pith. machine review for the scientific record. sign in

arxiv: 2604.27671 · v2 · submitted 2026-04-30 · 🌌 astro-ph.HE

Recognition: no theorem link

Long-term study of the gamma-ray emission of Cygnus X-3 with MAGIC and Fermi-LAT

A. Abhishek, A. Aguasca-Cabot, A. Arbet Engels, A. Babi\'c, A. Berti, A. Biland, A. Campoy-Ordaz, A. Carosi, A. Cervi\~no, A. Chilingarian, A. Cifuentes Santos, A. De Angelis, A. Dinesh, A. Donini, A. Hahn, A. J. Castro-Tirado, A. Lamastra, A. L\'opez-Oramas, A. Moralejo, A. Negro, A. Okumura, A. Roy, A. Sciaccaluga, A. Simongini, A. Stamerra, A. Tutone, A. Vigliano, B. De Lotto, C. Arcaro, C. Bakshi, C. Bigongiari, C. Campa, C. F. Vigorito, C. Nanci, C. Nigro, C. Walther, D. Cerasole, D. Dominis Prester, D. Dorner, D. Elsaesser, D. Hadasch, D. Hrupec, D. Israyelyan, D. Mazin, D. Miceli, D. Paneque, D. Sobczynska, D. Strom, E. Bernardini, E. Bronzini, E. Lindfors, E. Lyard, E. Molina, E. Prandini, E. Visentin, F. Dazzi, F. Di Pierro, F. Fr\'ias Garc\'ia-Lago, F. Giordano, F. G. Saturni, F. Longo, F. Podobnik, F. Schiavone, F. Wersig, G. Bonnoli, G. Ceribella, G. Chon, G. D'Amico, G. Harutyunyan, G. Maneva, G. Silvestri, G. Verna, H. A. Mondal, H. Kubo, I. Agudo, I. Albanese, I. Batkovi\'c, I. Burelli, I. Jim\'enez Mart\'inez, I. Viale, I. Vovk, J. A. Barrio, J. Abhir, J. Baxter, J. Becerra Gonz\'alez, J. Bernete, J. Besenrieder, J. Cortina, J. Delgado, J. G. Giesbrecht Paiva, J. G. Green, J. Herrera Llorente, J. Jahanvi, J. Jim\'enez Quiles, J. Konrad, J. Kushida, J. L. Contreras, J. M\'endez Gallego, J. M. Miranda, J. M. Paredes, J. Otero-Santos, J. Rico, J. Sitarek, J. Stri\v{s}kovi\'c, J. Tartera Barber\`a, K. Abe, K. Schmitz, L. A. Antonelli, L. Barrios-Jim\'enez, L. Di Venere, L. Eisenberger, L. Foffano, L. Font, L. Luli\'c, L. Nikoli\'c, M. Carretero-Castrillo, M. Delfino, M. Doro, M. Gaug, M. L\'ainez, M. L\'opez-Moya, M. Makariev, M. Manganaro, M. Mariotti, M. Mart\'inez, M. Molero Gonz\'alez, M. Nievas Rosillo, M. Peresano, M. Persic, M. Pihet, M. Rib\'o, M. Strzys, M. Teshima, M. Vazquez Acosta, M. Vorbrugg, N. Giglietto, N. Godinovi\'c, N. Sahakyan, O. Blanch, P. Bordas, P. Da Vela, P. Gliwny, P. G. Prada Moroni, P. G\"unther, P. K. H. Yeung, P. Majumdar, P. Maru\v{s}evec, P. M. Kouch, P. Temnikov, R. Carosi, R. Di Tria, R. Grau, R. L\'opez-Coto, R. Mirzoyan, R. Paoletti, R. Takeishi, R. Walter, S. Abe, S. Ansoldi, S. Covino, S. Fr\"ose, S. Garc\'ia Soto, S. Kankkunen, S. Lombardi, S. Loporchio, S. Mangano, S. Menchiari, S. Menon, S. Nozaki, S. Paiano, S. Ubach, S. Ventura, T. Aniello, T. Gradetzke, T. Hassan, T. Schweizer, T. Terzi\'c, T. T. H. Arnesen, U. Barres de Almeida, V. A. Acciari, V. Bosch-Ramon, V. Neustroev, V. Vitale, \v{Z}. Bo\v{s}njak, W. Bednarek, W. Rhode, Y. Fukazawa, Y. Suda

Authors on Pith no claims yet

Pith reviewed 2026-05-11 01:45 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords Cygnus X-3gamma-ray emissionMAGIC telescopesFermi-LATmicroquasarupper limitsTeV energiesflaring states
0
0 comments X

The pith

No significant TeV gamma-ray emission from Cygnus X-3 is detected across 130 hours of MAGIC observations from 2013 to 2024.

