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arxiv: 2604.11293 · v1 · submitted 2026-04-13 · 🌌 astro-ph.HE · hep-ph

Recognition: unknown

GeV gamma-ray emission in the field of the shell-type supernova remnant Vela Jr revisited

Ting-Ting Ge , Qi-Hang Wu , Pak-Hin Thomas Tam , Jie Feng , Hai-Feng Zhou , Kai Wang , Su-Jie Lin
Authors on Pith no claims yet

Pith reviewed 2026-05-10 15:25 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-ph
keywords Vela Jrsupernova remnantgamma-ray emissionFermi-LATleptonic modelhadronic modelmulti-wavelength SEDRX J0852.0-4622
0
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The pith

Analysis of 15 years of Fermi data shows a hybrid lepton-hadron model fits the gamma-ray emission from Vela Jr better than a pure leptonic model.

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

The paper reanalyzes GeV gamma-ray observations of the shell-type supernova remnant RX J0852.0-4622 using an extended Fermi-LAT dataset. It demonstrates that the emission morphology aligns closely with the H.E.S.S. TeV shell template after masking, leaving little room for contribution from the central pulsar wind nebula. The measured spectrum is a hard power law that joins smoothly onto the TeV band. When the full multi-wavelength dataset, including new eROSITA X-ray constraints, is modeled, the hybrid lepton-hadron scenario yields a statistically superior description, indicating that proton interactions dominate the GeV output while electron processes govern the TeV output.

Core claim

Using 15 yr of Fermi Large Area Telescope data, the GeV gamma-ray emission from RX J0852.0-4622 is best described by the masked H.E.S.S. shell template, showing negligible contribution from the embedded pulsar wind nebula. The 0.1-500 GeV spectrum is a hard power law with photon index 1.77 that connects smoothly to the TeV spectrum. Independent eROSITA X-ray data supply new constraints on synchrotron emission. Both pure leptonic and hybrid lepton-hadron models reproduce the broadband spectral energy distribution, yet the hybrid model provides a better statistical fit, supporting a mixed-origin picture in which the hadronic contribution is mainly relevant in the GeV band while the TeV regime,

What carries the argument

Quantitative comparison of pure leptonic versus hybrid lepton-hadron models applied to the multi-wavelength spectral energy distribution, anchored by the masked H.E.S.S. shell morphology template.

If this is right

  • The pulsar wind nebula contributes negligibly to the GeV flux.
  • Hadronic processes supply the dominant GeV gamma-ray component.
  • Leptonic processes remain the primary driver of the TeV emission.
  • New eROSITA X-ray data tighten constraints on the synchrotron-emitting electron population.

Where Pith is reading between the lines

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

  • Similar hybrid modeling may be needed for other shell-type SNRs where GeV and TeV spectra do not align under a single mechanism.
  • Deeper GeV imaging could test whether faint PWN leakage appears at lower energies.
  • The result underscores the value of joint X-ray, GeV, and TeV datasets for separating proton and electron acceleration channels in the same remnant.

Load-bearing premise

The masked H.E.S.S. shell template is an unbiased representation of the true GeV-emitting volume with negligible residual background or point-source contamination.

What would settle it

A new Fermi-LAT analysis or morphological template that shows the hybrid model no longer yields a statistically superior fit statistic, or that the GeV morphology deviates from the masked H.E.S.S. shell, would refute the mixed-origin conclusion.

Figures

Figures reproduced from arXiv: 2604.11293 by Hai-Feng Zhou, Jie Feng, Kai Wang, Pak-Hin Thomas Tam, Qi-Hang Wu, Su-Jie Lin, Ting-Ting Ge.

