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arxiv: 1907.05397 · v1 · pith:SULXXWBYnew · submitted 2019-07-11 · 🌌 astro-ph.HE · hep-ex

Origin of gamma-ray families accompanied by halos and detected in experiments with x-ray emulsion chambers

V.S. Puchkov , S.E. Pyatovsky This is my paper

Pith reviewed 2026-05-24 22:52 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-ex
keywords gamma-ray familieshalosx-ray emulsion chamberscosmic ray mass compositionprotonsheliumPamir experiment
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The pith

Gamma-ray families with halos are produced mostly by protons and helium nuclei.

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

Experiments with x-ray emulsion chambers detect gamma-ray families that sometimes include a halo of diffuse radiation. The paper compares the observed halo properties with Monte Carlo simulations of cosmic ray interactions in the atmosphere. It concludes that over 96 percent of these halo events come from primary protons and helium nuclei rather than heavier elements. This finding opens a route to use halo measurements to determine the light nuclei fraction in the primary cosmic ray flux at high energies.

Core claim

The experimental properties of halos are analyzed via a comparison with the results of their simulation. It is shown that gamma-ray families featuring halos are predominantly produced (more than 96 % of them) by protons and helium nuclei. This makes it possible to employ the experimental properties of halos to estimate the fraction of protons and helium nuclei in the mass composition of primary cosmic radiation.

What carries the argument

Monte Carlo simulation of the development of gamma-ray families and halos from different primary cosmic ray nuclei.

Load-bearing premise

The Monte Carlo simulation accurately reproduces the experimental properties of halos for protons, helium, and heavier nuclei under the conditions of the Pamir and other XREC setups.

What would settle it

Finding that a large fraction of observed halos have characteristics that the simulation assigns only to heavy nuclei would falsify the claim that light nuclei dominate halo production.

Figures

Figures reproduced from arXiv: 1907.05397 by S.E. Pyatovsky, V.S. Puchkov.

Figure 1
Figure 1. Figure 1: Layout of the Pamir XREC (X-ray emulsion chamber) experiment [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Scanned image of the experimental halos (a) FIANIT (Shalo=1020 mm2 ), (b) Tajikistan (Shalo=1451 mm2 ), and (c) Andromeda (Shalo=950 mm2 ). The photon energy is determined from the photometry of dark spots on an x-ray film. The optical density of dark spots is proportional to the number of particles, n=f(r,t,E) µm -2 , where r is the distance that is measured from e ± and γ in EAS to the scanned cell and w… view at source ↗
Figure 3
Figure 3. Figure 3: E0 dependence of the intensity of γ-ray families with halos and relative fractions of primary￾cosmicradiation nuclei producing these halos according to the simulation [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Area spectrum of the halos obtained in the Pamir XREC experiment and the experiments of the Brazil–Japan Collaboration along with the halo area spectrum from the simulation [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: (a) Scanned image of a multicenter gamma-ray family featuring a halo from the Pamir XREC experiment (ΣEγ=1688 TeV and Shalo=46 mm2 ); (b) calculated gamma-ray family characterized by the presence of a halo and produced by a primary helium nucleus (ΣEγ=1296 TeV and Shalo=67 mm2 ), a D isogram being given; and (c) calculated halo formed by a primary proton (ΣEγ=39.5 PeV and Shalo=2100 mm2 ). The gamma-ray fa… view at source ↗
Figure 6
Figure 6. Figure 6: Calculated one-center halo that was produced by a primary iron nucleus (E0=1.63 EeV and Shalo=3783 mm2 ): (a) D isogram; (b) model image on an x-ray film, D=0.5 boundary being indicated by a white contour; and (c) three-dimensional isogram [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Calculated multicenter gamma-ray families characterized by the presence of a halo and produced by (a) a primary proton (E0=0.19 EeV, S1=529 mm2 , and S2=102 mm2 ), (b) a primary helium nucleus (E0=0.07 EeV, S1=40 mm2 , and S2=27 mm2 ), and (c) a primary iron nucleus (E0=0.69 EeV, S1=441 mm2 , and S2=21 mm2 ). 3.3. Probabilities for halo formation The calculations on the basis of the МС0 model [3] involved … view at source ↗
Figure 8
Figure 8. Figure 8: Proton and p+He fractions in the mass composition of primary cosmic radiation according to data of the KASCADE [8, 13-15], ARGO-YBJ [16], Tunka [17-21], IceCube [22], and Pamir experiments. The probabilities for the formation of gamma-ray families with halos by protons and helium nuclei differ by a factor of four. On the basis of the known numbers of experimentally observed gamma￾ray families featuring hal… view at source ↗
read the original abstract