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

The paper examines the gamma-ray behavior of the microquasar Cygnus X-3, a binary system with a compact object orbiting a Wolf-Rayet star that has shown GeV and PeV emission during flares. MAGIC telescope data totaling 130 hours, the largest sample at TeV energies, are analyzed together with simultaneous Fermi-LAT data, with observations split by flaring state and orbital phase. No significant signal appears between 0.1 and 7 TeV in any subset, and the resulting upper limits on flux are the most stringent yet at these energies. These limits provide new constraints on the mechanisms that accelerate particles to high energies in this distinctive system.

Core claim

No significant detection of Cygnus X-3 is found between 0.1 and 7 TeV for any of the datasets, and differential and integral flux upper limits are reported over the long-term monitoring of the source. The MAGIC upper limits presented in this work represent the most constraining ones up to date at ~TeV energies. The Fermi-LAT fluxes can be considered compatible with previous results, taking into account the different data samples used across studies. An eventual detection of Cygnus X-3 at these energies would significantly constrain the source properties, and is not unreasonable to expect given that the source has already been detected in both the GeV and PeV regimes during flaring states.

What carries the argument

Point-like analysis of MAGIC telescope data combined with Fermi-LAT observations, segmented by flaring state and orbital phase, to derive differential and integral flux upper limits.

Load-bearing premise

Background subtraction, instrument response functions, and the identification of flaring states from other wavelengths are accurate enough that any undetected signal would not exceed the reported upper limits.

What would settle it

A statistically significant excess of gamma rays from the direction of Cygnus X-3 in the 0.1-7 TeV energy range that exceeds the reported MAGIC upper limits.

Figures

Figures reproduced from arXiv: 2604.27671 by A. Abhishek, A. Aguasca-Cabot, A. Arbet Engels, A. Babi\'c, A. Berti, A. Biland, A. Campoy-Ordaz, A. Carosi, A. Cervi\~no, A. Chilingarian, A. Cifuentes Santos, A. De Angelis, A. Dinesh, A. Donini, A. Hahn, A. J. Castro-Tirado, A. Lamastra, A. L\'opez-Oramas, A. Moralejo, A. Negro, A. Okumura, A. Roy, A. Sciaccaluga, A. Simongini, A. Stamerra, A. Tutone, A. Vigliano, B. De Lotto, C. Arcaro, C. Bakshi, C. Bigongiari, C. Campa, C. F. Vigorito, C. Nanci, C. Nigro, C. Walther, D. Cerasole, D. Dominis Prester, D. Dorner, D. Elsaesser, D. Hadasch, D. Hrupec, D. Israyelyan, D. Mazin, D. Miceli, D. Paneque, D. Sobczynska, D. Strom, E. Bernardini, E. Bronzini, E. Lindfors, E. Lyard, E. Molina, E. Prandini, E. Visentin, F. Dazzi, F. Di Pierro, F. Fr\'ias Garc\'ia-Lago, F. Giordano, F. G. Saturni, F. Longo, F. Podobnik, F. Schiavone, F. Wersig, G. Bonnoli, G. Ceribella, G. Chon, G. D'Amico, G. Harutyunyan, G. Maneva, G. Silvestri, G. Verna, H. A. Mondal, H. Kubo, I. Agudo, I. Albanese, I. Batkovi\'c, I. Burelli, I. Jim\'enez Mart\'inez, I. Viale, I. Vovk, J. A. Barrio, J. Abhir, J. Baxter, J. Becerra Gonz\'alez, J. Bernete, J. Besenrieder, J. Cortina, J. Delgado, J. G. Giesbrecht Paiva, J. G. Green, J. Herrera Llorente, J. Jahanvi, J. Jim\'enez Quiles, J. Konrad, J. Kushida, J. L. Contreras, J. M\'endez Gallego, J. M. Miranda, J. M. Paredes, J. Otero-Santos, J. Rico, J. Sitarek, J. Stri\v{s}kovi\'c, J. Tartera Barber\`a, K. Abe, K. Schmitz, L. A. Antonelli, L. Barrios-Jim\'enez, L. Di Venere, L. Eisenberger, L. Foffano, L. Font, L. Luli\'c, L. Nikoli\'c, M. Carretero-Castrillo, M. Delfino, M. Doro, M. Gaug, M. L\'ainez, M. L\'opez-Moya, M. Makariev, M. Manganaro, M. Mariotti, M. Mart\'inez, M. Molero Gonz\'alez, M. Nievas Rosillo, M. Peresano, M. Persic, M. Pihet, M. Rib\'o, M. Strzys, M. Teshima, M. Vazquez Acosta, M. Vorbrugg, N. Giglietto, N. Godinovi\'c, N. Sahakyan, O. Blanch, P. Bordas, P. Da Vela, P. Gliwny, P. G. Prada Moroni, P. G\"unther, P. K. H. Yeung, P. Majumdar, P. Maru\v{s}evec, P. M. Kouch, P. Temnikov, R. Carosi, R. Di Tria, R. Grau, R. L\'opez-Coto, R. Mirzoyan, R. Paoletti, R. Takeishi, R. Walter, S. Abe, S. Ansoldi, S. Covino, S. Fr\"ose, S. Garc\'ia Soto, S. Kankkunen, S. Lombardi, S. Loporchio, S. Mangano, S. Menchiari, S. Menon, S. Nozaki, S. Paiano, S. Ubach, S. Ventura, T. Aniello, T. Gradetzke, T. Hassan, T. Schweizer, T. Terzi\'c, T. T. H. Arnesen, U. Barres de Almeida, V. A. Acciari, V. Bosch-Ramon, V. Neustroev, V. Vitale, \v{Z}. Bo\v{s}njak, W. Bednarek, W. Rhode, Y. Fukazawa, Y. Suda.