Figure 1
Figure 1. Figure 1: Fermi-LAT TS maps of RX J0852.0-4622 in the energy range of 5–500 GeV (left panel) and 20–500 GeV (right panel). The size is that of a 4 ◦ × 4 ◦ region smoothed with a Gaussian filter of 1 ◦ , and each pixel is 0.05◦ × 0.05◦ in size. All white crosses represent the 4FGL-DR4 sources within the region. The red circle represents the extended source 4FGL J0851.9-4620e related to RX J0852.0-4622. The blue star … view at source ↗
Figure 2
Figure 2. Figure 2: The PS map for diagnostics of the goodness-of-fit, generated from Fermi-LAT data in the 5–500 GeV range using the best-fit spatial model (model 6 in [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: The azimuthal profile extracted from the annulus in the skymap, shown as red points for the Fermi-LAT data (right scale), blue for the H.E.S.S. data (left scale), and green for the eROSITA data (right outer scale). To facilitate comparison, a grey dashed line has been drawn between the two azimuthal periods. The azimuthal position of the PSR J0855-4644 and the centre of the region around the southern enhan… view at source ↗
Figure 4
Figure 4. Figure 4: SED of 𝛾-ray emission towards RX J0852.0-4622 (red points) extracted from the H.E.S.S. template in the energy range from 100 MeV to 500 GeV by Fermi-LAT. Red error bars show statistical errors, and blue error bars represent the quadrature sum of statistical and systematic errors. The black data points represent the H.E.S.S. energy flux spectra taken from RX J0852.0-4622. The blue dashed line represents the… view at source ↗
Figure 5
Figure 5. Figure 5: The broadband SED of RX J0852.0-4622 with the leptonic (top) and hybrid (bottom) scenarios (see sect. 3). The radio data, shown as orange points, were adopted by Duncan & Green (2000). The green points represent the eROSITA flux extracted in the 1–5 keV band from the entire remnant, with statistical uncertainties calculated at the 68% confidence level. GeV– TeV 𝛾-ray data are the same as [PITH_FULL_IMAGE:… view at source ↗
read the original abstract

We present an updated analysis of the gigaelectronvolt (GeV) gamma-ray emission from the shell-type supernova remnant (SNR) RX J0852.0-4622 (Vela Jr) using 15 yr of Fermi Large Area Telescope (Fermi-LAT) data. We quantitatively model the GeV morphology and find that it is best described by the masked H.E.S.S. shell template, indicating that the embedded pulsar wind nebula (PWN) contributes little to the GeV flux. The 0.1-500 GeV spectrum is well fitted by a hard power law with a photon index of $1.77 \pm 0.03$ and connects smoothly to the teraelectronvolt (TeV) spectrum, confirming previous results with improved precision. We further construct an independent eROSITA shell template and derive the 1-5 keV X-ray spectral energy distribution (SED) of the whole remnant, which provides new constraints on the synchrotron emission. We model the multi-wavelength (MWL) SED with a pure leptonic model and a hybrid lepton-hadron model. While the pure leptonic model reproduces the overall broadband shape, the hybrid model provides a better statistical description of the same dataset, supporting a mixed-origin picture in which the hadronic contribution is mainly relevant in the GeV band and the TeV emission remains predominantly leptonic.

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 / 2 minor

Summary. The paper presents an updated Fermi-LAT analysis of GeV emission from SNR Vela Jr (RX J0852.0-4622) using 15 years of data. It quantitatively shows that the morphology is best described by a masked H.E.S.S. shell template (indicating negligible PWN contribution), reports a hard power-law spectrum with index 1.77 ± 0.03 that connects smoothly to the TeV band, derives a new 1-5 keV X-ray SED from an independent eROSITA shell template, and models the MWL SED with both pure leptonic and hybrid lepton-hadron scenarios, claiming the hybrid model provides a better statistical description supporting a mixed-origin picture (hadronic mainly in GeV, leptonic in TeV).

Significance. If the hybrid-model preference is shown to be robust after penalizing for extra parameters, the result would strengthen evidence for mixed leptonic-hadronic gamma-ray emission in shell-type SNRs, with direct implications for distinguishing cosmic-ray acceleration channels. The longer Fermi-LAT baseline, independent X-ray template, and quantitative morphology test add useful constraints even if the model-comparison step requires refinement.

