pith. sign in

arxiv: 2605.14623 · v1 · pith:VFCUCIKWnew · submitted 2026-05-14 · 🌌 astro-ph.HE

GeV emission around SS 433 with 17 years Fermi-LAT observation

Qiwang Sun , Dmitry Khangulyan , Jiren Liu , Siming Liu This is my paper

Pith reviewed 2026-06-30 20:49 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords SS 433Fermi-LATmicroquasarW50GeV emissionhadronic interactionscosmic ray protonsoutflows
0
0 comments X

The pith

SS 433 outflows accelerate cosmic-ray protons to GeV energies

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

The paper analyzes 17 years of Fermi-LAT gamma-ray data on the microquasar SS 433 and identifies four GeV sources in the surrounding W50 region. Two of them, the West excess and J1913+0512, show soft spectra and positions offset from the X-ray and TeV lobes, which the authors attribute to GeV particles accelerated in SS 433 interacting with localized dense gas. This interpretation favors a hadronic process in which cosmic-ray protons collide with the gas, producing the observed emission. A sympathetic reader would care because it supplies the first direct hint that Galactic microquasars can accelerate protons in their large-scale outflows, linking them to the broader cosmic-ray population. The East excess is instead linked to electrons through inverse Compton scattering.

Core claim

The emission from the West excess and J1913+0512 can be explained by GeV particles accelerated in SS 433, distributed throughout the source volume, and interacting with localized dense gas targets. Under reasonable assumptions regarding particle transport and energetics, both proton-proton and bremsstrahlung scenarios are viable, although the hadronic scenario is more naturally accommodated. These findings may therefore represent the first observational evidence for the acceleration of cosmic-ray protons in large-scale outflows from Galactic microquasars.

What carries the argument

The soft-spectrum West excess (photon index ~2.6) and its spatial offset from known X-ray and TeV regions, which together indicate hadronic interactions with dense gas targets rather than the leptonic processes seen in the East excess.

If this is right

  • The hadronic channel is preferred for the West excess and J1913+0512 under standard transport assumptions.
  • Microquasars can accelerate cosmic-ray protons in their outflows at GeV energies.
  • The lack of detected periodicity in J1913+0512 over the full dataset removes earlier claims of modulation.
  • The East excess is produced by the same relativistic electrons responsible for the X-ray and TeV emission via inverse Compton.

Where Pith is reading between the lines

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

  • Similar GeV features may appear around other microquasars that drive outflows into dense interstellar gas.
  • Higher-resolution gamma-ray or radio maps could directly correlate the West excess with specific dense gas clumps inside W50.
  • If confirmed, microquasar outflows would join supernova remnants as contributors to the Galactic cosmic-ray spectrum below the knee.

Load-bearing premise

The GeV emission in the West excess and J1913+0512 comes from particles accelerated inside SS 433 that then interact with dense gas targets.

What would settle it

A future observation showing that the West excess has a hard spectrum matching the East excess, or exhibits the same periodic modulation as the central source, would undermine the hadronic interpretation.

Figures

Figures reproduced from arXiv: 2605.14623 by Dmitry Khangulyan, Jiren Liu, Qiwang Sun, Siming Liu.

Figure 1
Figure 1. Figure 1: Significance maps (√ T S) of the emission around SS 433 in the 1–100 GeV (left) and 3–100 GeV (right) bands. The green dashed circles, centered on each source, indicate the 68% positional uncertainties in the corresponding energy band. The white solid circle in the lower-right corner represents the 68% containment angle of the Fermi-LAT point-spread function (PSF) at 10 GeV. The magenta short line marks th… view at source ↗
Figure 3
Figure 3. Figure 3: The 95% spectral upper limits calculated from the eastern (upper panel) and the western (lower panel) test sources. The locations of the test sources are indicated in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Multiwavelength spectral fitting to the eastern (upper panel) and western (lower panel) lobes of SS 433. suggests that the excess seen in the 10-year dataset is rather a fluctuation than an evidence for real periodicity. 3.4. Mutiwavelength Analysis While J1913+0512 appears morphologically separated from the binary system and its non-thermal jets, it is less certain for the emission associated with the eas… view at source ↗
read the original abstract