The phenomenon of gamma-ray families featuring halos that is observed in an experiment with x-ray emulsion chambers (XREC) in the Pamir experiment and in other XREC experiments is explained. The experimental properties of halos are analyzed via a comparison with the results of their simulation. It is shown that gamma-ray families featuring halos are predominantly produced (more than 96 % of them) by protons and heliumnuclei. This makes it possible to employ the experimental properties of halos to estimate the fraction of protons and helium nuclei in the mass composition of primary cosmic radiation.

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 manuscript explains the observation of gamma-ray families with halos in XREC experiments (Pamir and others) by comparing their experimental properties to Monte Carlo simulations. It concludes that more than 96% of such families are produced by protons and helium nuclei, which would enable use of halo observables to estimate the light-component fraction in the primary cosmic-ray mass composition.

Significance. If the Monte Carlo modeling of halo formation is shown to be accurate across nuclear species, the result would provide a new experimental handle on the proton-helium fraction at energies near the knee, complementing other composition techniques. The approach is potentially useful for cosmic-ray astrophysics provided the simulation fidelity is independently validated.

major comments (2)
  1. [simulation results and comparison with data] Abstract and simulation-results section: the central 96% claim is obtained exclusively by comparing data to Monte Carlo outputs for different primaries, yet the manuscript supplies no information on the hadronic interaction models, electromagnetic-cascade treatment, parameter choices, or statistical uncertainties entering the comparison. Without these details it is impossible to judge whether the simulation correctly suppresses halo formation (or alters its observables) for A>4 under Pamir XREC conditions.
  2. [simulation results and comparison with data] Simulation-results section: the inference that heavier nuclei produce negligible matching halos rests on the untested assumption that the Monte Carlo reproduces experimental halo properties for protons, helium, and A>4 nuclei with comparable fidelity. Any systematic inaccuracy in hadronic modeling or detector response for heavier primaries would directly lower the reported light-component fraction.
minor comments (2)
  1. [Abstract] Abstract: 'heliumnuclei' should be written as two words ('helium nuclei').
  2. [Abstract] Abstract: the phrase 'other XREC experiments' is used without naming the experiments or providing references.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of the manuscript and the constructive comments regarding the simulation details. We address each major comment below and agree that the manuscript requires additional information on the Monte Carlo modeling to strengthen the presentation.

read point-by-point responses

  1. Referee: Abstract and simulation-results section: the central 96% claim is obtained exclusively by comparing data to Monte Carlo outputs for different primaries, yet the manuscript supplies no information on the hadronic interaction models, electromagnetic-cascade treatment, parameter choices, or statistical uncertainties entering the comparison. Without these details it is impossible to judge whether the simulation correctly suppresses halo formation (or alters its observables) for A>4 under Pamir XREC conditions.