major comments (2)
  1. [MWL SED modeling and abstract] In the MWL SED modeling section (and the abstract statement that the hybrid model 'provides a better statistical description'): no Δχ², likelihood-ratio test statistic, p-value, or penalized information criterion (AIC/BIC) is reported. Because the hybrid model necessarily introduces at least one additional free parameter (hadronic normalization, and likely a second such as proton index or cutoff), an unpenalized improvement in raw likelihood does not establish that the hadronic component is required; this is load-bearing for the central 'mixed-origin picture' claim.
  2. [Morphology modeling section] In the morphology analysis: the quantitative preference for the masked H.E.S.S. shell template assumes this template is an unbiased representation of the true GeV-emitting volume. No assessment is provided of residual background, point-source contamination, or masking artifacts after template application; this directly affects the conclusion of negligible PWN contribution at GeV energies.
minor comments (2)
  1. [Abstract and §3-4] The abstract and results text should explicitly state the background-modeling approach, the precise energy range and binning used for the Fermi-LAT spectrum, and the exact statistical metric (with value) used to compare the two SED models.
  2. [Spectral analysis and SED sections] Systematic uncertainties on the photon index, flux normalizations, and template normalizations are not discussed; adding a brief dedicated paragraph or table would improve transparency.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and constructive comments on our manuscript. We address each major comment point by point below. Revisions have been made to strengthen the statistical rigor and address potential systematics as suggested.

read point-by-point responses

  1. Referee: [MWL SED modeling and abstract] In the MWL SED modeling section (and the abstract statement that the hybrid model 'provides a better statistical description'): no Δχ², likelihood-ratio test statistic, p-value, or penalized information criterion (AIC/BIC) is reported. Because the hybrid model necessarily introduces at least one additional free parameter (hadronic normalization, and likely a second such as proton index or cutoff), an unpenalized improvement in raw likelihood does not establish that the hadronic component is required; this is load-bearing for the central 'mixed-origin picture' claim.

    Authors: We agree that an unpenalized comparison is insufficient and that a penalized criterion such as AIC is required to support the preference for the hybrid model. In the revised manuscript we have added AIC values for both models in the MWL SED section, along with the likelihood-ratio test statistic and associated p-value. The hybrid model remains preferred after the penalty for the extra hadronic normalization parameter. The abstract has been updated to state that the hybrid model provides a statistically preferred description according to the AIC. These additions directly address the concern and reinforce the mixed-origin interpretation with proper model selection. revision: yes

  2. Referee: [Morphology modeling section] In the morphology analysis: the quantitative preference for the masked H.E.S.S. shell template assumes this template is an unbiased representation of the true GeV-emitting volume. No assessment is provided of residual background, point-source contamination, or masking artifacts after template application; this directly affects the conclusion of negligible PWN contribution at GeV energies.

    Authors: We acknowledge the need for explicit checks on template fidelity. In the revised morphology section we now present residual maps after fitting the masked H.E.S.S. shell template, which show no significant structured residuals or background artifacts above the noise level within the ROI. We have also added a dedicated test in which an additional point-source component is included at the PWN position; its best-fit flux is consistent with zero, confirming negligible PWN contribution at GeV energies. These quantitative assessments address the potential for masking artifacts and contamination. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation uses independent external templates and standard emission models

full rationale

The paper fits Fermi-LAT counts to masked H.E.S.S. and independently constructed eROSITA templates to determine morphology and spectrum, then applies conventional leptonic and hybrid (lepton-hadron) emission formulas to the resulting MWL SED. The statement that the hybrid model gives a better statistical description does not reduce to a self-definitional loop, a fitted parameter renamed as a prediction, or a load-bearing self-citation chain; the templates and formulas are external to the target claim. No ansatz is smuggled via citation and no uniqueness theorem is invoked. The derivation chain remains self-contained against the external data and standard physics.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard high-energy astrophysics assumptions and several fitted parameters; no new physical entities are postulated.

free parameters (2)
  • Photon index = 1.77
    Fitted directly to the 0.1-500 GeV spectrum
  • SED model normalizations and cut-off energies
    Multiple parameters adjusted to match radio, X-ray, GeV and TeV data points in both leptonic and hybrid scenarios
axioms (2)
  • domain assumption The masked H.E.S.S. TeV shell template accurately traces the GeV-emitting region
    Invoked as the best morphological model for the Fermi-LAT data
  • domain assumption Standard leptonic and hadronic radiation processes dominate the observed emission
    Basis for constructing the two broadband SED models

pith-pipeline@v0.9.0 · 5577 in / 1568 out tokens · 47364 ms · 2026-05-10T15:25:03.730434+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

70 extracted references · 63 canonical work pages · 3 internal anchors

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  4. [4]

    A., et al., 2009, @doi [ ] 10.1088/0004-637X/706/1/L1 , https://ui.adsabs.harvard.edu/abs/2009ApJ...706L...1A 706, L1

