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arxiv: 2606.08931 · v1 · pith:BMSBPWWJnew · submitted 2026-06-08 · 🌌 astro-ph.HE

Discovery of CO Clouds Associated with the X-ray Jets of SS 433: Evidence for Shock-Cloud Interaction Enhancing Nonthermal X-ray Emission

Haruka Sakemi , Hidetoshi Sano , Yasuo Fukui , Mami Machida , Shigeo S. Kimura , Masato I.N. Kobayashi , Kazuho Kayama , Hiroaki Yamamoto
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Kengo Tachihara Hiroshi Nagai
This is my paper

Pith reviewed 2026-06-27 15:54 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords SS 433X-ray jetsmolecular clumpsshock-cloud interactionnonthermal emissionmicroquasarCO observationsinterstellar medium
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The pith

Molecular clumps coincide with SS 433 jet re-brightening regions, providing evidence that shock-cloud interactions amplify magnetic fields to produce nonthermal X-rays.

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

The paper reports the first detection of molecular clumps in 12CO emission that align spatially with the re-brightening zones at the heads of SS 433's large-scale X-ray jets. The X-ray intensity reaches a maximum immediately downstream from these clumps, and the hardness ratio rises at the clump surfaces, patterns inconsistent with absorption. These alignments supply direct evidence that the jets are driving shocks into the surrounding interstellar medium. The authors propose that the resulting turbulence strengthens magnetic fields at the interfaces, enabling the particle acceleration responsible for the nonthermal X-ray output. The work underscores the role of jet-ISM encounters in setting the high-energy appearance of microquasar jets.

Core claim

The first identification of molecular clumps directly associated with the re-brightening regions of the large-scale X-ray jets of SS 433, based on 12CO (J=1-0) observations. Multiple clumps toward the eastern and western jet heads show clear spatial correlation with the X-ray emission. The X-ray emission peaks immediately downstream of the molecular clumps, while the hardness ratio is enhanced at their surfaces. These results provide direct evidence for shock-cloud interactions between the jets and the surrounding interstellar medium. Turbulence generated at the jet-cloud interface amplifies magnetic fields, producing the observed non-thermal X-ray emission.

What carries the argument

Spatial correlation between CO molecular clumps and X-ray re-brightening regions, featuring a downstream X-ray peak and surface hardness enhancement, as the signature of physical shock interaction.

If this is right

  • Jet interactions with the interstellar medium determine the X-ray properties of microquasar jets.
  • Turbulence at jet-cloud boundaries amplifies magnetic fields.
  • The amplified fields accelerate particles and generate the observed nonthermal X-ray emission.
  • Similar shock-cloud processes operate at both eastern and western jet heads.

Where Pith is reading between the lines

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

  • The same interaction mechanism may appear in other microquasars once comparable CO mapping is obtained.
  • Detailed simulations of the turbulence layer could forecast the expected X-ray luminosity from such interfaces.
  • Multi-wavelength follow-up at higher angular resolution could locate the precise sites of field amplification.

Load-bearing premise

The spatial alignments and X-ray morphology indicate genuine physical shocks at the jet-cloud interfaces rather than chance projection or unrelated processes.

What would settle it

Finding CO clumps at the jet heads but without a corresponding downstream X-ray intensity peak or hardness increase at the clump surfaces would falsify the claimed shock interaction.

Figures

Figures reproduced from arXiv: 2606.08931 by Haruka Sakemi, Hidetoshi Sano, Hiroaki Yamamoto, Hiroshi Nagai, Kazuho Kayama, Kengo Tachihara, Mami Machida, Masato I.N. Kobayashi, Shigeo S. Kimura, Yasuo Fukui.

