The peak-flux of GRB 221009A measured with GRBAlpha

Řípa, J.; Takahashi, H.; Fukazawa, Yasushi; Werner, Norbert; Münz, F.; Pál, András; Ohno, M.; Dafcikova, Marianna; Mészáros, László; Csák, B.; Husarikova, Nikola; Kolář, Martin; Galgóczi, Gábor; Breuer, Jean-Paul; Hroch, Filip; Hudec, Ján; Kapus, Jakub; Frajt, Marcel; Rezenov, Maksim; Laszlo, Robert; Koleda, Martin; Šmelko, Miroslav; Hanák, Péter; Lipovský, Pavol; Urbanec, Tomas; Kasal, Miroslav; Povalač, Aleš; Uchida, Yuusuke; Poon, H.; Matake, Hiroto; Nakazawa, K.; Uchida, Naoshige; Bozóki, Tamás; Dálya, G.; Enoto, T.; Frei, Z.; Friss, Gergely; Ichinohe, Yuto; Kapas, Kornel; Kiss, L. L.; Mizuno, T.; Odaka, Hirokazu; Takátsy, János; Topinka, M.; Torigoe, Kento

doi:10.48550/arxiv.2302.10047

Cited by 8 publications

(9 citation statements)

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“…On 9 October 2022 at 13:16:59 UT (hereafter referred to as T 0 ), the Gamma-ray Burst Monitor (GBM) aboard Fermi (6), among other high-energy satellites [Konus-Wind, SRG, and GRBAlpha; (7,8)], detected an unprecedented, extremely bright burst lasting hundreds of seconds. This burst, dubbed GRB 221009A, is the brightest GRB ever detected in nearly 55 years of operating gamma-ray observatories, with an observed fluence of ≈5 × 10 −2 erg cm −2 in the 20-keV to 10-MeV band, more than an order of magnitude brighter than GRB 840304 and GRB 130427A (9), the previous record holders (Fig.…”

Section: Introductionmentioning

confidence: 99%

A structured jet explains the extreme GRB 221009A

et al. 2023

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Long-duration gamma-ray bursts (GRBs) are powerful cosmic explosions, signaling the death of massive stars. Among them, GRB 221009A is by far the brightest burst ever observed. Because of its enormous energy ( E iso ≈ 10 55 erg) and proximity ( z ≈ 0.15), GRB 221009A is an exceptionally rare event that pushes the limits of our theories. We present multiwavelength observations covering the first 3 months of its afterglow evolution. The x-ray brightness decays as a power law with slope ≈ t −1.66 , which is not consistent with standard predictions for jetted emission. We attribute this behavior to a shallow energy profile of the relativistic jet. A similar trend is observed in other energetic GRBs, suggesting that the most extreme explosions may be powered by structured jets launched by a common central engine.

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Section: Introductionmentioning

confidence: 99%

A structured jet explains the extreme GRB 221009A

et al. 2023

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“…The presence of dust at such large distances is confirmed by the XMM-Newton observations performed more than 20 days after the GRB (B. Vaia et al 2023, in preparation). 22 An even lower 0.5-5 fluence of 5 10 2 10 5 -+ - erg cm −2 is obtained by extrapolating the 80-800 keV fluence observed by GRBAlpha, assuming the spectrum is observed during the first 4 s of the main GRB peak (Ripa et al 2023). (Oganesyan et al 2017(Oganesyan et al , 2018.…”

Section: Discussionmentioning

confidence: 98%

“…Considering only the dust models giving reasonable fits to the 19 complete rings detected by XMM-Newton, the powerlaw photon index spans from 1 to 1.4. The steepest spectrum (Γ GRB = 1.37 ± 0.04) is derived from the best-fitting model (BARE-GR-B), whereas a harder slope (Γ GRB ∼ 0.8, with significant variability during the GRB evolution) is observed at the lowest energies by hard X-ray detectors during the peak of the main event (An et al 2023;Frederiks et al 2023;Ripa et al 2023). Together with the larger GRB fluence derived from our analysis of the X-ray rings, this suggests the presence of a soft excess in the prompt emission of GRB 221009A.…”

Section: Discussionmentioning

confidence: 99%

The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo

Tiengo

Pintore

Beatrice

et al. 2023

ApJL

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GRB 221009A is the brightest gamma-ray burst (GRB) ever detected that has occurred at low Galactic latitude. Owing to this exceptional combination, its prompt X-ray emission could be detected for weeks in the form of expanding X-ray rings produced by scattering in Galactic dust clouds. We report on the analysis of 20 rings, generated by dust at distances ranging from 0.3 to 18.6 kpc, detected during two X‐ray Multi Mirror (XMM)-Newton observations performed about 2 and 5 days after the GRB. By fitting the spectra of the rings with different models for the dust composition and grain size distribution, we reconstructed the spectrum of the GRB prompt emission in the 0.7–4 keV energy range as an absorbed power law with photon index Γ = 1–1.4 and absorption in the host galaxy N H,z = (4.1–5.3) × 1021 cm−2. Taking into account the systematic uncertainties regarding the column density of dust contained in the clouds producing the rings, the 0.5–5 keV fluence of GRB 221009A can be constrained between 10−3 and 7 × 10−3 erg cm−2. Both the fluence and the photon index indicate the presence of a possible soft excess with respect to the extrapolation of the main GRB peak observed at higher energies.

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“…PICsIT's spectral-timing data's limited energy range makes direct comparisons with instruments that extend to lower energies difficult if there is spectral curvature, as is reported by GR-BAlpha (Ripa et al 2023), Konus-Wind (Frederiks et al 2023), and GECAM (An et al 2023). However, AGILE/MCAL found that the data from T 0 + 181.00 − 194.03 s are well fit by a power law of Γ = 2.07 ± 0.04 (Ursi et al 2022).…”

Section: Prompt Emissionmentioning

confidence: 99%

Soft gamma-ray spectral and time evolution of the GRB 221009A: Prompt and afterglow emission with INTEGRAL/IBIS-PICsIT

Rodi¹,

Ubertini²

2023

A&A

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Aims. The gamma-ray burst (GRB) 221009A, with its extreme brightness, has provided the opportunity to explore GRB prompt and afterglow emission behavior on short timescales with high statistics. In conjunction with detection up to very-high-energy gamma rays, studies of this event shed light on the emission processes at work in the initial phases of GRBs' emission. Methods. Using INTEGRAL/IBIS's soft gamma-ray detector, PICsIT (200−2600 keV), we studied the temporal and spectral evolution during the prompt phase and the early afterglow period. Results. We found a "flux-tracking" behavior with the source spectrum "softer" when brighter. However, the relationship between the spectral index and the flux changes during the burst. The PICsIT light curve shows that afterglow emission begins to dominate at ∼ T 0 + 630 s and decays with a slope of 1.6 ± 0.2, consistent with the slopes reported at soft X-rays.

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The peak-flux of GRB 221009A measured with GRBAlpha

Cited by 8 publications

References 0 publications

A structured jet explains the extreme GRB 221009A

A structured jet explains the extreme GRB 221009A

The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo

Soft gamma-ray spectral and time evolution of the GRB 221009A: Prompt and afterglow emission with INTEGRAL/IBIS-PICsIT

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