    Abdo A. A., et al., 2009, @doi [ ] 10.1088/0004-637X/706/1/L1 , https://ui.adsabs.harvard.edu/abs/2009ApJ...706L...1A 706, L1

    work page doi:10.1088/0004-637x/706/1/l1 2009

  5. [5]

    Abdollahi S., et al., 2022, @doi [ ] 10.3847/1538-4365/ac6751 , https://ui.adsabs.harvard.edu/abs/2022ApJS..260...53A 260, 53

    work page doi:10.3847/1538-4365/ac6751 2022

  6. [6]

    Acero F., Gallant Y., Ballet J., Renaud M., Terrier R., 2013, @doi [ ] 10.1051/0004-6361/201220799 , https://ui.adsabs.harvard.edu/abs/2013A&A...551A...7A 551, A7

    work page doi:10.1051/0004-6361/201220799 2013

  7. [7]

    Ackermann M., et al., 2017, @doi [ ] 10.3847/1538-4357/aa775a , https://ui.adsabs.harvard.edu/abs/2017ApJ...843..139A 843, 139

    work page doi:10.3847/1538-4357/aa775a 2017

  8. [8]

    Aharonian F., et al., 2005, @doi [ ] 10.1051/0004-6361:200500130 , https://ui.adsabs.harvard.edu/abs/2005A&A...437L...7A 437, L7

    work page doi:10.1051/0004-6361:200500130 2005

  9. [9]

    Aharonian F., et al., 2007, @doi [ ] 10.1086/512603 , https://ui.adsabs.harvard.edu/abs/2007ApJ...661..236A 661, 236

    work page doi:10.1086/512603 2007

  10. [10]

    Aharonian F., et al., 2026, @doi [ ] 10.1051/0004-6361/202558346 , https://ui.adsabs.harvard.edu/abs/2026A&A...708A...6A 708, A6

    work page doi:10.1051/0004-6361/202558346 2026

  11. [11]

    Akaike H., 1974, IEEE Transactions on Automatic Control, https://ui.adsabs.harvard.edu/abs/1974ITAC...19..716A 19, 716

    1974

  12. [12]

    E., Chow K., DeLaney T., Filipovi \'c M

    Allen G. E., Chow K., DeLaney T., Filipovi \'c M. D., Houck J. C., Pannuti T. G., Stage M. D., 2015, @doi [ ] 10.1088/0004-637X/798/2/82 , https://ui.adsabs.harvard.edu/abs/2015ApJ...798...82A 798, 82

    work page doi:10.1088/0004-637x/798/2/82 2015

  13. [13]

    Aschenbach B., 1998, @doi [ ] 10.1038/24103 , https://ui.adsabs.harvard.edu/abs/1998Natur.396..141A 396, 141

    work page doi:10.1038/24103 1998

  14. [14]

    F., Sch \"o nfelder V., 1999, @doi [ ] 10.48550/arXiv.astro-ph/9909415 , https://ui.adsabs.harvard.edu/abs/1999A&A...350..997A 350, 997

    Aschenbach B., Iyudin A. F., Sch \"o nfelder V., 1999, @doi [ ] 10.48550/arXiv.astro-ph/9909415 , https://ui.adsabs.harvard.edu/abs/1999A&A...350..997A 350, 997

    work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/9909415 1999

  15. [15]

    B., Abdo, A

    Atwood W. B., et al., 2009, @doi [ ] 10.1088/0004-637X/697/2/1071 , https://ui.adsabs.harvard.edu/abs/2009ApJ...697.1071A 697, 1071

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

  16. [16]

    I., Leer E., Skadron G., 1977, in International Cosmic Ray Conference

    Axford W. I., Leer E., Skadron G., 1977, in International Cosmic Ray Conference. p. 132

    1977

  17. [17]

    H., Lott, B., & collaboration, T

    Ballet J., Bruel P., Burnett T. H., Lott B., The Fermi-LAT collaboration 2023, @doi [arXiv e-prints] 10.48550/arXiv.2307.12546 , https://ui.adsabs.harvard.edu/abs/2023arXiv230712546B p. arXiv:2307.12546

    work page doi:10.48550/arxiv.2307.12546 2023

  18. [18]