Figure 1
Figure 1. Figure 1: Two-color composite image of the integrated intensity of 12CO (J = 1–0) (cyan) and the X-ray photon flux in the 0.5–7 keV band observed with Chandra (orange) (N. Tsuji et al. 2025). The velocity ranges used for the CO integration are 46.5–58.3 km s−1 for the eastern side and 51.7–56.5 km s−1 for the western side. The position of SS 433 is indicated by a white star. The scale bar at the lower right assumes … view at source ↗
Figure 2
Figure 2. Figure 2: Integrated intensity maps of 12CO (J = 1–0). The left and right panels show the eastern and western jet head regions, respectively. The velocity ranges are the same as those in [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the spatial distributions of the X-ray surface brightness in the 0.5–10 keV band observed with XMM-Newton (K. Kayama et al. 2022, 2025) and the integrated intensity of 12CO (J = 1–0). The X-ray images are regridded to match the spatial grid of the CO data. The left and right columns correspond to the eastern and western jets, respectively. The top panels show the X-ray surface brightness, and… view at source ↗
Figure 4
Figure 4. Figure 4: Hardness ratio map between the 0.5–1.5 keV and 2.0–7.0 keV bands observed with XMM-Newton (K. Kayama et al. 2022, 2025). The images are regridded to match the spatial grid of the 12CO (J = 1–0) data, as in [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Schematic illustration of the shock–cloud interaction occurring in the head regions of the X-ray jets of SS 433. and 1.64, are significantly harder than those typically observed in shock regions of SNRs. In the case of SNRs, ideal DSA predicts Γ = 1.5, whereas observed values are typically in the range of Γ = 2–3 (S. P. Reynolds 2008). This discrepancy is generally attributed to synchrotron cooling and non… view at source ↗
read the original abstract

We report the first identification of molecular clumps directly associated with the re-brightening regions of the large-scale X-ray jets of SS 433, based on $^{12}$CO ($J$ = 1--0) observations with the Nobeyama 45-m Radio Telescope. Multiple clumps are detected toward the eastern and western jet heads, showing clear spatial correlation with the X-ray emission. The X-ray emission peaks immediately downstream of the molecular clumps, while the hardness ratio is enhanced at their surfaces, indicating that the observed structures cannot be explained by absorption effects. These results provide direct evidence for shock--cloud interactions between the jets and the surrounding interstellar medium. We suggest that turbulence generated at the jet--cloud interface amplifies magnetic fields, producing the observed non-thermal X-ray emission. Our findings highlight the importance of jet--ISM interactions in shaping the X-ray properties of microquasar jets.

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 reports the first detection of 12CO (J=1-0) molecular clumps toward the eastern and western X-ray jet heads of SS 433 using Nobeyama 45-m telescope observations. The clumps exhibit spatial correlation with X-ray re-brightening regions; X-ray emission peaks immediately downstream of the clumps while hardness ratios are enhanced at clump surfaces. The authors interpret these features as direct evidence for shock-cloud interactions, proposing that turbulence at the jet-cloud interface amplifies magnetic fields and produces the observed non-thermal X-ray emission.

Significance. If the physical association holds, the result would provide valuable new evidence on how jet-ISM interactions shape non-thermal X-ray properties in microquasars. The work is observationally novel in linking molecular gas directly to jet re-brightening sites in SS 433 and could inform models of turbulence-driven field amplification in relativistic jets.

major comments (2)
  1. [Abstract] Abstract: The central claim of 'direct evidence for shock-cloud interactions' depends on the spatial correlation being physical rather than coincidental. No quantitative chance-alignment probability, projection-effect test, or velocity information linking the CO clumps to the jet flow is reported, leaving the causal step under-supported.
  2. [Abstract] Abstract: The statement that the structures 'cannot be explained by absorption effects' rests on the downstream X-ray peak and surface hardness enhancement, yet the abstract supplies no explicit absorption modeling, hardness-ratio error analysis, or statistical significance of the correlation to substantiate this exclusion.
minor comments (1)
  1. [Abstract] The abstract would benefit from stating the number of detected clumps, the angular resolution of the Nobeyama data, and any quantitative measure of the CO-X-ray positional match.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments on our manuscript. We address each major comment point by point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim of 'direct evidence for shock-cloud interactions' depends on the spatial correlation being physical rather than coincidental. No quantitative chance-alignment probability, projection-effect test, or velocity information linking the CO clumps to the jet flow is reported, leaving the causal step under-supported.

    Authors: The CO clumps coincide precisely with the well-established positions of the X-ray jet heads, and the X-ray emission peaks immediately downstream of the clumps in both the eastern and western jets. This repeated morphological pattern across independent jet directions makes random alignment improbable. We did not include a formal statistical probability calculation. We will revise the manuscript to add explicit discussion of projection effects and note the absence of velocity information as a limitation while retaining the morphological evidence as support for physical association. revision: partial

  2. Referee: [Abstract] Abstract: The statement that the structures 'cannot be explained by absorption effects' rests on the downstream X-ray peak and surface hardness enhancement, yet the abstract supplies no explicit absorption modeling, hardness-ratio error analysis, or statistical significance of the correlation to substantiate this exclusion.

