):5279–5292, June

    work page doi:10.3847/1538-4357/ae1970

  31. [31]

    doi: 10.1093/mnras/staa1106. S. E. Clark, J. E. G. Peek, and M. A. Miville-Deschênes. ApJ, 874(2):171, Apr

    work page doi:10.1093/mnras/staa1106

  32. [32]

    doi: 10.3847/1538-4357/ab0b3b. D. Colombo et al. MNRAS, 475(2):1791–1808, Apr

    work page doi:10.3847/1538-4357/ab0b3b

  33. [33]

    doi: 10.1093/mnras/stx3233. D. Colombo et al. A&A, 644:A97, Dec

    work page doi:10.1093/mnras/stx3233

  34. [34]

    doi: 10.1051/0004-6361/202039005. D. Colombo et al. A&A, 655:L2, Nov

    work page doi:10.1051/0004-6361/202039005

  35. [35]

    doi: 10.1051/0004-6361/202142182. D. Colombo et al. A&A, 658:A54, Feb

    work page doi:10.1051/0004-6361/202142182

  36. [36]

    doi: 10.1051/0004-6361/202141287. D. Colombo et al. A&A, 699:A367, July

    work page doi:10.1051/0004-6361/202141287

  37. [37]

    27 The ionized and molecular Milky Way Karska et al

    doi: 10.1051/0004-6361/202453217. 27 The ionized and molecular Milky Way Karska et al. D. P. Cox and B. W. Smith. ApJ, 189:L105, May

    work page doi:10.1051/0004-6361/202453217

  38. [38]

    doi: 10.1086/181476. P. J. Dagdigian. MNRAS, 475(4):5480–5486, Apr

    work page doi:10.1086/181476

  39. [39]

    doi: 10.1093/mnras/sty193. J. Darling and B. Zeiger. ApJ, 749(2):L33, Apr

    work page doi:10.1093/mnras/sty193

  40. [40]

    doi: 10.1088/2041-8205/749/2/L33. J. R. Dawson et al. MNRAS, 439(2):1596–1614, Apr

    work page doi:10.1088/2041-8205/749/2/l33 2041

  41. [41]

    doi: 10.1093/mnras/stu032. J. R. Dawson et al. MNRAS, 512(3):3345–3364, May

    work page doi:10.1093/mnras/stu032

  42. [42]

    doi: 10.1093/mnras/stac636. J. R. Dawson, S. L. Breen, and Gaskap-Oh Team. In T. Hirota, H. Imai, K. Menten, and Y. Pihlström, editors,Cosmic Masers: ProperMotionTowardtheNext-GenerationLargeProjects,volume380ofIAUSymposium,pages486–490, Jan

    work page doi:10.1093/mnras/stac636

  43. [43]

    doi: 10.1017/S1743921323002405. E. M. Di Teodoro et al. ApJ, 855(1):33, Mar

    work page doi:10.1017/s1743921323002405

  44. [44]

    doi: 10.3847/1538-4357/aaad6a. J. M. Dickey and F. J. Lockman. ARA&A, 28:215–261, Jan

    work page doi:10.3847/1538-4357/aaad6a

  45. [45]

    doi: 10.1146/annurev.aa.28.090190.001243. B. T. Draine and F. Bertoldi. ApJ, 468:269, Sept

    work page doi:10.1146/annurev.aa.28.090190.001243

  46. [46]

    doi: 10.1086/177689. A. Duarte-Cabral et al. MNRAS, 500(3):3027–3049, Jan. 2021a. doi: 10.1093/mnras/staa2480. A. Duarte-Cabral et al. The SEDIGISM survey: molecular clouds in the inner Galaxy. Monthly Notices of the Royal Astronomical Society, Volume 500, Issue 3, pp.3027-3049, Jan. 2021b. Y. Ebisawa, N. Sakai, K. M. Menten, and S. Yamamoto. ApJ, 871(1):89, Jan

    work page doi:10.1086/177689

  47. [47]

    doi: 10.3847/1538-4357/aaf72b. D. J. Eden et al. MNRAS, 431(2):1587–1595, May

    work page doi:10.3847/1538-4357/aaf72b

  48. [48]

    doi: 10.1093/mnras/stt279. F. Egusa, A. Hirota, J. Baba, and K. Muraoka. ApJ, 854(2):90, Feb

    work page doi:10.1093/mnras/stt279

  49. [49]

    doi: 10.3847/1538-4357/aaa76d. D. Elia et al. MNRAS, 471:100–143, Oct

    work page doi:10.3847/1538-4357/aaa76d

  50. [50]

    doi: 10.1093/mnras/stx1357. D. Elia et al. MNRAS, 504(2):2742–2766, June

    work page doi:10.1093/mnras/stx1357

  51. [51]

    doi: 10.1093/mnras/stab1038. B. G. Elmegreen. ApJ, 338:178–196, Mar

    work page doi:10.1093/mnras/stab1038

  52. [52]

    doi: 10.1086/167192. C. P. Endres et al.Journal of Molecular Spectroscopy, 327:95–104, Sept

    work page doi:10.1086/167192

  53. [53]

    doi: 10.1016/j.jms.2016.03.005. N. J. Evans, II, M. L. Kutner, and L. G. Mundy. ApJ, 323:145, Dec

    work page doi:10.1016/j.jms.2016.03.005 2016

  54. [54]

    doi: 10.1086/165814. Y. Gao and P. M. Solomon. ApJ, 606(1):271–290, May

    work page doi:10.1086/165814

  55. [55]

    doi: 10.1086/382999. Y. M. Georgelin and Y. P. Georgelin. A&A, 49:57–79, May

    work page doi:10.1086/382999

  56. [56]

