pith. sign in

arxiv: 2606.25607 · v1 · pith:UISDPL7Gnew · submitted 2026-06-24 · 🌌 astro-ph.SR · astro-ph.HE

Evolved massive stars and their impact on their environment

C.S. Buemi , G. Umana , C. Trigilio , C. Bordiu , F. Bufano , J. van den Eijnden , S. Orlando , P. Leto
show 10 more authors
F. Bocchino M. Miceli M. P\'erez-Torres A. Alberdi F. Cavallaro L. Cerrigone A. Ingallinera S. Loru S. Riggi A.C. Ruggeri
This is my paper

Pith reviewed 2026-06-25 19:22 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords evolved massive starscircumstellar environmentstellar windssupernovaeSquare Kilometre Arraymass lossWolf-Rayetluminous blue variables
0
0 comments X

The pith

The Square Kilometre Array will overcome observational limits on circumstellar environments of massive stars to connect them to supernovae.

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

This review paper establishes that the study of circumstellar environments around evolved massive stars is essential for understanding how stellar winds and mass loss shape the conditions for supernova explosions. It focuses on the transitional phases from red supergiants through luminous blue variables to Wolf-Rayet stars, where eruptive events create nebulae that interact with supernova ejecta. Current limitations in resolution and sensitivity prevent detailed characterization of these environments. The paper claims that the Square Kilometre Array's high spatial resolution, sensitivity, and wide frequency coverage will resolve these issues.

Core claim

The final stages of massive star evolution involve stellar winds and circumstellar environments that profoundly shape the surroundings in which supernovae explode. The Square Kilometre Array, with its high spatial resolution, sensitivity and wide frequency coverage, will address the most critical observational issues that currently prevent detailed characterization of circumstellar environments and thus limit our ability to constrain its connections to supernova and remnant properties.

What carries the argument

The Square Kilometre Array's capabilities in combining high spatial resolution, sensitivity, and wide frequency coverage for radio observations of circumstellar environments.

If this is right

  • Such characterization will directly prove the mass-loss activity of the star through wind and eruptive events.
  • The shaped environment will be shown to heavily affect supernovae spectrophotometric signatures through interaction with ejecta.
  • Constraints will be placed on connections between circumstellar environments and supernova remnant properties.
  • Understanding of pre-supernova progenitors will improve by focusing on their nebulae.

Where Pith is reading between the lines

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

  • Future SKA data could be used to model the specific mass-loss histories of individual massive stars.
  • Improved CSE characterization might help distinguish between different supernova types based on progenitor mass loss.
  • Connections to remnant properties could influence models of how massive stars contribute to interstellar medium enrichment.

Load-bearing premise

Overcoming current observational limitations on characterizing circumstellar environments will directly enable constraints on their connections to supernova and remnant properties.

What would settle it

If SKA observations of circumstellar environments around evolved massive stars do not yield new information that constrains their influence on supernova properties, the asserted benefit would not hold.

Figures

Figures reproduced from arXiv: 2606.25607 by A. Alberdi, A.C. Ruggeri, A. Ingallinera, C. Bordiu, C.S. Buemi, C. Trigilio, F. Bocchino, F. Bufano, F. Cavallaro, G. Umana, J. van den Eijnden, L. Cerrigone, M. Miceli, M. P\'erez-Torres, P. Leto, S. Loru, S. Orlando, S. Riggi.

