GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Канн, Д. А.; Agayeva, S.; Aivazyan, V.; Alishov, S.; C., Andrade,; Antier, S.; Baransky, A.; Bendjoya, P.; Benkhaldoun, Z.; Beradze, S.; Berezin, D.; Boër, M.; Broens, E.; Brunier, S; Bulla, Mattia; Бурхонов, О.; Burns, E.; Chen, Y; Chen, Y.; Conti, M.; Coughlin, M. W.; Cui, Wei; Daigne, F.; Delaveau, B; Devillepoix, Hadrien A. R.; Dietrich, Tim; Dornic, D.; Dubois, F.; Ducoin, Jean-Grégoire; Durand, Éric; Duverne, P.-A.; Eggenstein, H.-B.; Ehgamberdiev, S. A.; Fouad, Ahmed M.; Freeberg, M; Froebrich, D.; Ge, Ming-Yu; Gervasoni, S; Godunova, V.; Gokuldass, P.; Gurbanov, E. A.; Han, Danxiang; E., Hasanov,; Hello, P.; T., Hussenot-Desenonges,; Inasaridze, R.; Iskandar, Abdusamatjan; Исмаилов, Н. З.; A., Janati,; du, Laz, T. Jegou; Jia, Shihai; Karpov, S. V.; Kaeouach, A.; Kiendrebeogo, R.W; Klotz, A.; R., Kneip,; Kochiashvili, N.; Kunert, Nina; Lekic, A; Leonini, S; Li, Chi Kong; Li, W; Li, X. B.; Liao, J. Y.; Logie, Ludwig; Lu, F. J.; Mao, J.; D., Marchais,; Menard, R.; Morris, David C.; Natsvlishvili, R.; Nedora, Vsevolod; K., Noonan,; Noysena, K.; Orange, N. B.; Pang, P. T. H.; Peng, Hui-Sheng; Pellouin, Clément; Peloton, J.; Pradier, T.; Pyshna, O; Rajabov, Y.; Rau, Steve; Rinner, C.; Rivet, J.-P; Romanov, Filipp Dmitrievich; Rosi, P.; V., Rupchandani,; Serrau, M.; Shokry, Azza; Simon, A.; Smith, K.; Sokoliuk, O.; Soliman, M. A.; Song, Liming; Takey, A.; Tillayev, Yusufjon; Ramirez, L. M. Tinjaca; Melo, I. Tosta e; Turpin, D.; Postigo, A. de Ugarte; Vanaverbeke, Sigfried; Vasylenko, V.; Vernet, D.; Vidadi, Z.; Wang, Chunling; Wang, J; Wang, L.; Wang, X.-F.; Xiong, S. L.; Xu, YP; Xue, Weicheng; Zeng, Xiaopeng; Zhang, S.; Zhao, H. S.; Zhao, Xiao-Hong

doi:10.3847/2041-8213/acc8d0

Cited by 24 publications

(19 citation statements)

References 122 publications

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“…We use their measurements of F625W = 24.88 ± 0.08 mag and F775W = 23.80 ± 0.14 mag, which approximately correspond to the r′ and i′ bands. Previous analyses (Fulton et al 2023;Kann et al 2023;Shrestha et al 2023) did not incorporate the host contribution explicitly in their analysis (though Pan-STARRS and DECam photometry in Fulton et al 2023, andDECam photometry in Shrestha et al 2023 are subjected to template subtraction, which negates the host contribution to a degree).…”

Section: Previous Broadband Modeling Resultsmentioning

confidence: 99%

“…This is likely why they were able to find significant evidence of excess emission, while our preference for the SN model is moderate. Shrestha et al (2023) and Levan et al (2023) report no evidence for bright SN emission, while Kann et al (2023) does not find any strong evidence for or against SN emission. None of them rule out the possibility of a faint associated SN, and one of the conclusions of Levan et al (2023) is that an associated SN to GRB 221009A must be either substantially (∼10%-40%) fainter or bluer than SN 1998bw.…”

Section: Model Selectionmentioning

confidence: 92%

“…Assuming the optical afterglow is powered by synchrotron emission from the forward shock (Mészáros & Rees 1997), we fit the early-time light curve with power-law models ( f ν ∝ t − α ) to attempt to isolate the contribution from the SN. Prior to T 0 + 1 day, the optical data display a shallow initial slope with α = 0.88 ± 0.05 (Kann et al 2023;O'Connor et al 2023). Beyond this time there is a clear steepening in the decay, and a single power law does not provide a good fit to all optical data (D' Avanzo et al 2022).…”