    Bamba A., Yamazaki R., Yoshida T., Terasawa T., Koyama K., 2005, @doi [ ] 10.1086/427620 , https://ui.adsabs.harvard.edu/abs/2005ApJ...621..793B 621, 793

    work page doi:10.1086/427620 2005

  19. [19]

    R., 1978, @doi [ ] 10.1093/mnras/182.2.147 , https://ui.adsabs.harvard.edu/abs/1978MNRAS.182..147B 182, 147

    Bell A. R., 1978, @doi [ ] 10.1093/mnras/182.2.147 , https://ui.adsabs.harvard.edu/abs/1978MNRAS.182..147B 182, 147

    work page doi:10.1093/mnras/182.2.147 1978

  20. [20]

    Blandford R., Eichler D., 1987, @doi [ ] 10.1016/0370-1573(87)90134-7 , https://ui.adsabs.harvard.edu/abs/1987PhR...154....1B 154, 1

    work page doi:10.1016/0370-1573(87)90134-7 1987

  21. [21]

    D., & Ostriker , J

    Blandford R. D., Ostriker J. P., 1978, @doi [ ] 10.1086/182658 , https://ui.adsabs.harvard.edu/abs/1978ApJ...221L..29B 221, L29

    work page doi:10.1086/182658 1978

  22. [22]

    Blasi P., 2013, @doi [ ] 10.1007/s00159-013-0070-7 , https://ui.adsabs.harvard.edu/abs/2013A&ARv..21...70B 21, 70

    work page doi:10.1007/s00159-013-0070-7 2013

  23. [23]

    and Wolfire, Mark and Leroy, Adam K

    Bolatto A. D., Wolfire M., Leroy A. K., 2013, @doi [ ] 10.1146/annurev-astro-082812-140944 , https://ui.adsabs.harvard.edu/abs/2013ARA&A..51..207B 51, 207

    work page Pith review doi:10.1146/annurev-astro-082812-140944 2013

  24. [24]

    Bruel P., 2021, @doi [ ] 10.1051/0004-6361/202141553 , https://ui.adsabs.harvard.edu/abs/2021A&A...656A..81B 656, A81

    work page doi:10.1051/0004-6361/202141553 2021

  25. [25]

    H., Digel, S

    Bruel P., Burnett T. H., Digel S. W., Johannesson G., Omodei N., Wood M., 2018, @doi [arXiv e-prints] 10.48550/arXiv.1810.11394 , https://ui.adsabs.harvard.edu/abs/2018arXiv181011394B p. arXiv:1810.11394

    work page doi:10.48550/arxiv.1810.11394 2018

  26. [26]

    Camilloni F., Becker W., Predehl P., Dennerl K., Freyberg M., Mayer M. G. F., Sasaki M., 2023, @doi [ ] 10.1051/0004-6361/202245475 , https://ui.adsabs.harvard.edu/abs/2023A&A...673A..45C 673, A45

    work page doi:10.1051/0004-6361/202245475 2023

  27. [27]

    Condon B., Lemoine-Goumard M., Acero F., Katagiri H., 2017, @doi [ ] 10.3847/1538-4357/aa9be8 , https://ui.adsabs.harvard.edu/abs/2017ApJ...851..100C 851, 100

    work page doi:10.3847/1538-4357/aa9be8 2017

  28. [28]

    , keywords =

    Dame T. M., Hartmann D., Thaddeus P., 2001, @doi [ ] 10.1086/318388 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547..792D 547, 792

    work page doi:10.1086/318388 2001

  29. [29]

    R., Green D

    Duncan A. R., Green D. A., 2000, @doi [ ] 10.48550/arXiv.astro-ph/0009289 , https://ui.adsabs.harvard.edu/abs/2000A&A...364..732D 364, 732

    work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/0009289 2000

  30. [30]

    Enomoto R., et al., 2006, @doi [ ] 10.1086/508531 , https://ui.adsabs.harvard.edu/abs/2006ApJ...652.1268E 652, 1268

    work page doi:10.1086/508531 2006

  31. [31]

    Fukui Y., et al., 2012, @doi [ ] 10.1088/0004-637X/746/1/82 , https://ui.adsabs.harvard.edu/abs/2012ApJ...746...82F 746, 82

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

  32. [32]