Figure 1
Figure 1. Figure 1: WR 49-1 nebula as observed in SMGPS, compared with MeerKAT and SKA-Mid synthetic images. Left column, top row: SMGPS observation at 1.3 GHz (left) and best-fit model convolved with the corresponding MeerKAT beam (8′′, right). Left column, bottom row: Radial brightness profile with best￾fitting spherical shell model overlaid (left), and the unconvolved model image including an added compact central source (… view at source ↗
Figure 2
Figure 2. Figure 2: SKA detectability test for the WR 75ab nebula at extragalactic distances. Left column: SMGPS observation and best-fit model (same procedure as [PITH_FULL_IMAGE:figures/full_fig_p015_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Error on spectral index (𝜎𝛼) between SKA-Mid Band 2 (central frequency 1.31 GHz) and Band 5b (central frequency 11.85 GHz) as a function of integration time (sensitivity) for sources of different brightness levels (𝐵). Top panels refer to extended radio emission with positive spectral indices (𝐵1 < 𝐵2). Bottom panels refer to cases where the spectral indices of the brightness are negative (𝐵2 < 𝐵1). Colour… view at source ↗
Figure 4
Figure 4. Figure 4: The fraction of bow shocks expected to be detectable with SKA-mid (left) and SKA-low (right). We assume detection thresholds of ∼ 9/50 𝜇Jy for SKA-mid/low, respectively, versus typical detection thresholds in current surveys of ∼ 100/200/250 𝜇Jy for SMGPS/EMU/LOFAR. orders of magnitude and that, with the SKA, the measurement of these fractions can be used to test the assumptions made in calculating them. I… view at source ↗
read the original abstract

The comprehension of the final stages of massive star evolution and their path toward the eventual supernova explosion necessarily involves the study of stellar winds and the circumstellar environment (CSE) surrounding them in the transitional phases, during which stellar winds and eruptive mass loss profoundly shape the surrounding environment. The study of the pre-supernova progenitors, from Red Supergiants, passing through the Luminous Blue Variable stage to Wolf-Rayet stars, is of key importance because, focusing on their nebulae, they directly prove the mass-loss activity of the star that, through wind and eruptive events, shapes the environment in which the supernova will explode. Such environment, interacting with the ejecta, will heavily affect supernovae spectrophotometric signatures. The Square Kilometre Array, with its extraordinary capabilities to combine high spatial resolution, sensitivity and wide frequency coverage will adress the most critical observational issues that currently prevent detailed characterization of CSE and, thus limit our ability to constrain its connections to supernova and remnants proprierties.

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 manuscript claims that studying stellar winds and circumstellar environments (CSE) around evolved massive stars (Red Supergiants, Luminous Blue Variables, and Wolf-Rayet stars) is essential for understanding mass-loss activity and its effects on the environments in which supernovae explode. It further asserts that the Square Kilometre Array's combination of high spatial resolution, sensitivity, and wide frequency coverage will resolve current observational limitations on CSE characterization and thereby enable constraints on connections between CSE and supernova/remnant properties.

Significance. If the central linkage holds, the work could usefully flag an observational opportunity for SKA in massive-star and supernova-progenitor research. However, the absence of any data, derivations, error analysis, cited models, or concrete diagnostics means the significance is restricted to a qualitative call for future observations rather than a substantiated advance.

major comments (1)
  1. [Abstract] Abstract: The claim that SKA 'will adress the most critical observational issues that currently prevent detailed characterization of CSE and, thus limit our ability to constrain its connections to supernova and remnants proprierties' is unsupported. No mechanism, reference, or example is supplied showing how specific CSE observables (density profiles, kinematics, or abundances) would map onto supernova light-curve parameters or remnant morphologies; this 'thus' step is load-bearing for the paper's motivation yet remains an assertion without evidence.
minor comments (2)
  1. [Abstract] Abstract: Spelling and grammar errors ('adress' → 'address'; 'proprierties' → 'properties'). The second paragraph is a single run-on sentence whose logical structure is unclear.
  2. [Abstract] Abstract: The first paragraph contains a lengthy compound sentence that would benefit from splitting or rephrasing for readability.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their review. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The claim that SKA 'will adress the most critical observational issues that currently prevent detailed characterization of CSE and, thus limit our ability to constrain its connections to supernova and remnants proprierties' is unsupported. No mechanism, reference, or example is supplied showing how specific CSE observables (density profiles, kinematics, or abundances) would map onto supernova light-curve parameters or remnant morphologies; this 'thus' step is load-bearing for the paper's motivation yet remains an assertion without evidence.