Figure 1
Figure 1. Figure 1: Multiwavelength light curve of Cygnus X-3 at different energy ranges. From top to bottom, the panels show the LHAASO UHE flux above 100 TeV in bins of 30 days, the view at source ↗
Figure 2
Figure 2. Figure 2: Orbital LCs of Cygnus X-3 during flaring states. Two full view at source ↗
Figure 3
Figure 3. Figure 3: Gamma-ray SEDs of Cygnus X-3 for the Global (top view at source ↗
read the original abstract

Cygnus X-3 is a microquasar composed of a compact object of unknown nature closely orbiting around a Wolf-Rayet star. The particularities of this source make it a unique case among microquasars. This fact, together with its recent establishment as a PeV particle accelerator, makes Cygnus X-3 a very interesting target for the investigation of the physical processes leading to gamma-ray production. In this work, the TeV and GeV gamma-ray emission of Cygnus X-3 is studied in order to determine its origin and constrain the properties of the system. For that purpose, a point-like analysis of 130 h of data taken with the MAGIC telescopes between 2013 and 2024 was performed, which represents the largest available sample for Cygnus X-3 at $\sim$TeV energies. Additionally, contemporary data from Fermi-LAT were also analysed to better contextualize the MAGIC observations. For a more detailed investigation of the source physics, the data were divided into three subsets according to the flaring state of the source and orbital phase. No significant detection of Cygnus X-3 is found between 0.1 and 7 TeV for any of the datasets, and differential and integral flux upper limits are reported over the long-term monitoring of the source. The Fermi-LAT fluxes can be considered compatible with previous results, taking into account the different data samples used across studies. The MAGIC upper limits presented in this work represent the most constraining ones up to date at $\sim$TeV energies. An eventual detection of Cygnus X-3 at these energies would significantly constrain the source properties, and is not unreasonable to expect given that the source has already been detected in both the GeV and PeV regimes during flaring states. Further observations of Cygnus X-3 at energies above tens of GeV would be valuable for this purpose.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 3 minor

Summary. The manuscript reports results from a long-term monitoring campaign of the microquasar Cygnus X-3 using 130 hours of MAGIC telescope data collected between 2013 and 2024, together with contemporaneous Fermi-LAT observations. No significant gamma-ray detection is found in the 0.1–7 TeV range for the full dataset or for subsets divided according to flaring state and orbital phase. Differential and integral flux upper limits are presented, with the MAGIC limits stated to be the most constraining available at TeV energies; the Fermi-LAT fluxes are reported as compatible with earlier measurements.

Significance. If the upper limits are robust, the work supplies valuable constraints on particle acceleration and gamma-ray production in Cygnus X-3, a source already established as a GeV flarer and PeVatron. The long baseline and state-resolved analysis help characterize the source’s high-energy behavior across activity levels, informing emission models for microquasars and guiding expectations for future very-high-energy detections.

major comments (1)
  1. [Results] Results section: the claim that the MAGIC upper limits are the most constraining to date at ∼TeV energies is load-bearing for the paper’s impact but is not supported by a quantitative comparison table or text that lists previous limits (e.g., from VERITAS or H.E.S.S.) together with the exact energy bins, exposure, and limit values used for the comparison.
minor comments (3)
  1. [Abstract] Abstract: the phrasing 'not unreasonable to expect' is informal; a more precise statement such as 'remains plausible given the source’s GeV and PeV detections' would improve tone.
  2. [Data analysis] Data analysis: the criteria used to classify flaring states from multi-wavelength monitoring and the exact orbital-phase binning scheme should be stated explicitly, including any thresholds or reference papers for state identification.
  3. [Fermi-LAT analysis] Fermi-LAT section: specify the precise time intervals, event class, and energy range employed so that compatibility with prior Fermi-LAT results can be verified quantitatively.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the positive evaluation of our manuscript and for the constructive comment. We address the major point below and will incorporate the suggested revision.

read point-by-point responses

  1. Referee: Results section: the claim that the MAGIC upper limits are the most constraining to date at ∼TeV energies is load-bearing for the paper’s impact but is not supported by a quantitative comparison table or text that lists previous limits (e.g., from VERITAS or H.E.S.S.) together with the exact energy bins, exposure, and limit values used for the comparison.