We present an analysis of 17 years of Fermi-LAT observations of the microquasar SS~433. We detect four GeV sources in the region: a newly identified source, PS J1910+0550, located outside W50; the previously reported source J1913+0512; and two features, denoted as the East and West excesses, apparently associated with the X-ray lobes. We focus on the three sources located within W50. We do not confirm the previously reported periodic modulation from J1913+0512, as no significant periodicity is found in the full 17-year dataset. The East and West excesses exhibit distinct morphological and spectral properties, suggesting different physical origins. The East excess shows a hard spectrum with photon index $\sim1.7$, consistent with inverse Compton emission from relativistic electrons accelerated together with the particles responsible for the X-ray and TeV emission. In contrast, the West excess has a much softer spectrum with photon index $\sim2.6$ and is spatially offset from the known X-ray and TeV emission regions in the western lobe. The spectral shape and offset position of the West excess make it strikingly similar to J1913+0512. The emission from these two regions can be explained by GeV particles accelerated in SS~433, distributed throughout the source volume, and interacting with localized dense gas targets. Under reasonable assumptions regarding particle transport and energetics, both proton-proton and bremsstrahlung scenarios are viable, although the hadronic scenario is more naturally accommodated. These findings may therefore represent the first observational evidence for the acceleration of cosmic-ray protons in large-scale outflows from Galactic microquasars.

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

3 major / 2 minor

Summary. The manuscript analyzes 17 years of Fermi-LAT data on the microquasar SS 433, detecting four GeV sources including a new source outside W50, the previously reported J1913+0512, and East/West excesses associated with the X-ray lobes. It reports no significant periodicity in J1913+0512 over the full dataset, describes the East excess as having a hard spectrum (photon index ~1.7) consistent with inverse Compton emission, and the West excess as softer (~2.6) and offset from known lobes, similar to J1913+0512. The emission from J1913+0512 and the West excess is interpreted as arising from GeV particles accelerated in SS 433 outflows, distributed throughout the volume, and interacting with localized dense gas targets, with both pp and bremsstrahlung scenarios viable but the hadronic one preferred under reasonable transport and energetics assumptions. This is presented as possible first evidence for cosmic-ray proton acceleration in large-scale outflows from Galactic microquasars.

Significance. If the associations and hadronic interpretation hold after quantitative verification, the result would be significant as the first observational indication of proton acceleration in microquasar outflows, with implications for cosmic-ray origins in Galactic sources. The extended 17-year dataset and explicit non-confirmation of prior periodicity represent a strength in reassessing earlier claims.

major comments (3)
  1. [Discussion] The central claim that the West excess and J1913+0512 represent GeV particles from SS 433 outflows interacting with dense gas targets rests on 'reasonable assumptions regarding particle transport and energetics' without explicit calculations (e.g., required proton luminosity, diffusion timescales, or target column densities) matched to observed HI/CO structures at those precise locations.
  2. [Results (J1913+0512 analysis)] The non-confirmation of the 162-day periodicity in the full 17-year dataset removes the primary prior link for J1913+0512; the manuscript should quantify the periodicity search sensitivity and discuss what alternative morphological or spectral evidence now supports the outflow association.
  3. [Morphological and spectral analysis] The spatial offset of the West excess from the X-ray/TeV lobes is noted as making it similar to J1913+0512, but without a propagation model or comparison of energy budgets, the assertion that particles are 'distributed throughout the source volume' remains unquantified and load-bearing for the hadronic scenario.
minor comments (2)
  1. [Abstract and Results] Photon indices are quoted approximately (~1.7, ~2.6); reporting best-fit values with statistical uncertainties and the energy range of the fits would improve clarity.
  2. [Introduction/Results] The newly identified source PS J1910+0550 is mentioned but not analyzed in detail; a brief statement on why it is excluded from the W50-focused discussion would aid context.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address each major comment below and indicate the revisions made to the manuscript.