    Authors: This is a perspective paper whose purpose is to flag an observational opportunity with SKA rather than to derive new mappings. The manuscript text already states that the CSE 'interacting with the ejecta, will heavily affect supernovae spectrophotometric signatures,' and the broader CSE-SN connection is supported by the existing literature on ejecta-CSM interaction. Nevertheless, we agree that the abstract would be strengthened by a brief concrete illustration. We will revise the abstract to include one short example (e.g., how a dense, asymmetric CSE can produce both enhanced early light-curve luminosity and asymmetric remnant morphology) together with a pointer to the relevant literature. This change will make the 'thus' step explicit without converting the paper into a review. revision: yes

Circularity Check

0 steps flagged

No circularity: purely descriptive claims with no derivations or self-referential reductions

full rationale

The manuscript is a perspective piece on massive-star mass loss and SKA prospects. It contains no equations, no fitted parameters, no derivation chain, and no load-bearing self-citations. The sole forward-looking assertion (“will address … and, thus limit our ability to constrain”) is an empirical claim about future instrumentation rather than a result obtained by substituting one expression for another or by renaming a fitted quantity. Because no step reduces to its own inputs by construction, the circularity score is 0.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The paper is a review relying on standard astrophysical domain knowledge about stellar evolution and mass loss; no free parameters, new axioms, or invented entities are introduced.

axioms (1)
  • domain assumption Mass loss via winds and eruptions from evolved massive stars shapes the circumstellar environment, which then interacts with supernova ejecta to affect observed properties.
    This premise is stated directly in the abstract as the basis for why CSE studies matter for supernovae.

pith-pipeline@v0.9.1-grok · 5794 in / 1238 out tokens · 37825 ms · 2026-06-25T19:22:09.820744+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

104 extracted references · 103 canonical work pages

  1. [1]

    doi: 10.1093/mnras/stw2986. P. Agrawal et al. MNRAS, 512(4):5717–5725, June

    work page doi:10.1093/mnras/stw2986

  2. [2]

    doi: 10.1093/mnras/stac930. F. Aharonian et al. A&A, 666:A124, Oct

    work page doi:10.1093/mnras/stac930

  3. [3]

    21 Evolved Massive Stars and Environment C

    doi: 10.1051/0004-6361/202244323. 21 Evolved Massive Stars and Environment C. Buemi et al. A. R. Bell. MNRAS, 182:147–156, Jan

    work page doi:10.1051/0004-6361/202244323

  4. [4]

    doi: 10.1093/mnras/182.2.147. P. Benaglia et al. A&A, 517:L10, July

    work page doi:10.1093/mnras/182.2.147

  5. [5]

    doi: 10.1051/0004-6361/201015232. A. Blaauw. Bull. Astron. Inst. Netherlands, 15:265, May

    work page doi:10.1051/0004-6361/201015232

  6. [6]

    InJ.Mackey,J.S.Vink,andN.St-Louis,editors, MassiveStarsNearandFar , volume361of IAUSymposium,pages447–453,Jan.2024a

    A.Z.Bonanosetal. InJ.Mackey,J.S.Vink,andN.St-Louis,editors, MassiveStarsNearandFar , volume361of IAUSymposium,pages447–453,Jan.2024a. doi: 10.1017/S1743921322002782. A. Z. Bonanos et al. A&A, 686:A77, June 2024b. doi: 10.1051/0004-6361/202348527. C. Bordiu, J. R. Rizzo, and A. Ritacco. MNRAS, 482(2):1651–1663, Jan

    work page doi:10.1017/s1743921322002782

  7. [7]

    doi: 10.1093/mnras/staa3606. C. Bordiu et al. ApJ, 939(2):L30, Nov

    work page doi:10.1093/mnras/staa3606

  8. [8]