    Fukui Y., et al., 2017, @doi [ ] 10.3847/1538-4357/aa9219 , https://ui.adsabs.harvard.edu/abs/2017ApJ...850...71F 850, 71

    work page doi:10.3847/1538-4357/aa9219 2017

  33. [33]

    Fukui Y., Aruga M., Sano H., Hayakawa T., Inoue T., Rowell G., Einecke S., Tachihara K., 2024, @doi [ ] 10.3847/1538-4357/ad0da3 , https://ui.adsabs.harvard.edu/abs/2024ApJ...961..162F 961, 162

    work page doi:10.3847/1538-4357/ad0da3 2024

  34. [34]

    Guo X.-L., Xin Y.-L., Liao N.-H., Yuan Q., Gao W.-H., Fan Y.-Z., 2018, @doi [ ] 10.3847/1538-4357/aaa3f8 , https://ui.adsabs.harvard.edu/abs/2018ApJ...853....2G 853, 2

    work page doi:10.3847/1538-4357/aaa3f8 2018

  35. [35]

    H. E. S. S. Collaboration et al., 2018a, @doi [ ] 10.1051/0004-6361/201629377 , https://ui.adsabs.harvard.edu/abs/2018A&A...612A...2H 612, A2

    work page doi:10.1051/0004-6361/201629377

  36. [36]

    H. E. S. S. Collaboration et al., 2018b, @doi [ ] 10.1051/0004-6361/201526545 , https://ui.adsabs.harvard.edu/abs/2018A&A...612A...4H 612, A4

    work page doi:10.1051/0004-6361/201526545

  37. [37]

    H. E. S. S. Collaboration et al., 2018c, @doi [ ] 10.1051/0004-6361/201629790 , https://ui.adsabs.harvard.edu/abs/2018A&A...612A...6H 612, A6

    work page doi:10.1051/0004-6361/201629790

  38. [38]

    H. E. S. S. Collaboration et al., 2018d, @doi [ ] 10.1051/0004-6361/201630002 , https://ui.adsabs.harvard.edu/abs/2018A&A...612A...7H 612, A7

    work page doi:10.1051/0004-6361/201630002

  39. [39]

    H. E. S. S. Collaboration et al., 2018e, @doi [ ] 10.1051/0004-6361/201730737 , https://ui.adsabs.harvard.edu/abs/2018A&A...612A...8H 612, A8

    work page doi:10.1051/0004-6361/201730737

  40. [40]

    HI4PI Collaboration et al., 2016, @doi [ ] 10.1051/0004-6361/201629178 , https://ui.adsabs.harvard.edu/abs/2016A&A...594A.116H 594, A116

    work page doi:10.1051/0004-6361/201629178 2016

  41. [41]

    W., Lemoine-Goumard M., 2015, @doi [Comptes Rendus Physique] 10.1016/j.crhy.2015.08.015 , https://ui.adsabs.harvard.edu/abs/2015CRPhy..16..674H 16, 674

    Hewitt J. W., Lemoine-Goumard M., 2015, @doi [Comptes Rendus Physique] 10.1016/j.crhy.2015.08.015 , https://ui.adsabs.harvard.edu/abs/2015CRPhy..16..674H 16, 674

    work page doi:10.1016/j.crhy.2015.08.015 2015

  42. [42]

    Inoue T., Yamazaki R., Inutsuka S.-i., Fukui Y., 2012, @doi [ ] 10.1088/0004-637X/744/1/71 , https://ui.adsabs.harvard.edu/abs/2012ApJ...744...71I 744, 71

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

  43. [43]

    F., et al., 1998, @doi [ ] 10.1038/24106 , https://ui.adsabs.harvard.edu/abs/1998Natur.396..142I 396, 142

    Iyudin A. F., et al., 1998, @doi [ ] 10.1038/24106 , https://ui.adsabs.harvard.edu/abs/1998Natur.396..142I 396, 142

    work page doi:10.1038/24106 1998

  44. [44]

    F., Aschenbach B., Becker W., Dennerl K., Haberl F., 2005, @doi [ ] 10.1051/0004-6361:20041779 , https://ui.adsabs.harvard.edu/abs/2005A&A...429..225I 429, 225

    Iyudin A. F., Aschenbach B., Becker W., Dennerl K., Haberl F., 2005, @doi [ ] 10.1051/0004-6361:20041779 , https://ui.adsabs.harvard.edu/abs/2005A&A...429..225I 429, 225

    work page doi:10.1051/0004-6361:20041779 2005

  45. [46]

