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Very High Energy Afterglow of Structured Jets: GW 170817 and Prospects for Future Detections

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Clément Pellouin, Frédéric Daigne

High Energy Astrophysical Phenomena · Submitted 12 Jun 2024

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim However, we show that either a smaller viewing angle or a higher external density would make similar off-axis events detectable in the future at VHE, even above 100 Mpc with the sensitivity of the Cherenkov telescope array.

how it is stated · asserted 0.68 read the record →

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arXiv ID2406.08254 (version 2)
Pith IDDZTOFLE7, Pith's permanent record of this paper and its review
CitationCl\'ement Pellouin, Fr\'ed\'eric Daigne. "Very High Energy Afterglow of Structured Jets: GW 170817 and Prospects for Future Detections." arXiv:2406.08254 (2024). https://pith.science/paper/DZTOFLE7
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The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,580 input tokens.

What the abstract itself states, as probabilities: claims first 0.05 · states limitation 0.84 · human participants 0.01 · controlled comparison 0.08 · randomized assignment 0.01 · states quantitative result 0.66 · compares with prior results 0.85 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

We present a complete numerical model of the afterglow of a laterally structured relativistic ejecta from the radio to very high energies (VHE). This includes a self-consistent calculation of the synchrotron radiation, with its maximum frequency, and of synchrotron self-Compton (SSC) scattering that takes the Klein-Nishina regime into account. Attenuation due to pair production is also included. This model is computationally efficient and allows multi-wavelength data fitting. As a validation test, the radiative model was used to fit the broad-band spectrum of GRB 190114C at 90 s up to the TeV range. The full model was then used to fit the afterglow of GW 170817 and predict its VHE emission. We find that the SSC flux at the peak was much dimmer than the upper limit from H.E.S.S. observations. However, we show that either a smaller viewing angle or a higher external density would make similar off-axis events detectable in the future at VHE, even above 100 Mpc with the sensitivity of the Cherenkov telescope array. High external densities are expected in the case of fast mergers, but the existence of a formation channel for these binary neutron stars is still uncertain. We highlight that VHE afterglow detections would help to efficiently probe systems like this.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We present a complete numerical model of the afterglow of a laterally structured relativistic ejecta from the radio to very high energies (VHE). contribution 0.93 0.95 0.05 asserted 1.00
s1 This includes a self-consistent calculation of the synchrotron radiation, with its maximum frequency, and of synchrotron self-Compton (SSC) scattering that takes the Klein-Nishina regime into account. method 0.95 0.86 0.02 asserted 0.99
s2 Attenuation due to pair production is also included. method 0.98 0.70 0.02 asserted 1.00
s3 This model is computationally efficient and allows multi-wavelength data fitting. method 0.77 0.72 0.03 asserted 1.00
s4 As a validation test, the radiative model was used to fit the broad-band spectrum of GRB 190114C at 90 s up to the TeV range. method 0.87 0.92 0.03 asserted 1.00
s5 The full model was then used to fit the afterglow of GW 170817 and predict its VHE emission. contribution 0.55 0.95 0.08 asserted 1.00
s6 We find that the SSC flux at the peak was much dimmer than the upper limit from H.E.S.S. observations. result 1.00 0.95 0.22 asserted 1.00
s7 However, we show that either a smaller viewing angle or a higher external density would make similar off-axis events detectable in the future at VHE, even above 100 Mpc with the sensitivity of the Cherenkov telescope array. interpretation 0.72 0.89 0.69 asserted 0.68
s8 High external densities are expected in the case of fast mergers, but the existence of a formation channel for these binary neutron stars is still uncertain. background 0.40 0.08 0.05 asserted 0.52
s9 We highlight that VHE afterglow detections would help to efficiently probe systems like this. interpretation 0.81 0.23 0.21 asserted 0.64

What kind of paper the classifier reports this is: simulation study 0.67 · evidence from simulation or computation 0.98.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

We present a complete numerical model of the afterglow of a laterally structured relativistic ejecta from the radio to very high energies (VHE). This includes a self-consistent calculation of the synchrotron radiation, with its maximum frequency, and of synchrotron self-Compton (SSC) scattering that takes the Klein-Nishina regime into account. Attenuation due to pair production is also included. This model is computationally efficient and allows multi-wavelength data fitting. As a validation test, the radiative model was used to fit the broad-band spectrum of GRB 190114C at 90 s up to the TeV range. The full model was then used to fit the afterglow of GW 170817 and predict its VHE emission. We find that the SSC flux at the peak was much dimmer than the upper limit from H.E.S.S. observations. However, we show that either a smaller viewing angle or a higher external density would make similar off-axis events detectable in the future at VHE, even above 100 Mpc with the sensitivity of the Cherenkov telescope array. High external densities are expected in the case of fast mergers, but the existence of a formation channel for these binary neutron stars is still uncertain. We highlight that VHE afterglow detections would help to efficiently probe systems like this.

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