    doi: 10.3847/2041-8213/ac9b10. C. Bordiu et al. A&A, 690:A53, Oct

    work page doi:10.3847/2041-8213/ac9b10 2041

  9. [9]

    doi: 10.1051/0004-6361/202450766. C. Bordiu et al. MNRAS, 543(4):3708–3730, Nov. 2025a. doi: 10.1093/mnras/staf1667. C. Bordiu et al. A&A, 695:A144, Mar. 2025b. doi: 10.1051/0004-6361/202450356. C. Buemi et al. High-resolution radio imaging of circumstellar nebulae around evolved massive stars. in preparation, 2026a. C. Buemi et al. Meerkat-gps view of wo...

    work page doi:10.1051/0004-6361/202450766

  10. [10]

    doi: 10.1088/0004-637X/721/2/1404. C. S. Buemi et al. MNRAS, 465(4):4147–4158, Mar

    work page doi:10.1088/0004-637x/721/2/1404

  11. [11]

    doi: 10.1093/mnras/stw3074. S. Burgemeister et al. MNRAS, 429(4):3305–3315, Mar

    work page doi:10.1093/mnras/stw3074

  12. [12]

    doi: 10.1093/mnras/sts588. M. Cano-González et al. A&A, 692:A23, Dec

    work page doi:10.1093/mnras/sts588

  13. [13]

    doi: 10.1051/0004-6361/202451771. M. Cano-González et al. A&A, 700:A246, Aug

    work page doi:10.1051/0004-6361/202451771

  14. [14]

    J.Cantó,A.C.Raga,andL.F.Rodríguez

    doi: 10.1051/0004-6361/202554533. J.Cantó,A.C.Raga,andL.F.Rodríguez. ApJ,536(2):896–901,June2000. doi: 10.1086/308983. C. Cappa, W. M. Goss, and K. A. van der Hucht. AJ, 127(5):2885–2897, May

    work page doi:10.1051/0004-6361/202554533

  15. [15]

    doi: 10.1086/383286. M. Carretero-Castrillo, M. Ribó, and J. M. Paredes. A&A, 679:A109, Nov

    work page doi:10.1086/383286

  16. [16]

    doi: 10.1007/s11214-017-0461-6. A.-N. Chené, N. St-Louis, A. F. J. Moffat, and K. G. Gayley. ApJ, 903(2):113, Nov

    work page doi:10.1007/s11214-017-0461-6

  17. [17]

    doi: 10.3847/1538-4357/abba24. R. A. Chevalier. ApJ, 258:790–797, July

    work page doi:10.3847/1538-4357/abba24

  18. [18]

    doi: 10.1086/160126. J. Chisholm, C. Tremonti, and C. Leitherer. MNRAS, 481(2):1690–1706, Dec

    work page doi:10.1086/160126

  19. [19]

    doi: 10.1086/507015. M. Cohen, Q. A. Parker, and A. J. Green. MNRAS, 360(4):1439–1447, July

    work page doi:10.1086/507015

  20. [20]

    1937-5956.2010.01194.x

    doi: 10.1111/j. 1365-2966.2005.09137.x. P. A. Crowther. ARA&A, 45(1):177–219, Sept

    work page doi:10.1111/j 2005

  21. [21]

    doi: 10.1146/annurev.astro.45.051806. 110615. S. Daley-Yates, I. R. Stevens, and T. D. Crossland. MNRAS, 463(3):2735–2745, Dec

    work page doi:10.1146/annurev.astro.45.051806

  22. [22]

    doi: 10.1093/mnras/stw2184. B. Davies, R. D. Oudmaijer, and J. S. Vink. A&A, 439(3):1107–1125, Sept

    work page doi:10.1093/mnras/stw2184

  23. [23]

    doi: 10.1051/ 0004-6361:20052781. L. Dessart.arXiv e-prints, art. arXiv:2405.04259, May

    arXiv

  24. [24]

    doi: 10.48550/arXiv.2405.04259. S. M. Dougherty et al. ApJ, 623(1):447–459, Apr

    work page doi:10.48550/arxiv.2405.04259

  25. [25]

