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Abstract <p>The AVS-F catalog contains several dozen γ-ray bursts (GRBs), the NATALYA-2M consists of 6 bursts (maximum photon energies ∼150 and ∼60 MeV, respectively), and the Fermi/LAT catalog contains more than 200 bursts in the range <i>E</i> &gt; 100 MeV. Different behavior of the prompt emission time profiles is observed in the high and low energy ranges during some events with a high-energy spectral component. When using parameter <i>R</i><sub>t</sub> (the ratio of the time of arrival of γ-photons with maximum energy to the duration of a burst), which does not require considering the cosmological length of dilation, the following groups can be distinguished among long bursts: (1) For ∼25% of all GRBs, the duration of high-energy emission is shorter than that of the low-energy range. (2) The opposite situation is observed for the remaining ∼75%, but the maximum energy in γ-rays is detected during (2a) a low-energy prompt emission or (2b) after it is complete. The characteristics of GRBs with γ-rays in the sub-TeV region are similar to types 2a and 2b, since there is no significant correlation between their maximum energies and redshifts.</p>

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Properties of GRB High-Energy Gamma Rays from Fermi/LAT, CORONAS-F/AVS-F, and PHOTON/NATALYA-2M Data

  • 期刊论文

  • 发表日期：

    2025年6月1日

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  • I. V. Arkhangelskaja,
  • A. I. Arkhangelskiy

摘要

Abstract

The AVS-F catalog contains several dozen γ-ray bursts (GRBs), the NATALYA-2M consists of 6 bursts (maximum photon energies ∼150 and ∼60 MeV, respectively), and the Fermi/LAT catalog contains more than 200 bursts in the range E > 100 MeV. Different behavior of the prompt emission time profiles is observed in the high and low energy ranges during some events with a high-energy spectral component. When using parameter Rt (the ratio of the time of arrival of γ-photons with maximum energy to the duration of a burst), which does not require considering the cosmological length of dilation, the following groups can be distinguished among long bursts: (1) For ∼25% of all GRBs, the duration of high-energy emission is shorter than that of the low-energy range. (2) The opposite situation is observed for the remaining ∼75%, but the maximum energy in γ-rays is detected during (2a) a low-energy prompt emission or (2b) after it is complete. The characteristics of GRBs with γ-rays in the sub-TeV region are similar to types 2a and 2b, since there is no significant correlation between their maximum energies and redshifts.