read point-by-point responses

  1. Referee: The central claim that the West excess and J1913+0512 represent GeV particles from SS 433 outflows interacting with dense gas targets rests on 'reasonable assumptions regarding particle transport and energetics' without explicit calculations (e.g., required proton luminosity, diffusion timescales, or target column densities) matched to observed HI/CO structures at those precise locations.

    Authors: We agree that explicit calculations strengthen the discussion. In the revised manuscript we add order-of-magnitude estimates of the required proton luminosity to produce the observed GeV flux, diffusion timescales using standard ISM coefficients, and references to published HI and CO maps to estimate target column densities at the source locations. These calculations confirm that the hadronic scenario remains viable. revision: yes

  2. Referee: The non-confirmation of the 162-day periodicity in the full 17-year dataset removes the primary prior link for J1913+0512; the manuscript should quantify the periodicity search sensitivity and discuss what alternative morphological or spectral evidence now supports the outflow association.

    Authors: We have added a quantitative assessment of the periodicity-search sensitivity, showing that a modulation of the previously reported amplitude would have been detected at high significance in the 17-year data set. We now explicitly discuss the supporting morphological (location inside W50) and spectral (soft index consistent with hadronic emission and similarity to the West excess) evidence that remains after the periodicity is ruled out. revision: yes

  3. Referee: The spatial offset of the West excess from the X-ray/TeV lobes is noted as making it similar to J1913+0512, but without a propagation model or comparison of energy budgets, the assertion that particles are 'distributed throughout the source volume' remains unquantified and load-bearing for the hadronic scenario.

    Authors: We acknowledge that a full propagation model lies beyond the scope of this observational work. In revision we have added a comparison of the total energy in relativistic particles required by the observed flux with the known power of SS 433 outflows; this shows that the required energy can be supplied and distributed throughout the volume under plausible conditions. We have clarified the qualitative nature of this argument in the text. revision: partial

Circularity Check

0 steps flagged

No circularity: observational analysis with interpretive claims under explicit assumptions

full rationale

The paper performs Fermi-LAT data analysis, source detection, periodicity searches, and spectral fitting on 17 years of observations. The central claim is an interpretation that the observed GeV emission 'can be explained by' particles from SS 433 interacting with dense targets, presented as viable under 'reasonable assumptions' rather than derived from first principles or forced by any fit. No equations, predictions, or uniqueness theorems are invoked that reduce to the input data or self-citations by construction. The non-confirmation of prior periodicity is explicitly stated, removing reliance on earlier links. This is a standard observational report whose interpretation remains falsifiable against external gas maps and energetics constraints.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on domain assumptions about particle acceleration, transport, and interaction with gas in the SS 433 system rather than new free parameters or invented entities.

axioms (1)
  • domain assumption Assumptions regarding particle transport and energetics in the SS 433 outflows allow the hadronic scenario to be viable
    Invoked in the abstract to conclude that proton-proton interactions can explain the observed GeV emission from particles originating in SS 433.

pith-pipeline@v0.9.1-grok · 5849 in / 1487 out tokens · 34775 ms · 2026-06-30T20:49:38.502624+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

31 extracted references · 29 canonical work pages · 3 internal anchors

  1. [1]

    U., Albert, A., Alfaro, R., et al

    Abeysekara, A. U., Albert, A., Alfaro, R., et al. 2018, Nature, 562, 82, doi: 10.1038/s41586-018-0565-5

    work page doi:10.1038/s41586-018-0565-5 2018

  2. [2]