    Authors: The exclusion of absorption follows from the X-ray peak lying downstream of the clumps and the hardness ratio increasing specifically at clump surfaces; absorption by foreground molecular gas would suppress rather than shift or harden emission in this manner. The abstract is necessarily concise. We will revise the main text to include additional details on hardness-ratio uncertainties and the spatial correlation significance to better support the statement. revision: partial

Circularity Check

0 steps flagged

Purely observational result with no derivation chain or fitted predictions

full rationale

The manuscript reports new 12CO (J=1-0) observations with the Nobeyama 45-m telescope showing spatial correlations between molecular clumps and X-ray re-brightening regions in the SS 433 jets. It notes downstream X-ray peaks and surface hardness enhancements, then interprets these as evidence for shock-cloud interactions. No equations, model fits, parameter estimations, or mathematical derivations appear anywhere in the text. The central claim rests on direct observational associations rather than any reduction of a predicted quantity to fitted inputs or self-citations. No load-bearing steps match any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard radio-astronomy assumptions about molecular-line tracing and the physical meaning of spatial correlations; no free parameters or new entities are introduced.

axioms (2)
  • domain assumption 12CO (J=1-0) emission reliably traces dense molecular hydrogen gas in the interstellar medium
    Standard assumption invoked when mapping molecular clumps with radio telescopes.
  • domain assumption Spatial coincidence plus downstream X-ray peak and surface hardness enhancement indicate physical interaction rather than projection effects
    This interpretive step is required to move from observed correlation to shock-cloud interaction claim.

pith-pipeline@v0.9.1-grok · 5739 in / 1440 out tokens · 21223 ms · 2026-06-27T15:54:39.404012+00:00 · methodology

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Works this paper leans on

51 extracted references · 49 canonical work pages · 1 internal anchor

  1. [1]

    O., & Margon, B

    Abell, G. O., & Margon, B. 1979, Nature, 279, 701, doi: 10.1038/279701a0

    work page doi:10.1038/279701a0 1979

  2. [2]

    E., van den Eijnden, J., et al

    Atri, P., Motta, S. E., van den Eijnden, J., et al. 2025, A&A, 696, A223, doi: 10.1051/0004-6361/202452837

    work page doi:10.1051/0004-6361/202452837 2025

  3. [3]

    doi:10.1086/426542 , eprint =

    Blundell, K. M., & Bowler, M. G. 2004, ApJL, 616, L159, doi: 10.1086/426542

    work page doi:10.1086/426542 2004

  4. [4]

    M., Laing, R., Lee, S., & Richards, A

    Blundell, K. M., Laing, R., Lee, S., & Richards, A. 2018, ApJL, 867, L25, doi: 10.3847/2041-8213/aae890

    work page doi:10.3847/2041-8213/aae890 2018

  5. [5]

    J., Rosolowsky, E., et al

    Bosch-Cabot, P., Tetarenko, A. J., Rosolowsky, E., et al. 2026, ApJ, 997, 64, doi: 10.3847/1538-4357/ae20f2

    work page doi:10.3847/1538-4357/ae20f2 2026

  6. [6]

    1996, A&A, 312, 306

    Brinkmann, W., Aschenbach, B., & Kawai, N. 1996, A&A, 312, 306

    1996

  7. [7]

    2007, A&A, 463, 611, doi: 10.1051/0004-6361:20065570

    Burwitz, V. 2007, A&A, 463, 611, doi: 10.1051/0004-6361:20065570

    work page doi:10.1051/0004-6361:20065570 2007

  8. [8]

    The Jets and and Supercritical Accretion Disk in SS433

    Fabrika, S. 2004, Astrophys. Space Phys. Res., 12, 1, doi: 10.48550/arXiv.astro-ph/0603390

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0603390 2004

  9. [9]

    2003, PASJ, 55, L61, doi: 10.1093/pasj/55.5.L61

    Fukui, Y., Moriguchi, Y., Tamura, K., et al. 2003, PASJ, 55, L61, doi: 10.1093/pasj/55.5.L61

    work page doi:10.1093/pasj/55.5.l61 2003

  10. [10]