    G., Sanwal D., Garmire G

    Kargaltsev O., Pavlov G. G., Sanwal D., Garmire G. P., 2002b, @doi [ ] 10.1086/343852 , https://ui.adsabs.harvard.edu/abs/2002ApJ...580.1060K 580, 1060

    work page doi:10.1086/343852

  46. [47]

    Katagiri H., et al., 2005, @doi [ ] 10.1086/427980 , https://ui.adsabs.harvard.edu/abs/2005ApJ...619L.163K 619, L163

    work page doi:10.1086/427980 2005

  47. [48]

    Katsuda S., Tsunemi H., Mori K., 2008, @doi [ ] 10.1086/588499 , https://ui.adsabs.harvard.edu/abs/2008ApJ...678L..35K 678, L35

    work page doi:10.1086/588499 2008

  48. [49]

    A., & Kelner, S

    Khangulyan D., Aharonian F. A., Kelner S. R., 2014, @doi [ ] 10.1088/0004-637X/783/2/100 , https://ui.adsabs.harvard.edu/abs/2014ApJ...783..100K 783, 100

    work page doi:10.1088/0004-637x/783/2/100 2014

  49. [50]

    Kishishita T., Hiraga J., Uchiyama Y., 2013, @doi [ ] 10.1051/0004-6361/201220525 , https://ui.adsabs.harvard.edu/abs/2013A&A...551A.132K 551, A132

    work page doi:10.1051/0004-6361/201220525 2013

  50. [51]

    Kramer M., et al., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06637.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.342.1299K 342, 1299

    work page doi:10.1046/j.1365-8711.2003.06637.x 2003

  51. [52]

    F., 1977, Akademiia Nauk SSSR Doklady, https://ui.adsabs.harvard.edu/abs/1977DoSSR.234.1306K 234, 1306

    Krymskii G. F., 1977, Akademiia Nauk SSSR Doklady, https://ui.adsabs.harvard.edu/abs/1977DoSSR.234.1306K 234, 1306

    1977

  52. [53]

    Lebrun F., et al., 1983, @doi [ ] 10.1086/161440 , https://ui.adsabs.harvard.edu/abs/1983ApJ...274..231L 274, 231

    work page doi:10.1086/161440 1983

  53. [54]

    O., Ellison D

    Lee S.-H., Slane P. O., Ellison D. C., Nagataki S., Patnaude D. J., 2013, @doi [ ] 10.1088/0004-637X/767/1/20 , https://ui.adsabs.harvard.edu/abs/2013ApJ...767...20L 767, 20

    work page doi:10.1088/0004-637x/767/1/20 2013

  54. [55]

    I., et al., 2018, @doi [ ] 10.3847/1538-4357/aae082 , https://ui.adsabs.harvard.edu/abs/2018ApJ...866...76M 866, 76

    Maxted N. I., et al., 2018, @doi [ ] 10.3847/1538-4357/aae082 , https://ui.adsabs.harvard.edu/abs/2018ApJ...866...76M 866, 76

    work page doi:10.3847/1538-4357/aae082 2018

  55. [56]

    Mayer M. G. F., Becker W., Predehl P., Sasaki M., 2023, @doi [ ] 10.1051/0004-6361/202346691 , https://ui.adsabs.harvard.edu/abs/2023A&A...676A..68M 676, A68

    work page doi:10.1051/0004-6361/202346691 2023

  56. [57]

    Merloni A., et al., 2024, @doi [ ] 10.1051/0004-6361/202347165 , https://ui.adsabs.harvard.edu/abs/2024A&A...682A..34M 682, A34

    work page internal anchor Pith review doi:10.1051/0004-6361/202347165 2024

  57. [58]

    G., Allen G

    Pannuti T. G., Allen G. E., Filipovi \'c M. D., De Horta A., Stupar M., Agrawal R., 2010, @doi [ ] 10.1088/0004-637X/721/2/1492 , https://ui.adsabs.harvard.edu/abs/2010ApJ...721.1492P 721, 1492

    work page doi:10.1088/0004-637x/721/2/1492 2010

  58. [59]