    A., Atoyan, A

    Aharonian, F. A., Atoyan, A. M., & Kifune, T. 1997, MNRAS, 291, 162, doi: 10.1093/mnras/291.1.162

    work page doi:10.1093/mnras/291.1.162 1997

  3. [3]

    C., et al

    Alfaro, R., Alvarez, C., Arteaga-Vel´ azquez, J. C., et al. 2024, ApJ, 976, 30, doi: 10.3847/1538-4357/ad7e1b

    work page doi:10.3847/1538-4357/ad7e1b 2024

  4. [4]

    J.6971071–1102 doi:10.1088/0004-637X/697/2/1071

    Atwood, W. B., Abdo, A. A., Ackermann, M., et al. 2009, ApJ, 697, 1071, doi: 10.1088/0004-637X/697/2/1071

    work page doi:10.1088/0004-637x/697/2/1071 2009

  5. [5]

    M., & Bowler, M

    Blundell, K. M., & Bowler, M. G. 2004, ApJL, 616, L159, doi: 10.1086/426542 AASTeX v6.3.1 Sample article9

    work page doi:10.1086/426542 2004

  6. [6]

    M., & Perucho, M

    Bordas, P., Bosch-Ramon, V., Paredes, J. M., & Perucho, M. 2009, A&A, 497, 325, doi: 10.1051/0004-6361/200810781

    work page doi:10.1051/0004-6361/200810781 2009

  7. [7]

    2015, ApJL, 807, L8, doi: 10.1088/2041-8205/807/1/L8

    Bordas, P., Yang, R., Kafexhiu, E., & Aharonian, F. 2015, ApJL, 807, L8, doi: 10.1088/2041-8205/807/1/L8

    work page doi:10.1088/2041-8205/807/1/l8 2015

  8. [8]

    2009, International Journal of Modern Physics D, 18, 347, doi: 10.1142/S0218271809014601

    Bosch-Ramon, V., & Khangulyan, D. 2009, International Journal of Modern Physics D, 18, 347, doi: 10.1142/S0218271809014601

    work page doi:10.1142/s0218271809014601 2009

  9. [9]

    2011, A&A, 528, A89, doi: 10.1051/0004-6361/201016364

    Bosch-Ramon, V., Perucho, M., & Bordas, P. 2011, A&A, 528, A89, doi: 10.1051/0004-6361/201016364

    work page doi:10.1051/0004-6361/201016364 2011

  10. [10]

    1996, A&A, 312, 306

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

    1996

  11. [11]

    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

  12. [12]

    M., Dodin, A

    Cherepashchuk, A. M., Dodin, A. V., & Postnov, K. A. 2025, arXiv e-prints, arXiv:2506.01106, doi: 10.48550/arXiv.2506.01106

    work page doi:10.48550/arxiv.2506.01106 2025

  13. [13]

    H., & Murdin, P

    Clark, D. H., & Murdin, P. 1978, Nature, 276, 44, doi: 10.1038/276044a0 de la Cita, V. M., del Palacio, S., Bosch-Ramon, V., et al. 2017, A&A, 604, A39, doi: 10.1051/0004-6361/201630060

    work page doi:10.1038/276044a0 1978

  14. [14]

    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

  15. [15]

    Fang, K., Charles, E., & Blandford, R. D. 2020, ApJL, 889, L5, doi: 10.3847/2041-8213/ab62b8 H. E. S. S. Collaboration, Aharonian, F., Ait Benkhali, F., et al. 2024, Science, 383, 402, doi: 10.1126/science.adi2048

    work page doi:10.3847/2041-8213/ab62b8 2020

  16. [16]

    2024, ApJL, 961, L12, doi: 10.3847/2041-8213/ad103b

    Kaaret, P., Ferrazzoli, R., Silvestri, S., et al. 2024, ApJL, 961, L12, doi: 10.3847/2041-8213/ad103b

    work page doi:10.3847/2041-8213/ad103b 2024

  17. [17]

    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

  18. [18]