    2012, ApJ, 746, 82, doi: 10.1088/0004-637X/746/1/82

    Fukui, Y., Sano, H., Sato, J., et al. 2012, ApJ, 746, 82, doi: 10.1088/0004-637X/746/1/82

    work page doi:10.1088/0004-637x/746/1/82 2012

  11. [11]

    R., Huang, W., & McSwain, M

    Gies, D. R., Huang, W., & McSwain, M. V. 2002, ApJL, 578, L67, doi: 10.1086/344436

    work page doi:10.1086/344436 2002

  12. [12]

    2026, A&A, 706, A283, doi: 10.1051/0004-6361/202557124 H

    Grollimund, N., Corbel, S., Fender, R., et al. 2026, A&A, 706, A283, doi: 10.1051/0004-6361/202557124 H. E. S. S. Collaboration, Aharonian, F., Ait Benkhali, F., et al. 2024, Science, 383, 402, doi: 10.1126/science.adi2048

    work page doi:10.1051/0004-6361/202557124 2026

  13. [13]

    C., & Gies, D

    Hillwig, T. C., & Gies, D. R. 2008, ApJL, 676, L37, doi: 10.1086/587140

    work page doi:10.1086/587140 2008

  14. [14]

    2012, ApJ, 744, 71, doi: 10.1088/0004-637X/744/1/71

    Inoue, T., Yamazaki, R., Inutsuka, S.-i., & Fukui, Y. 2012, ApJ, 744, 71, doi: 10.1088/0004-637X/744/1/71

    work page doi:10.1088/0004-637x/744/1/71 2012

  15. [15]

    2025, PASJ, 77, 880, doi: 10.1093/pasj/psaf059

    Kayama, K., Tanaka, T., Uchida, H., et al. 2025, PASJ, 77, 880, doi: 10.1093/pasj/psaf059

    work page doi:10.1093/pasj/psaf059 2025

  16. [16]

    2022, PASJ, 74, 1143, doi: 10.1093/pasj/psac060

    Kayama, K., Tanaka, T., Uchida, H., et al. 2022, PASJ, 74, 1143, doi: 10.1093/pasj/psac060

    work page doi:10.1093/pasj/psac060 2022

  17. [17]

    S., Murase, K., & M´ esz´ aros, P

    Kimura, S. S., Murase, K., & M´ esz´ aros, P. 2020, ApJ, 904, 188, doi: 10.3847/1538-4357/abbe00

    work page doi:10.3847/1538-4357/abbe00 2020

  18. [18]

    S., & Falle, S

    Komissarov, S. S., & Falle, S. A. E. G. 1997, MNRAS, 288, 833, doi: 10.1093/mnras/288.4.833

    work page doi:10.1093/mnras/288.4.833 1997

  19. [19]

    2010, ApJ, 709, 1374, doi: 10.1088/0004-637X/709/2/1374

    Kubota, K., Ueda, Y., Fabrika, S., et al. 2010, ApJ, 709, 1374, doi: 10.1088/0004-637X/709/2/1374

    work page doi:10.1088/0004-637x/709/2/1374 2010

  20. [20]

    2011, in IAU

    Kuno, N., Tosaki, T., Onodera, S., et al. 2011, in IAU

    2011

  21. [21]

    277, Tracing the Ancestry of Galaxies, ed

    Symposium, Vol. 277, Tracing the Ancestry of Galaxies, ed. C. Carignan, F. Combes, & K. C. Freeman, 67–70, doi: 10.1017/S1743921311022484

    work page doi:10.1017/s1743921311022484

  22. [22]

    L., & Ulich, B

    Kutner, M. L., & Ulich, B. L. 1981, ApJ, 250, 341, doi: 10.1086/159380 Lhaaso Collaboration, Cao, Z., Aharonian, F., et al. 2025, National Science Review, 12, nwaf496, doi: 10.1093/nsr/nwaf496 8

    work page doi:10.1086/159380 1981

  23. [23]

    2020, ApJ, 892, 143, doi: 10.3847/1538-4357/ab7a22

    Liu, Q.-C., Chen, Y., Zhou, P., Zhang, X., & Jiang, B. 2020, ApJ, 892, 143, doi: 10.3847/1538-4357/ab7a22

    work page doi:10.3847/1538-4357/ab7a22 2020

  24. [24]