    Authors: We agree that the manuscript as submitted lacks explicit details on the hadronic interaction models, electromagnetic-cascade treatment, parameter choices, and statistical uncertainties. In the revised version we will add a dedicated subsection in the simulation-results section that specifies the hadronic model employed, the electromagnetic cascade code and its parameters, the XREC detector response modeling, and the statistical uncertainties on the halo-matching fractions. This addition will allow readers to assess the suppression of halo formation for A>4 nuclei under the Pamir conditions. revision: yes

  2. Referee: Simulation-results section: the inference that heavier nuclei produce negligible matching halos rests on the untested assumption that the Monte Carlo reproduces experimental halo properties for protons, helium, and A>4 nuclei with comparable fidelity. Any systematic inaccuracy in hadronic modeling or detector response for heavier primaries would directly lower the reported light-component fraction.

    Authors: The referee is correct that the conclusion relies on the assumption of comparable simulation fidelity across primary species. While the same standard interaction models are applied uniformly, direct experimental validation of halo observables for heavy nuclei is limited. In the revision we will expand the discussion to include an explicit statement of this assumption, a qualitative assessment of possible systematic biases for A>4, and references to any cross-checks or model validations that support the robustness of the reported >96% light-component fraction. revision: yes

Circularity Check

0 steps flagged

No significant circularity; simulation-based comparison is independent

full rationale

The paper's central claim rests on comparing observed halo properties in XREC data against Monte Carlo simulations for protons, helium, and heavier nuclei. No quoted equations, self-citations, or ansatzes in the abstract or description reduce the >96% fraction to a fitted input or self-definition. The simulation is presented as an external benchmark for distinguishing primaries, making the derivation self-contained rather than tautological.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Only the abstract is available, so the ledger is limited to the explicit reliance on simulation comparison stated in the abstract.

axioms (1)
  • domain assumption The simulation model accurately reproduces the experimental properties of halos for different primary particles.
    The 96% figure and the proposed composition estimator are derived from this comparison.

pith-pipeline@v0.9.0 · 5628 in / 1120 out tokens · 23628 ms · 2026-05-24T22:52:10.857944+00:00 · methodology

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Works this paper leans on

22 extracted references · 22 canonical work pages

  1. [1]

    S. B. Shaulov, P. F. Beyl, R. U. Beysembaev, E. A. Beysembaeva, S. P. Bezshapov, A. S. Borisov, K. V. Cherdyntceva, M. M. Chernyavsky, A. P. Chubenko, O. D. Dalkarov, V. G. Denisova, A. D. Erlykin, N. V. Kabanova, E. A. Kanevskaya, K. A. Kotelnikov, A. E. Morozov, et al., in Proceedings of the 19th International Symposium on Very High Energy Cosmic Ray In...

    work page doi:10.1051/epjconf/201614517001 2016

  2. [2]

    A. S. Borisov, V. G. Denisova, Z. M. Guseva, E. A. Kanevskaya, S. E. Pyatovsky, M. G. Kogan, A. E. Morozov, R. A. Mukhamedshin, V. S. Puchkov, S. B. S haulov, G. P. Shoziyoev, and M. D. Smirnova, in Proceedings of the 19th International Symposium on Very High Energy Cosmic Ray Interactions ISVHECRI 2016, EPJ Web Conf. 145, 19008 (2017). doi 10.1051/epjcon...

    work page doi:10.1051/epjconf/201614519008 2016

  3. [3]

    Mukhamedshin, Eur

    R. Mukhamedshin, Eur. Phys. J. C 60, 345 (2009). doi 10.1140/epjc/s10052-009-0945-y

    work page doi:10.1140/epjc/s10052-009-0945-y 2009

  4. [4]

    V. S. Puchkov, A. S. Borisov, Z. M. Guseva, V. G . Denisova, E. A. Kanevskaya, M. G. Kogan, V. M. Maksimenko, A. E. Morozov, R. A. Mukhamedshin, S. E . Pyatovskii, and M. D. Smirnova, Bull. Russ. Acad. Sci.: Phys. 75, 392 (2011). doi 10.3103/S106287381103035X

    work page doi:10.3103/s106287381103035x 2011

  5. [5]