    22 Evolved Massive Stars and Environment C

    doi: 10.1086/428494. 22 Evolved Massive Stars and Environment C. Buemi et al. S. M. Dougherty et al. A&A, 511:A58, Feb

    work page doi:10.1086/428494

  26. [26]

    doi: 10.1051/0004-6361/200913505. J. E. Drew. ApJS, 71:267, Oct

    work page doi:10.1051/0004-6361/200913505

  27. [27]

    doi: 10.1086/191374. G. A. Dulk. ARA&A, 23:169–224, Jan

    work page doi:10.1086/191374

  28. [28]

    doi: 10.1146/annurev.aa.23.090185.001125. D. Eichler and V. Usov. ApJ, 402:271, Jan

    work page doi:10.1146/annurev.aa.23.090185.001125

  29. [29]

    doi: 10.1086/172130. J. J. Eldridge and E. R. Stanway. ARA&A, 60:455–494, Aug

    work page doi:10.1086/172130

  30. [30]

    doi: 10.1051/0004-6361/201321258. R. Fender et al. InMeerKAT Science: On the Pathway to the SKA, page 13, Jan

    work page doi:10.1051/0004-6361/201321258

  31. [31]

    doi: 10.22323/1.277.0013. B. L. Flores and D. J. Hillier. MNRAS, 504(1):311–325, June

    work page doi:10.22323/1.277.0013

  32. [32]

    doi: 10.1093/mnras/stab707. A. T. Gallego-Calvente et al. A&A, 664:A49, Aug

    work page doi:10.1093/mnras/stab707

  33. [33]

    doi: 10.1051/0004-6361/202141895. G. Garcia-Segura, M.-M. Mac Low, and N. Langer. A&A, 305:229, Jan

    work page doi:10.1051/0004-6361/202141895

  34. [34]

    doi: 10.1093/mnras/stae1166. J. H. Groh, G. Meynet, and S. Ekström. A&A, 550:L7, Feb

    work page doi:10.1093/mnras/stae1166

  35. [36]

    doi: 10.1111/j.1365-2966.2010.16496.x. R. Hainich et al. A&A, 565:A27, May

    work page doi:10.1111/j.1365-2966.2010.16496.x 2010

  36. [37]

    doi: 10.1051/0004-6361/201322696. G. M. Harper, A. Brown, and J. Lim.ApJ, 551:1073–1098,

    work page doi:10.1051/0004-6361/201322696

  37. [38]

    doi: 10.1086/320215. I. Heywood et al. ApJ, 925(2):165, Feb

    work page doi:10.1086/320215

  38. [39]

    doi: 10.3847/1538-4357/ac449a. Q. Huang et al. AJ, 166(1):23, July

    work page doi:10.3847/1538-4357/ac449a

  39. [40]

    doi: 10.3847/1538-3881/acd92e. R. Ignace. MNRAS, 457(4):4123–4134, Apr

    work page doi:10.3847/1538-3881/acd92e

  40. [41]

    doi: 10.1093/mnras/stw216. A. Ingallinera et al. MNRAS, 437(4):3626–3638, Feb

    work page doi:10.1093/mnras/stw216

  41. [42]

    doi: 10.1093/mnras/stt2157. A. Ingallinera et al. MNRAS, 463(1):723–739, Nov

    work page doi:10.1093/mnras/stt2157

  42. [43]

    doi: 10.1093/mnras/stw2053. T. Jayasinghe et al. MNRAS, 488(1):1141–1165, Sept

    work page doi:10.1093/mnras/stw2053

  43. [44]

    doi: 10.1093/mnras/stz1738. P. Kervella et al. A&A, 609:A67, Jan

    work page doi:10.1093/mnras/stz1738

  44. [45]