    1984, ARA&A, 22, 507, doi: 10.1146/annurev.aa.22.090184.002451

    Margon, B. 1984, ARA&A, 22, 507, doi: 10.1146/annurev.aa.22.090184.002451

    work page doi:10.1146/annurev.aa.22.090184.002451 1984

  25. [25]

    E., Atri, P., et al

    Mariani, I., Motta, S. E., Atri, P., et al. 2025, A&A, 704, A239, doi: 10.1051/0004-6361/202556290 Mart´ ı, J., Bujalance-Fern´ andez, I., Luque-Escamilla, P. L., et al. 2018, A&A, 619, A40, doi: 10.1051/0004-6361/201833733

    work page doi:10.1051/0004-6361/202556290 2025

  26. [26]

    2002, Science, 297, 1673, doi: 10.1126/science.1073660

    Migliari, S., Fender, R., & M´ endez, M. 2002, Science, 297, 1673, doi: 10.1126/science.1073660

    work page doi:10.1126/science.1073660 2002

  27. [27]

    M., Seljak, U., et al

    Migliari, S., Fender, R. P., Blundell, K. M., M´ endez, M., & van der Klis, M. 2005, MNRAS, 358, 860, doi: 10.1111/j.1365-2966.2005.08791.x

    work page doi:10.1111/j.1365-2966.2005.08791.x 2005

  28. [28]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Minamidani, T., Nishimura, A., Miyamoto, Y., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, ed. W. S. Holland & J. Zmuidzinas, 99141Z, doi: 10.1117/12.2232137

    work page doi:10.1117/12.2232137 2016

  29. [29]

    2005, Advances in Space Research, 35, 1062, doi: 10.1016/j.asr.2005.01.086

    Moldowan, A., Safi-Harb, S., Fuchs, Y., & Dubner, G. 2005, Advances in Space Research, 35, 1062, doi: 10.1016/j.asr.2005.01.086

    work page doi:10.1016/j.asr.2005.01.086 2005

  30. [30]

    E., Atri, P., Matthews, J

    Motta, S. E., Atri, P., Matthews, J. H., et al. 2025, A&A, 696, A222, doi: 10.1051/0004-6361/202452838

    work page doi:10.1051/0004-6361/202452838 2025

  31. [31]

    2015, PASJ, 67, 117, doi: 10.1093/pasj/psv088

    Nakamura, F., Ogawa, H., Yonekura, Y., et al. 2015, PASJ, 67, 117, doi: 10.1093/pasj/psv088

    work page doi:10.1093/pasj/psv088 2015

  32. [32]

    2026, arXiv e-prints, arXiv:2603.21550, doi: 10.48550/arXiv.2603.21550

    Oka, T., Ariyama, R., & Kotani, T. 2026, arXiv e-prints, arXiv:2603.21550, doi: 10.48550/arXiv.2603.21550

    work page doi:10.48550/arxiv.2603.21550 2026

  33. [33]

    Reynolds, S. P. 2008, ARA&A, 46, 89, doi: 10.1146/annurev.astro.46.060407.145237

    work page doi:10.1146/annurev.astro.46.060407.145237 2008

  34. [34]

    1997, ApJ, 483, 868, doi: 10.1086/304274

    Safi-Harb, S., & ¨Ogelman, H. 1997, ApJ, 483, 868, doi: 10.1086/304274

    work page doi:10.1086/304274 1997

  35. [35]

    1999, ApJ, 512, 784, doi: 10.1086/306803

    Safi-Harb, S., & Petre, R. 1999, ApJ, 512, 784, doi: 10.1086/306803

    work page doi:10.1086/306803 1999

  36. [36]

    2022, ApJ, 935, 163, doi: 10.3847/1538-4357/ac7c05

    Safi-Harb, S., Mac Intyre, B., Zhang, S., et al. 2022, ApJ, 935, 163, doi: 10.3847/1538-4357/ac7c05

    work page doi:10.3847/1538-4357/ac7c05 2022

  37. [37]

    2025, PASJ, 77, 1113, doi: 10.1093/pasj/psaf088

    Sakai, Y., Yamada, S., Sakemi, H., et al. 2025, PASJ, 77, 1113, doi: 10.1093/pasj/psaf088

    work page doi:10.1093/pasj/psaf088 2025

  38. [38]

