GRB 221009A: The BOAT

Burns, E.; Svinkin, D.; Fenimore, E. E.; Канн, Д. А.; Fernández, J. F. Agüı́; Frederiks, D.; Hamburg, R.; Lesage, S.; Temiraev, Yuri; Tsvetkova, A. E.; Bissaldi, E.; Briggs, M. S.; Dalessi, Sarah; Dunwoody, Rachel; Fletcher, Cori; Goldstein, A.; Hui, C. M.; Hristov, Boyan; Kocevski, D.; Lysenko, A.; Mailyan, B.; Mangan, Joseph; McBreen, S.; Racusin, J. L.; Ridnaia, A.; Roberts, O. J.; Ulanov, M.; Vereš, P.; Wilson-Hodge, C.; Wood, J.

doi:10.3847/2041-8213/acc39c

Cited by 68 publications

(51 citation statements)

References 80 publications

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“…Thus, GRB 221009A is at the extreme end of the bright GRB population being simultaneously very longduration and hard-spectrum. A more detailed analysis of GRB 221009A in the context of the bright GRB population is presented in a separate paper (Burns et al 2023).…”

Section: Prompt Emission In Contextmentioning

confidence: 99%

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

Frederiks

Svinkin

Lysenko

et al. 2023

ApJL

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We report on Konus-WIND (KW) and Mikhail Pavlinsky Astronomical Roentgen Telescope – X-ray Concentrator (ART-XC) observations and analysis of a nearby GRB 221009A, the brightest γ-ray burst (GRB) detected by KW for >28 yr of observations. The prompt, pulsed phase of the burst emission lasts for ∼600 s and is followed by a steady power-law decay lasting for more than 25 ks. From the analysis of the KW and ART-XC light curves and the KW spectral data, we derive time-averaged spectral peak energy of the burst E p ≈ 2.6 MeV, E p at the brightest emission peak ≈ 3.0 MeV, the total 20 keV–10 MeV energy fluence of ≈0.22 erg cm−2, and the peak energy flux in the same band of ≈0.031 erg cm−2 s−1. The enormous observed fluence and peak flux imply, at redshift z = 0.151, huge values of isotropic energy release E iso ≈ 1.2 × 1055 erg (or ≳6.5 solar rest mass) and isotropic peak luminosity L iso ≈ 3.4 × 1054 erg s−1 (64 ms scale), making GRB 221009A the most energetic and one of the most luminous bursts observed since the beginning of the GRB cosmological era in 1997. The isotropic energetics of the burst fit nicely both “Amati” and “Yonetoku” hardness–intensity correlations for >300 KW long GRBs, implying that GRB 221009A is most likely a very hard, super-energetic version of a “normal” long GRB.

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Section: Prompt Emission In Contextmentioning

confidence: 99%

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

Frederiks

Svinkin

Lysenko

et al. 2023

ApJL

Self Cite

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“…With a geometric extrapolation of the total fluence and peak flux distributions, Burns et al (2023) argue that GRB 221009A appears to be a once-in-10,000 yr event. Given that the most prominent characteristic of GRB 221009A is its exceedingly high total isotropic energy, our objective is to ascertain the predictability and low probability of its occurrence through a comprehensive examination of the energy/luminosity functions of GRBs.…”

Section: Introductionmentioning

confidence: 97%

GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties

Lin

Liu

Xiao

et al. 2023

ApJL

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The gamma-ray burst GRB 221009A, known as the “brightest of all time,” is the closest energetic burst detected so far, with an energy of E γ,iso ∼ 1055 erg. This study aims to assess its compatibility with known GRB energy and luminosity distributions. Our analysis indicates that the energy/luminosity function of GRBs is consistent across various redshift intervals, and that the inclusion of GRB 221009A does not significantly impact the function at low redshifts. Additionally, our evaluation of the best-fitting result of the entire GRB sample suggests that the expected number of GRBs with energy greater than 1055 erg at a low redshift is 0.2, so that the emergence of GRB 221009A is consistent with expected energy/luminosity functions within ∼2σ Poisson fluctuation error, still adhering to the principles of small number statistics. Furthermore, we find that GRB 221009A and other energetic bursts, defined as E γ,iso ≳ 1054 erg, exhibit no significant differences in terms of distributions of T 90, minimum timescale, Amati relation, E γ,iso–E X,iso relation, L γ,iso–Γ0 relation, E γ,iso–Γ0 relation, L γ,iso–E p,i–Γ0 relation, and host galaxy properties, compared to normal long GRBs. This suggests that energetic GRBs (including GRB 221009A) and other long GRBs likely have similar progenitor systems and undergo similar energy dissipation and radiation processes. The generation of energetic GRBs may be due to more extreme central engine properties or, more likely, a rarer viewing configuration of a quasi-universal structured jet.

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“…GRB 221009A is extraordinarily bright, with isotropic prompt emission energy E γ,iso ; 1.5 × 10 55 erg (An et al 2023;Yang et al 2023) with redshift z = 0.151 (Castro-Tirado et al 2022;de Ugarte Postigo et al 2022b;Malesani et al 2023). Very energetic GRBs at such close distances are estimated to occur only once in a century (Atteia 2022) or even 10,000 yr (Burns et al 2023), and it is possible to detect very high energy (VHE) photons (Xue et al 2009). As expected, China's Large High Altitude Air Shower Observatory recorded at least tens of thousands of photon signals in the VHE region above 100 GeV, including photons with energy greater than 10 TeV (Huang et al 2022), which can give the finest measurement of the light curve in the highest energy band of GRBs.…”

Section: Introductionmentioning

confidence: 99%

The Possibility of Modeling the Very High Energy Afterglow of GRB 221009A in a Wind Environment

Ren

Wang

Zhang

et al. 2023

ApJ

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In this paper, we model the dynamics and radiation physics of the rarity event GRB 221009A afterglow in detail. By introducing a top-hat jet that propagates in an environment dominated by stellar winds, we explain the publicly available observations of afterglow associated with GRB 221009A over the first week. It is predicted that GRB 221009A emits a luminous very high energy afterglow based on the synchrotron self-Compton (SSC) process in our model. We show the broadband spectral energy distribution (SED) analysis results of GRB 221009A and find that the SSC radiation component of GRB 221009A is very bright in the 0.1–10 TeV band. The integrated SED shows that the SSC emission in the TeV band has detection sensitivity significantly higher than that of LHASSO, MAGIC, and CTA. However, since the release of further observations, deviations from the standard wind environment model have gradually shown up in data. For example, the late-time multiband afterglow cannot be consistently explained under the standard wind environment scenario. It may be necessary to consider modeling with a structured jet with complex geometry or a partial revision of the standard model. Furthermore, we find that the inclusion of GeV observations could break the degeneracy between model parameters, highlighting the significance of high-energy observations in determining accurate parameters for GRB afterglows.

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GRB 221009A: The BOAT

Cited by 68 publications

References 80 publications

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties

The Possibility of Modeling the Very High Energy Afterglow of GRB 221009A in a Wind Environment

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