    Authors: We agree that an explicit quantitative comparison strengthens the claim. In the revised manuscript we will add a dedicated table (and accompanying text) in the Results section that directly compares our differential and integral upper limits with all previously published limits from VERITAS, H.E.S.S., and other IACTs. The table will list, for each energy bin or integral threshold, the exposure, observation period, and numerical limit value, allowing a transparent assessment of which dataset provides the most stringent constraint at each energy. revision: yes

Circularity Check

0 steps flagged

Purely observational non-detection; no derivation chain present

full rationale

The paper reports MAGIC and Fermi-LAT observations of Cygnus X-3, splits data by flaring state and orbital phase, performs a standard point-like analysis, finds no significant detection, and quotes differential/integral upper limits. No mathematical model, fitted parameters, ansatz, uniqueness theorem, or self-referential equation is invoked. The central result (non-detection and most constraining TeV limits) is a direct data product, not a prediction derived from prior results within the paper. Self-citations, if any, are limited to instrument descriptions or prior observations and are not load-bearing for the reported limits. This matches the default expectation of zero circularity for observational astronomy papers.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard domain assumptions in high-energy astrophysics data analysis rather than new free parameters, axioms unique to the paper, or invented entities.

axioms (1)
  • domain assumption Standard assumptions in gamma-ray astronomy for background subtraction, instrument response functions, and point-source modeling hold for MAGIC and Fermi-LAT data.
    Invoked implicitly when reporting non-detections and upper limits from observational data.

pith-pipeline@v0.9.0 · 6785 in / 1291 out tokens · 39680 ms · 2026-05-11T01:45:48.260667+00:00 · methodology

Review history (2 revisions) →

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

4 extracted references · 4 canonical work pages

  1. [1]

    Planck 2018 results

    A&A 538, A63. doi:10.1051/0004-6361/ 201016129,arXiv:1111.4960. Cao, X., Zdziarski, A.A., 2020. Jets in the soft state in Cyg X-3 caused by advection of the donor mag- netic field and unification with low-mass X-ray binaries. MNRAS 492, 223–231. doi:10.1093/mnras/stz3447, arXiv:1910.01377. Corbel, S., et al., 2012. A giant radio flare from Cygnus X-3 with...

    work page doi:10.1051/0004-6361/ 2020

  2. [2]

    Homan, J., Belloni, T., 2005

    doi:10.1103/PhysRev.155.1404. Homan, J., Belloni, T., 2005. The Evolution of Black Hole States. Ap&SS 300, 107–117. doi:10.1007/ s10509-005-1197-4,arXiv:astro-ph/0412597. Khangulyan, D., Aharonian, F.A., Kelner, S.R., 2014. Simple Analytical Approximations for Treatment of In- verse Compton Scattering of Relativistic Electrons in the Blackbody Radiation F...

    work page doi:10.1103/physrev.155.1404 2005

  3. [3]

    doi:10.3847/1538-4357/aab848, arXiv:1803.06703

    ApJ 857, 123. doi:10.3847/1538-4357/aab848, arXiv:1803.06703. Li, T.P., Ma, Y.Q., 1983. Analysis methods for results in gamma-ray astronomy. ApJ 272, 317–324. doi:10.1086/ 161295. Marti, J., Paredes, J.M., Estalella, R., 1992. Modelling Cygnus X-3 radio outbursts : particle injection into twin jets. A&A 258, 309. Martí, J., Paredes, J.M., Peracaula, M., 2...

    work page doi:10.3847/1538-4357/aab848 1983

  4. [4]

    , keywords =

    doi:10.1146/annurev.astro.44.051905.092532, arXiv:astro-ph/0606352. Richards, J.L., et al., 2011. Blazars in the Fermi Era: The OVRO 40 m Telescope Monitoring Pro- gram. ApJS 194, 29. doi:10.1088/0067-0049/194/2/ 29,arXiv:1011.3111. Rolke, W.A., López, A.M., Conrad, J., 2005. Limits and confidence intervals in the presence of nuisance param- eters. Nuclea...

    work page doi:10.1146/annurev.astro.44.051905.092532 2011