Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Ror, Amit Kumar; Gupta, Rahul; Jelínek, M.; Castro-Tirado, A. J.; Hu, Y.-D.; Maleňáková, Alžběta; Štrobl, J.; Thöne, C. C.; Hudec, R.; Karpov, S. V.; Kumar, Amit; Aryan, Amar; Oates, S. R.; Fernández-García, E.; Pulgar, C. Pérez del; Caballero‐García, M. D.; Castellón, A.; Carrasco-García, Irene María; I., Pérez-García,; Terol, A. J. Reina; Rendon, F.

doi:10.3847/1538-4357/aca414

Cited by 5 publications

(1 citation statement)

References 92 publications

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“…10 The power-law decay slope is α X = 1.74 ± 0.06, and the power-law photon index is Γ X = 2.0 ± 0.14 of the X-ray afterglows. Its optical afterglow data are taken from Shrestha et al (2020), Izzo et al (2020a), andRor et al (2023). We convert the ¢ r and C band data to the R band.…”

Section: Grb 201216cmentioning

confidence: 99%

Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Zhang

Ren

Wang

et al. 2023

ApJ

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Gamma-ray bursts (GRBs) 201015A and 201216C are valuable cases where very-high-energy (VHE) gamma-ray afterglows have been detected. By analyzing their prompt emission data, we find that GRB 201216C is an extremely energetic, long GRB with a hard gamma-ray spectrum, while GRB 201015A is a relative subenergetic, soft-spectrum GRB. Attributing their radio–optical–X-ray afterglows to the synchrotron radiation of the relativistic electrons accelerated in their jets, we fit their afterglow lightcurves with the standard external shock model and infer their VHE afterglows from the synchrotron self-Compton scattering process of the electrons. It is found that the jet of GRB 201015A is midrelativistic (Γ0 = 44), surrounded by a very dense medium (n = 1202 cm−3), and the jet of GRB 201216C is ultrarelativistic (Γ0 = 331), surrounded by a moderate dense medium (n = 5 cm−3). The inferred peak luminosity of the VHE gamma-ray afterglows of GRB 201216C is approximately 10−9 erg cm−2 s−1 at 57–600 s after the GRB trigger, making it detectable with the MAGIC telescopes at a high confidence level, even though the GRB is at a redshift of 1.1. Comparing their intrinsic VHE gamma-ray lightcurves and spectral energy distributions with GRBs 180720B, 190114C, and 190829A, we show that their intrinsic peak luminosity of VHE gamma-ray afterglows at 104 s after the GRB trigger is variable from 1045 to 5 × 1048 erg s−1, and their kinetic energy, initial Lorentz factor, and medium density are diverse among bursts.

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Section: Grb 201216cmentioning

confidence: 99%

Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Zhang

Ren

Wang

et al. 2023

ApJ

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Science with a Small Two-Band UV-Photometry Mission I: Mission Description and Follow-up Observations of Stellar Transients

Werner,

Řípa,

Thöne

et al. 2024

Space Sci Rev

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This is the first in a collection of three papers introducing the science with an ultra-violet (UV) space telescope on an approximately 130 kg small satellite with a moderately fast re-pointing capability and a real-time alert communication system approved for a Czech national space mission. The mission, called Quick Ultra-Violet Kilonova surveyor—QUVIK, will provide key follow-up capabilities to increase the discovery potential of gravitational wave observatories and future wide-field multi-wavelength surveys. The primary objective of the mission is the measurement of the UV brightness evolution of kilonovae, resulting from mergers of neutron stars, to distinguish between different explosion scenarios. The mission, which is designed to be complementary to the Ultraviolet Transient Astronomy Satellite—ULTRASAT, will also provide unique follow-up capabilities for other transients both in the near- and far-UV bands. Between the observations of transients, the satellite will target other objects described in this collection of papers, which demonstrates that a small and relatively affordable dedicated UV-space telescope can be transformative for many fields of astrophysics.

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GRB 201015A: from seconds to months of optical monitoring and supernova discovery

Belkin,

Pozanenko,

Minaev

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present full photometric coverage and spectroscopic data for soft GRB 201015A with a redshift z = 0.426. Our data spans a time range of 85 days following the detection of GRB. These observations revealed an underlying supernova SN 201015A with a maximum at 8.54 ±1.48 days (rest frame) and an optical peak absolute magnitude $-19.45_{-0.47}^{+0.85}$ mag. The supernova stands out clearly, since the contribution of the afterglow at this time is not dominant, which made it possible to determine SN’s parameters. A comparison of these parameters reveals that the SN 201015A is the earliest (the minimum Tmax) known supernova associated with gamma-ray bursts. Spectroscopic observations during the supernova decay stage showed broad lines, indicating a large photospheric velocity, and identified this supernova as a type Ic-BL. Thus, the SN 201015A associated with the GRB 201015A becomes the 27th SN/GRB confirmed by both photometric and spectroscopic observations. Using the results of spectral analysis based on the available data of Fermi-GBM experiment, the parameters Ep, i = 20.0 ± 8.5 keV and Eiso = (1.1 ± 0.2) × 1050 erg were obtained. According to the position of the burst on the Ep, i–Eiso correlation, GRB 201015A was classified as a Type II (long) gamma-ray burst, which was also confirmed by the T90, i–EH diagram.

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Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Cited by 5 publications

References 92 publications

Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Science with a Small Two-Band UV-Photometry Mission I: Mission Description and Follow-up Observations of Stellar Transients

GRB 201015A: from seconds to months of optical monitoring and supernova discovery

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