    2023, PASJ, 75, 338, doi: 10.1093/pasj/psad001

    Sakemi, H., Machida, M., Yamamoto, H., & Tachihara, K. 2023, PASJ, 75, 338, doi: 10.1093/pasj/psad001

    work page doi:10.1093/pasj/psad001 2023

  39. [39]

    2010, ApJ, 724, 59, doi: 10.1088/0004-637X/724/1/59

    Sano, H., Sato, J., Horachi, H., et al. 2010, ApJ, 724, 59, doi: 10.1088/0004-637X/724/1/59

    work page doi:10.1088/0004-637x/724/1/59 2010

  40. [40]

    2020, ApJL, 904, L24, doi: 10.3847/2041-8213/abc884

    Sano, H., Inoue, T., Tokuda, K., et al. 2020, ApJL, 904, L24, doi: 10.3847/2041-8213/abc884

    work page doi:10.3847/2041-8213/abc884 2020

  41. [41]

    2008, PASJ, 60, 445, doi: 10.1093/pasj/60.3.445

    Sawada, T., Ikeda, N., Sunada, K., et al. 2008, PASJ, 60, 445, doi: 10.1093/pasj/60.3.445

    work page doi:10.1093/pasj/60.3.445 2008

  42. [42]

    2018, ApJ, 863, 103, doi: 10.3847/1538-4357/aad04e

    Su, Y., Zhou, X., Yang, J., et al. 2018, ApJ, 863, 103, doi: 10.3847/1538-4357/aad04e

    work page doi:10.3847/1538-4357/aad04e 2018

  43. [43]

    2020, ApJ, 889, 146, doi: 10.3847/1538-4357/ab6442

    Sudoh, T., Inoue, Y., & Khangulyan, D. 2020, ApJ, 889, 146, doi: 10.3847/1538-4357/ab6442

    work page doi:10.3847/1538-4357/ab6442 2020

  44. [44]

    2026, A&A, 707, A278, doi: 10.1051/0004-6361/202557726

    Sunyaev, R., Khabibullin, I., Churazov, E., et al. 2026, A&A, 707, A278, doi: 10.1051/0004-6361/202557726

    work page doi:10.1051/0004-6361/202557726 2026

  45. [45]

    Miller-Jones, J. C. A., & Sivakoff, G. R. 2018, MNRAS, 475, 448, doi: 10.1093/mnras/stx3151

    work page doi:10.1093/mnras/stx3151 2018

  46. [46]

    J., Rosolowsky, E

    Tetarenko, A. J., Rosolowsky, E. W., Miller-Jones, J. C. A., & Sivakoff, G. R. 2020, MNRAS, 497, 3504, doi: 10.1093/mnras/staa2175

    work page doi:10.1093/mnras/staa2175 2020

  47. [47]

    2025, ApJL, 993, L24, doi: 10.3847/2041-8213/ae0e73

    Tsuji, N., Inoue, Y., Khangulyan, D., et al. 2025, ApJL, 993, L24, doi: 10.3847/2041-8213/ae0e73

    work page doi:10.3847/2041-8213/ae0e73 2025

  48. [48]

    A., Tanaka, T., Takahashi, T., & Maeda, Y

    Uchiyama, Y., Aharonian, F. A., Tanaka, T., Takahashi, T., & Maeda, Y. 2007, Nature, 449, 576, doi: 10.1038/nature06210

    work page doi:10.1038/nature06210 2007

  49. [49]

    Yamamoto, H., Ishikawa, T., & Takeuchi, T. T. 2024, PASJ, 76, L1, doi: 10.1093/pasj/psae007

    work page doi:10.1093/pasj/psae007 2024

  50. [50]

    2022, PASJ, 74, 493, doi: 10.1093/pasj/psac012

    Yamamoto, H., Okamoto, R., Murata, Y., et al. 2022, PASJ, 74, 493, doi: 10.1093/pasj/psac012

    work page doi:10.1093/pasj/psac012 2022

  51. [51]

    2008, PASJ, 60, 715, doi: 10.1093/pasj/60.4.715

    Yamamoto, H., Ito, S., Ishigami, S., et al. 2008, PASJ, 60, 715, doi: 10.1093/pasj/60.4.715

    work page doi:10.1093/pasj/60.4.715 2008