    doi: 10.1051/0004-6361/201731761. H. A. Kobulnicky et al. ApJS, 227(2):18, Dec

    work page doi:10.1051/0004-6361/201731761

  45. [46]

    doi: 10.3847/0067-0049/227/2/18. R. Kotak and J. S. Vink. A&A, 460(2):L5–L8, Dec

    work page doi:10.3847/0067-0049/227/2/18

  46. [47]

    doi: 10.1051/0004-6361:20065800. C. C. Lang, K. E. Johnson, W. M. Goss, and L. F. Rodríguez. AJ, 130(5):2185–2196, Nov

    work page doi:10.1051/0004-6361:20065800

  47. [48]

    doi: 10.1086/496976. N. Langer. ARA&A, 50:107–164, Sept

    work page doi:10.1086/496976

  48. [49]

    doi: 10.1146/annurev-astro-081811-125534. C. Leitherer and C. Robert. ApJ, 377:629, Aug

    work page doi:10.1146/annurev-astro-081811-125534

  49. [50]

    S.LépineandA.F.J.Moffat

    doi: 10.1086/170390. S.LépineandA.F.J.Moffat. AJ,136(2):548–553,Aug.2008. doi: 10.1088/0004-6256/136/2/548. S. Lépine et al. AJ, 120(6):3201–3217, Dec

    work page doi:10.1086/170390 2008

  50. [51]

    doi: 10.1086/316858. S.-C. Leung, S. Wu, and J. Fuller. ApJ, 923(1):41, Dec

    work page doi:10.1086/316858

  51. [52]

    doi: 10.3847/1538-4357/ac2c63. S. J. Lipscy, M. Jura, and M. J. Reid. ApJ, 626(1):439–445, June

    work page doi:10.3847/1538-4357/ac2c63

  52. [53]

    doi: 10.1086/429900. G. Maravelias et al.Galaxies, 11(3):79, June

    work page doi:10.1086/429900

  53. [54]

    doi: 10.3390/galaxies11030079. J. M. Marcaide et al. A&A, 505(3):927–945, Oct

    work page doi:10.3390/galaxies11030079

  54. [55]

    doi: 10.1051/0004-6361/200912133. A. Marcowith et al. MNRAS, 479(4):4470–4485, Oct

    work page doi:10.1051/0004-6361/200912133

  55. [56]

    doi: 10.1093/mnras/sty1743. R. Margutti et al. ApJ, 835(2):140, Feb

    work page doi:10.1093/mnras/sty1743

  56. [57]

    doi: 10.3847/1538-4357/835/2/140. I. Martí-Vidal et al. A&A, 526:A143, Feb. 2011a. doi: 10.1051/0004-6361/201014517. I. Martí-Vidal et al. A&A, 526:A142, Feb. 2011b. doi: 10.1051/0004-6361/200913831. P. Massey, E. Waterhouse, and K. DeGioia-Eastwood. AJ, 119(5):2214–2241, May

    work page doi:10.3847/1538-4357/835/2/140

  57. [58]

    Buemi et al

    doi: 23 Evolved Massive Stars and Environment C. Buemi et al. 10.1086/301345. D. McConnell et al. PASA, 37:e048, Nov

    work page doi:10.1086/301345

  58. [59]

    doi: 10.1017/pasa.2020.41. P. G. Mezger and A. P. Henderson. ApJ, 147:471, Feb

    work page doi:10.1017/pasa.2020.41 2020

  59. [60]

    doi: 10.1086/149030. M. Miceli et al. A&A, 593:A26, Aug

    work page doi:10.1086/149030

  60. [61]

    doi: 10.1051/0004-6361/201628725. D. Milisavljevic et al. ApJ, 815(2):120, Dec

    work page doi:10.1051/0004-6361/201628725

  61. [62]