    A. S. Borisov, Z. M. Guseva, V. G. Denisova, E. A. Kanevskaya, M. G. Kogan, V.M. Maximenko, A. E. Morozov, R. A. Mukhamedshin, V. S. Puchkov, S. E . Pyatovsky, andM.D. Smirnova, in Proceedings of the 17th International Symposiumon Very High Energy Cosmic Ray Interactions ISVHECRI 2012, EPJ Web Conf. 52, 04007 (2013). doi 10.1051/epjconf/20125204007

    work page doi:10.1051/epjconf/20125204007 2012

  6. [6]

    V. S. Puchkov, A. S. Borisov, Z. M. Guseva, V. G . Denisova, E. A. Kanevskaya, M. G. Kogan, V. M. Maximenko, A. E. Morozov, R. A. Mukhamedshin, S. E. Pyatovsky, and M. D. Smirnova, in Proceedings of the 32nd International Cosmic Ray Conference, Be ijing, Aug. 11–18, 2011, Vol. 1, p. 182. doi 10.7529/ICRC2011/V01/0143

    work page doi:10.7529/icrc2011/v01/0143 2011

  7. [7]

    H. P. Dembinski, R. Engel, A. Fedynitch, Th.Gais ser, F. Riehn, and T. Stanev, in Proceedings of the 35th International Cosmic Ray Conference, 2017, PoS(ICRC2017), 533 (2017)

    work page 2017

  8. [8]

    KASCADE-Grande Collab. (S. Schoo et al.), in Proceedings of the 35th International Cosmic Ray Conference, 2017, PoS(ICRC2017), 339 (2017)

    work page 2017

  9. [9]

    Menjo, O

    H. Menjo, O. Adriani, E. Berti, L. Bonechi, M. B ongi, G. Castellini, R. D’Alessandro, M. Haguenauer, Y. Itow, K. Kasahara, K. Masuda, Y. Matsubara, Y. M uraki, K. Oohashi, P. Papini, et al., in Proceedings of the 35th International Cosmic Ray Conference, 2017, PoS(ICRC2017), 1099 (2017)

    work page 2017

  10. [10]

    Kuzmichev, I

    L. Kuzmichev, I. Astapov, P. Bezyazeekov,V. Bor eyko, A. Borodin, M. Bru Ё ckner, N. Budnev, A. Chiavassa, O. Gress, T. Gress, O. Grishin, A. Dyach ok, S. Epimakhov, O. Fedorov, A. Gafarov, V. Grebenyuk, et al., in Proceedings of the 19th International Symposium on Very High Energy Cosmic Ray Interactions ISVHECRI 2016, EPJ Web Conf. 145, 01001 (2017). do...

    work page doi:10.1051/epjconf/201614501001 2016

  11. [11]

    Kuzmichev, I

    V. Ptuskin, in Proceedings of the 19th International Symposium on Very High Energy Cosmic Ray Interactions ISVHECRI 2016, EPJ Web Conf. 145, 03001 (2017). doi 10.1051/epjconf/201614503001

    work page doi:10.1051/epjconf/201614503001 2016

  12. [12]

    Tunka-Rex Collab. (D. Kostunin et al.), in Proceedings of the 19th International Symposium on Very High Energy Cosmic Ray Interactions ISVHECRI 2016, EPJ Web Conf. 145, 11001 (2017). doi 10.1051/epjconf/201614511001

    work page doi:10.1051/epjconf/201614511001 2016

  13. [13]

    W. D. Apel, J. C. Arteaga, A. F. Badea, K. Bekk , J. Blumer, H. Bozdog, I. M. Brancus, M. Bruggemann, P. Buchholz, F. Cossavella, K. Daumille r, V. de Souza, P. Doll, R. Engel, J. Engler, M. Finger, et al., Astropart. Phys. 31, 86 (2009). doi 10.1016/j.astropartphys.2008.11.008

    work page doi:10.1016/j.astropartphys.2008.11.008 2009

  14. [14]