    doi: 10.1051/0004-6361/202449152. S. J. Gibson, A. R. Taylor, L. A. Higgs, and P. E. Dewdney. ApJ, 540(2):851–862, Sept

    work page doi:10.1051/0004-6361/202449152

  57. [57]

    doi: 10.1086/309364. D. Gigli et al. A&A, 704:A171, Dec

    work page doi:10.1086/309364

  58. [58]

    doi: 10.1051/0004-6361/202555956. A. Ginsburg et al. ApJ, 736(2):149, Aug

    work page doi:10.1051/0004-6361/202555956

  59. [59]

    doi: 10.1088/0004-637X/736/2/149. A. Ginsburg et al. A&A, 573:A106, Jan

    work page doi:10.1088/0004-637x/736/2/149

  60. [60]

    doi: 10.1051/0004-6361/201424979. S. C. O. Glover and P. C. Clark. MNRAS, 426:377–388, Oct

    work page doi:10.1051/0004-6361/201424979

  61. [61]

    doi: 10.1111/j.1365-2966.2012.21737.x. S. C. O. Glover and M.-M. Mac Low. ApJ, 659(2):1317–1337, Apr

    work page doi:10.1111/j.1365-2966.2012.21737.x 2012

  62. [62]

    doi: 10.1086/512227. S. C. O. Glover and M. M. Mac Low. MNRAS, 412(1):337–350, Mar

    work page doi:10.1086/512227

  63. [63]

    doi: 10.1111/j.1365-2966.2010.17907.x. P. F. Goldsmith, D. Li, and M. Krčo. ApJ, 654(1):273–289, Jan

    work page doi:10.1111/j.1365-2966.2010.17907.x 2010

  64. [64]

    doi: 10.1086/509067. P. F. Goldsmith, U. A. Yıldız, W. D. Langer, and J. L. Pineda. ApJ, 814(2):133, Dec

    work page doi:10.1086/509067

  65. [65]

    doi: 10.1088/0004-637X/ 814/2/133. Y. Gong et al. A&A, 678:A130, Oct

    work page doi:10.1088/0004-637x/

  66. [66]

    doi: 10.1051/0004-6361/202346102. S. R. Gramze et al. ApJ, 959(2):93, Dec

    work page doi:10.1051/0004-6361/202346102

  67. [67]

    GRAVITY Collaboration et al

    doi: 10.3847/1538-4357/ad01be. GRAVITY Collaboration et al. A&A, 625:L10, May

    work page doi:10.3847/1538-4357/ad01be

  68. [68]

    I.A.Grenier,J.-M.Casandjian,andR.Terrier.Science,307(5713):1292–1295,Feb.2005.doi: 10.1126/science.1106924

    doi: 10.1051/0004-6361/201935656. I.A.Grenier,J.-M.Casandjian,andR.Terrier.Science,307(5713):1292–1295,Feb.2005.doi: 10.1126/science.1106924. J. Guibert, N. Q. Rieu, and M. Elitzur. A&A, 66(3):395–405, June

    work page doi:10.1051/0004-6361/201935656 2005

  69. [69]

    doi: 10.48550/arXiv.2203.09562. L. M. Haffner et al. ApJS, 149:405–422, Dec

    work page doi:10.48550/arxiv.2203.09562

  70. [70]

    doi: 10.1086/378850. L. M. Haffner et al.Reviews of Modern Physics, 81:969–997, July

    work page doi:10.1086/378850

  71. [71]

    doi: 10.1103/RevModPhys.81.969. A. Hafner, J. R. Dawson, and M. Wardle. MNRAS, 497(4):4066–4076, Oct

    work page doi:10.1103/revmodphys.81.969

  72. [72]

    doi: 10.1093/mnras/staa2234. A. Hafner et al. PASA, 40:e015, Apr

    work page doi:10.1093/mnras/staa2234

  73. [73]

    doi: 10.1017/pasa.2023.8. H. P. Hatchfield et al. ApJS, 251(1):14, Nov

    work page doi:10.1017/pasa.2023.8 2023

  74. [74]

    doi: 10.3847/1538-4365/abb610. C. Heiles. In C. E. Woodward, M. D. Bicay, and J. M. Shull, editors,Tetons 4: Galactic Structure, Stars and the Interstellar Medium, volume 231 ofAstronomical Society of the Pacific Conference Series, page 294, Jan

    work page doi:10.3847/1538-4365/abb610

  75. [75]

    doi: 10.48550/arXiv.astro-ph/0010047. C. Heiles and T. H. Troland. ApJ, 586(2):1067–1093, Apr

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0010047

  76. [76]

    doi: 10.1086/367828. J. D. Henshaw et al. In S. Inutsuka et al., editors,Protostars and Planets VII, volume 534 ofAstronomical Society of the 28 The ionized and molecular Milky Way Karska et al. Pacific Conference Series, page 83, July

    work page doi:10.1086/367828

  77. [77]

    doi: 10.48550/arXiv.2203.11223. M. Heyer and T. M. Dame. ARA&A, 53:583–629, Aug

    work page doi:10.48550/arxiv.2203.11223

  78. [78]

    doi: 10.1146/annurev-astro-082214-122324. L. M. Hogarth et al. MNRAS, 528(4):6768–6785, Mar

    work page doi:10.1146/annurev-astro-082214-122324

  79. [79]

    doi: 10.1093/mnras/stae377. L. Hou et al.Science China Physics, Mechanics, and Astronomy, 65(12):129703, Dec

    work page doi:10.1093/mnras/stae377

  80. [80]

    doi: 10.1007/ s11433-022-2039-8. L. G. Hou and J. L. Han. A&A, 569:A125, Sept

    2039

Showing first 80 references.