    doi: 10.1088/0004-637X/815/2/120. D. R. Mizuno et al. AJ, 139(4):1542–1552, Apr

    work page doi:10.1088/0004-637x/815/2/120

  62. [63]

    doi: 10.1088/0004-6256/139/4/1542. A. F. J. Moffat, L. Drissen, R. Lamontagne, and C. Robert. ApJ, 334:1038, Nov

    work page doi:10.1088/0004-6256/139/4/1542

  63. [64]

    doi: 10.1086/166895. J. M. Moran. Rev. Mexicana Astron. Astrofis., 7:95–107, Aug

    work page doi:10.1086/166895

  64. [65]

    doi: 10.3847/1538-4357/aa71b3. M. Moutzouri et al. A&A, 663:A80, July

    work page doi:10.3847/1538-4357/aa71b3

  65. [66]

    doi: 10.1051/0004-6361/202243098. K. Murase et al. ApJ, 874(1):80, Mar

    work page doi:10.1051/0004-6361/202243098

  66. [67]

    doi: 10.3847/1538-4357/ab0422. R. P. Norris et al. PASA, 28(3):215–248, Aug

    work page doi:10.3847/1538-4357/ab0422

  67. [68]

    doi: 10.1071/AS11021. E. O’Gorman et al. A&A, 638:A65, June

    work page doi:10.1071/as11021

  68. [69]

    doi: 10.1051/0004-6361/202037756. S. Orlando et al. A&A, 622:A73, Feb

    work page doi:10.1051/0004-6361/202037756

  69. [70]

    doi: 10.1051/0004-6361/201834487. S. Orlando et al. A&A, 636:A22, Apr

    work page doi:10.1051/0004-6361/201834487

  70. [71]

    doi: 10.1051/0004-6361/201936718. S. Orlando et al. A&A, 645:A66, Jan

    work page doi:10.1051/0004-6361/201936718

  71. [72]

    doi: 10.1051/0004-6361/202039335. S. Orlando et al. A&A, 666:A2, Oct

    work page doi:10.1051/0004-6361/202039335

  72. [73]

    doi: 10.1051/0004-6361/202243258. S. Orlando et al. ApJ, 977(1):118, Dec

    work page doi:10.1051/0004-6361/202243258

  73. [74]

    doi: 10.3847/1538-4357/ad8ac8. S. Orlando et al. A&A, 696:A188, Apr

    work page doi:10.3847/1538-4357/ad8ac8

  74. [75]

    doi: 10.1051/0004-6361/202553902. N. Panagia and M. Felli. A&A, 39:1–5, Feb

    work page doi:10.1051/0004-6361/202553902

  75. [76]

    doi: 10.1051/0004-6361:20010774. C. S. Peri et al. A&A, 538:A108, Feb

    work page doi:10.1051/0004-6361:20010774

  76. [77]

    doi: 10.1051/0004-6361/201118116. C. S. Peri, P. Benaglia, and N. L. Isequilla. A&A, 578:A45, June

    work page doi:10.1051/0004-6361/201118116

  77. [78]

    doi: 10.1051/0004-6361/ 201424676. O. Petruk et al. MNRAS, 518(4):6377–6389, Feb

    work page doi:10.1051/0004-6361/

  78. [79]

    doi: 10.1093/mnras/stac3564. S. F. Portegies Zwart, S. L. W. McMillan, and M. Gieles. ARA&A, 48:431–493, Sept

    work page doi:10.1093/mnras/stac3564

  79. [80]

    doi: 10.1146/annurev-astro-081309-130834. J. Puls, J. S. Vink, and F. Najarro. A&A Rev., 16(3-4):209–325, Dec

    work page doi:10.1146/annurev-astro-081309-130834

  80. [81]

    doi: 10.1051/0004-6361/202346980. J. Sanchez-Bermudez et al. A&A, 624:A55, Apr

    work page doi:10.1051/0004-6361/202346980

Showing first 80 references.