Section: Optical Afterglow Modelingmentioning

confidence: 99%

“…The unprecedented brightness led to extensive follow up across the electromagnetic spectrum (e.g., Fulton et al 2023;Laskar et al 2023;Kann et al 2023;O'Connor et al 2023;Williams et al 2023). Spectroscopy of the optical afterglow led to a redshift measurement of z = 0.151 (de Ugarte Postigo et al 2022a;Castro-Tirado et al 2022;Malesani et al 2023).…”

Section: Introductionmentioning

confidence: 99%

“…In Section 2 we report the observations of the optical afterglow of GRB 221009A; in Section 3 we analyze the observations, and statistically compare models with and without a SN component; in Section 4 we constrain the physical parameters of SN 2022xiw; in Section 5 we place GRB 221009A/SN 2022xiw in the context of the GRB-SN sample in the literature; and in Section 6 we summarize our conclusions. In the final stages of manuscript preparation, studies reporting conflicting results on the existence of SN emission were posted on the arXiv (Fulton et al 2023;Kann et al 2023;Levan et al 2023;Shrestha et al 2023)-where relevant we highlight differences in our approach and contrasts in our results.…”

Section: Introductionmentioning

confidence: 99%

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A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

Srinivasaragavan

O’Connor

Cenko

et al. 2023

ApJL

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We report observations of the optical counterpart of the long gamma-ray burst GRB 221009A. Due to the extreme rarity of being both nearby (z = 0.151) and highly energetic (E γ,iso ≥ 1054 erg), GRB 221009A offers a unique opportunity to probe the connection between massive star core collapse and relativistic jet formation across a very broad range of γ-ray properties. Adopting a phenomenological power-law model for the afterglow and host galaxy estimates from high-resolution Hubble Space Telescope imaging, we use Bayesian model comparison techniques to determine the likelihood of an associated supernova (SN) contributing excess flux to the optical light curve. Though not conclusive, we find moderate evidence (K Bayes = 101.2) for the presence of an additional component arising from an associated SN, SN 2022xiw, and find that it must be substantially fainter (<67% as bright at the 99% confidence interval) than SN 1998bw. Given the large and uncertain line-of-sight extinction, we attempt to constrain the SN parameters (M Ni, M ej, and E KE) under several different assumptions with respect to the host galaxy’s extinction. We find properties that are broadly consistent with previous GRB-associated SNe: M Ni = 0.05–0.25 M ⊙, M ej = 3.5–11.1 M ⊙, and E KE = (1.6–5.2) × 1052 erg. We note that these properties are weakly constrained due to the faintness of the SN with respect to the afterglow and host emission, but we do find a robust upper limit on M Ni of M Ni < 0.36 M ⊙. Given the tremendous range in isotropic gamma-ray energy release exhibited by GRBs (seven orders of magnitude), the SN emission appears to be decoupled from the central engine in these systems.

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Section: Previous Broadband Modeling Resultsmentioning

confidence: 99%

Section: Model Selectionmentioning

confidence: 92%

Section: Optical Afterglow Modelingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

Srinivasaragavan

O’Connor

Cenko

et al. 2023

ApJL

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The BOAT GRB 221009A: A Poynting-flux-dominated narrow jet surrounded by a matter-dominated structured jet wing

Zhang,

Wang,

Zheng

2024

Journal of High Energy Astrophysics

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JWST detection of a supernova associated with GRB 221009A without an r-process signature

Blanchard,

Villar,

Chornock

et al. 2024

Nat Astron

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Identifying the sites of r-process nucleosynthesis, a primary mechanism of heavy element production, is a key goal of astrophysics. The discovery of the brightest gamma-ray burst (GRB) to date, GRB 221009A, presented an opportunity to spectroscopically test the idea that r-process elements are produced following the collapse of rapidly rotating massive stars. Here we present James Webb Space Telescope observations of GRB 221009A obtained +168 and +170 rest-frame days after the gamma-ray trigger, and demonstrate that they are well described by a SN 1998bw-like supernova (SN) and power-law afterglow, with no evidence for a component from r-process emission. The SN, with a nickel mass of approximately 0.09 M⊙, is only slightly fainter than the brightness of SN 1998bw at this phase, which indicates that the SN is not an unusual GRB-SN. This demonstrates that the GRB and SN mechanisms are decoupled and that highly energetic GRBs are not likely to produce significant quantities of r-process material, which leaves open the question of whether explosions of massive stars are key sources of r-process elements. Moreover, the host galaxy of GRB 221009A has a very low metallicity of approximately 0.12 Z⊙ and strong H2 emission at the explosion site, which is consistent with recent star formation, hinting that environmental factors are responsible for its extreme energetics.

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GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Cited by 24 publications

References 122 publications

A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

The BOAT GRB 221009A: A Poynting-flux-dominated narrow jet surrounded by a matter-dominated structured jet wing

JWST detection of a supernova associated with GRB 221009A without an r-process signature

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