    Cygnus X-3: A variable petaelectronvolt gamma-ray source

    Khangulyan, D., Aharonian, F. A., & Kelner, S. R. 2014, ApJ, 783, 100, doi: 10.1088/0004-637X/783/2/100 LHAASO Collaboration, Cao, Z., Aharonian, F., et al. 2025a, National Science Review, 12, nwaf496, doi: 10.1093/nsr/nwaf496 —. 2025b, arXiv e-prints, arXiv:2512.16638, doi: 10.48550/arXiv.2512.16638

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/783/2/100 2014

  19. [19]

    F., Liu, R.-Y., et al

    Li, J., Torres, D. F., Liu, R.-Y., et al. 2020, Nature Astronomy, 4, 1177, doi: 10.1038/s41550-020-1164-6

    work page doi:10.1038/s41550-020-1164-6 2020

  20. [20]

    C., Grandi, S

    Margon, B., Ford, H. C., Grandi, S. A., & Stone, R. P. S. 1979, ApJL, 233, L63, doi: 10.1086/183077

    work page doi:10.1086/183077 1979

  21. [21]

    2026, ApJ, 1001, 92, doi: 10.3847/1538-4357/ae4e18

    Oka, T., Ariyama, R., & Kotani, T. 2026, ApJ, 1001, 92, doi: 10.3847/1538-4357/ae4e18

    work page doi:10.3847/1538-4357/ae4e18 2026

  22. [22]

    M., Graham, J

    Rasul, K., Chadwick, P. M., Graham, J. A., & Brown, A. M. 2019, MNRAS, 485, 2970, doi: 10.1093/mnras/stz559

    work page doi:10.1093/mnras/stz559 2019

  23. [23]

    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

  24. [24]

    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

  25. [25]

    B., & Sanduleak, N

    Stephenson, C. B., & Sanduleak, N. 1971, Publications of the Warner & Swasey Observatory, 1, 1

    1971

  26. [26]

    2019, A&A, 626, A113, doi: 10.1051/0004-6361/201935621

    Sun, X.-N., Yang, R.-Z., Liu, B., Xi, S.-Q., & Wang, X.-Y. 2019, A&A, 626, A113, doi: 10.1051/0004-6361/201935621

    work page doi:10.1051/0004-6361/201935621 2019

  27. [27]

    2025, arXiv e-prints, arXiv:2510.14938, doi: 10.48550/arXiv.2510.14938

    Sunyaev, R., Khabibullin, I., Churazov, E., et al. 2025, arXiv e-prints, arXiv:2510.14938, doi: 10.48550/arXiv.2510.14938

    work page doi:10.48550/arxiv.2510.14938 2025

  28. [28]

    Investigation of the Microquasar SS 433 with VERITAS

    Tsuji, N., Inoue, Y., Khangulyan, D., et al. 2025, ApJL, 993, L24, doi: 10.3847/2041-8213/ae0e73 VERITAS Collaboration, Archer, A., Bangale, P., et al. 2026, arXiv e-prints, arXiv:2603.22105, doi: 10.48550/arXiv.2603.22105

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ae0e73 2025

  29. [29]

    Wang, J., Reville, B., & Aharonian, F. A. 2025, ApJL, 989, L25, doi: 10.3847/2041-8213/adf3a4

    work page doi:10.3847/2041-8213/adf3a4 2025

  30. [30]

    2019, ApJ, 872, 25, doi: 10.3847/1538-4357/aafc60

    Xing, Y., Wang, Z., Zhang, X., Chen, Y., & Jithesh, V. 2019, ApJ, 872, 25, doi: 10.3847/1538-4357/aafc60

    work page doi:10.3847/1538-4357/aafc60 2019

  31. [31]

    T., Kimura, S

    Zhang, B. T., Kimura, S. S., & Murase, K. 2025, PhRvD, 112, 123015, doi: 10.1103/p6r1-qg5q

    work page doi:10.1103/p6r1-qg5q 2025