    G., Sanwal D., K z ltan B., Garmire G

    Pavlov G. G., Sanwal D., K z ltan B., Garmire G. P., 2001, @doi [ ] 10.1086/323975 , https://ui.adsabs.harvard.edu/abs/2001ApJ...559L.131P 559, L131

    work page doi:10.1086/323975 2001

  59. [60]

    Petrosian V., Liu S., 2004, @doi [ ] 10.1086/421486 , https://ui.adsabs.harvard.edu/abs/2004ApJ...610..550P 610, 550

    work page doi:10.1086/421486 2004

  60. [61]

    U., Tr \"u mper J., Yorke H., eds, Roentgenstrahlung from the Universe

    Pfeffermann E., Aschenbach B., 1996, in Zimmermann H. U., Tr \"u mper J., Yorke H., eds, Roentgenstrahlung from the Universe. pp 267--268

    1996

  61. [62]

    A., Moskalenko I

    Porter T. A., Moskalenko I. V., Strong A. W., 2006, @doi [ ] 10.1086/507770 , https://ui.adsabs.harvard.edu/abs/2006ApJ...648L..29P 648, L29

    work page doi:10.1086/507770 2006

  62. [63]

    P., Edgar R

    Slane P., Hughes J. P., Edgar R. J., Plucinsky P. P., Miyata E., Tsunemi H., Aschenbach B., 2001, @doi [ ] 10.1086/319033 , https://ui.adsabs.harvard.edu/abs/2001ApJ...548..814S 548, 814

    work page doi:10.1086/319033 2001

  63. [64]

    arXiv:2512.04956

    Suherli J., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2512.04956 , https://ui.adsabs.harvard.edu/abs/2025arXiv251204956S p. arXiv:2512.04956

    work page doi:10.48550/arxiv.2512.04956 2025

  64. [65]

    S., Katsuda S., Yamazaki R., Ohira Y., Iwakiri W., 2016, @doi [ ] 10.1093/pasj/psw036 , https://ui.adsabs.harvard.edu/abs/2016PASJ...68S..10T 68, S10

    Takeda S., Bamba A., Terada Y., Tashiro M. S., Katsuda S., Yamazaki R., Ohira Y., Iwakiri W., 2016, @doi [ ] 10.1093/pasj/psw036 , https://ui.adsabs.harvard.edu/abs/2016PASJ...68S..10T 68, S10

    work page doi:10.1093/pasj/psw036 2016

  65. [66]

    Tanaka T., et al., 2011, @doi [ ] 10.1088/2041-8205/740/2/L51 , https://ui.adsabs.harvard.edu/abs/2011ApJ...740L..51T 740, L51

    work page doi:10.1088/2041-8205/740/2/l51 2011

  66. [67]

    Tsunemi H., Miyata E., Aschenbach B., Hiraga J., Akutsu D., 2000, @doi [ ] 10.1093/pasj/52.5.887 , https://ui.adsabs.harvard.edu/abs/2000PASJ...52..887T 52, 887

    work page doi:10.1093/pasj/52.5.887 2000

  67. [68]

    Xing Y., Wang Z., Zhang X., Chen Y., 2016, @doi [ ] 10.3847/0004-637X/823/1/44 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823...44X 823, 44

    work page doi:10.3847/0004-637x/823/1/44 2016

  68. [69]

    L., 2011, @doi [ ] 10.1088/0004-637X/735/2/120 , https://ui.adsabs.harvard.edu/abs/2011ApJ...735..120Y 735, 120

    Yuan Q., Liu S., Fan Z., Bi X., Fryer C. L., 2011, @doi [ ] 10.1088/0004-637X/735/2/120 , https://ui.adsabs.harvard.edu/abs/2011ApJ...735..120Y 735, 120

    work page doi:10.1088/0004-637x/735/2/120 2011

  69. [70]

    Zabalza V., 2015, in 34th International Cosmic Ray Conference (ICRC2015). p. 922 ( @eprint arXiv 1509.03319 )

    work page arXiv 2015

  70. [71]

    Zeng H., Xin Y., Zhang S., Liu S., 2021, @doi [ ] 10.3847/1538-4357/abe37e , https://ui.adsabs.harvard.edu/abs/2021ApJ...910...78Z 910, 78

    work page doi:10.3847/1538-4357/abe37e 2021