    Kampert and M

    K.-H. Kampert and M. Unger, Astropart. Phys. 35 , 660 (2012). doi 10.1016/j.astropartphys.2012.02.004

    work page doi:10.1016/j.astropartphys.2012.02.004 2012

  15. [15]

    W. D. Apel, J. C. Arteaga-Velazquez, K. Bekk, M . Bertaina, J. Blumer, H. Bozdog, I. M. Brancus, E. Cantoni, A. Chiavassa, F. Cossavella, K. Daumiller, V. de Souza, F. di Pierro, P. Doll, R. Engel, J. Engler, et al., Astropart. Phys. 47, 54 (2013). doi 10.1016/j.astropartphys.2013.06.004

    work page doi:10.1016/j.astropartphys.2013.06.004 2013

  16. [16]

    de Mitri (on behalf of the ARGO-YBJ Collab.) , in Proceedings of the 18th International Symposium on Very High Energy Cosmic Ray Interactio ns ISVHECRI 2014, EPJ Web Conf

    I. de Mitri (on behalf of the ARGO-YBJ Collab.) , in Proceedings of the 18th International Symposium on Very High Energy Cosmic Ray Interactio ns ISVHECRI 2014, EPJ Web Conf. 99, 08003 (2015). doi 10.1051/epjconf/20159908003

    work page doi:10.1051/epjconf/20159908003 2014

  17. [17]

    Budnev, I

    N. Budnev, I. Astapov, P. Bezyazeekov, V. Borey ko, A. Borodin, M. Brueckner,A. Chiavassa, A.Dyachok, O. Fedorov, A. Gafarov, N. Gorbunov, V. Grebenyuk, O. Gress, T. Gress, O. Grishin, A. Grinyuk, et al., in Proceedings of the 35th International Cosmic Ray Co nference, 2017, PoS(ICRC2017), 768 (2017)

    work page 2017

  18. [18]

    Tunka-Rex Collab. (O. Fedorov et al.), in Proceedings of the 35th International Cosmic Ray Conference, 2017, PoS(ICRC2017), 387 (2017)

    work page 2017

  19. [19]

    Sveshnikova, I

    L. Sveshnikova, I. Astapov, P. Bezyazeekov, V. Boreyko, A. Borodin, M. Brueckner, N. Budnev, A. Chiavassa, A. Dyachok, O. Fedorov, A. Gafarov, N. G orbunov, V. Grebenyuk, O. Gress, T. Gress, O. Grishin, et al., in Proceedings of the 35th International Cosmic Ray Co nference, 2017, PoS(ICRC2017), 677 (2017)

    work page 2017

  20. [20]

    Porelli, R

    A. Porelli, R. Wischnewski, A. Garmash, I. Asta pov, P. Bezyazeekov, V. Boreyko, A. Borodin, M. Brueckner, N. Budnev, A. Chiavassa, A. Dyachok, O. Fedorov, A. Gafarov, E. Gorbovskoy, N. Gorbunov, V. Grebenyuk, et al., in Proceedings of the 35th International Cosmic Ray Co nference, 2017, PoS(ICRC2017), 754 (2017)

    work page 2017

  21. [21]

    Postnikov, I

    E. Postnikov, I. Astapov, P. Bezyazeekov, V. Bo reyko, A. Borodin, M. Brueckner, N. Budnev, A. Chiavassa, A. Dyachok, A. S. Elshoukrofy, O. Fedoro v, A. Gafarov, A. Garmash, N. Gorbunov, V. Grebenyuk, O. Gress, et al., in Proceedings of the 35th International Cosmic Ray Co nference, 2017, PoS(ICRC2017), 756 (2017)

    work page 2017

  22. [22]

    IceCube Collab. (C. Kopper), in Proceedings of the 35th International Cosmic Ray Conference, 2017, PoS(ICRC2017), 981 (2017)

    work page 2017