Light scalar explanation for 18 TeV GRB 221009A

Balaji, Shyam; Ramirez-Quezada, Maura E.; Silk, Joseph; Zhang, Yongchao

doi:10.48550/arxiv.2301.02258

Cited by 2 publications

(2 citation statements)

References 63 publications

(86 reference statements)

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“…The detection of very energetic photons in the TeV range such as in the case of GRB 190114C (MAGIC Collaboration et al 2019) and now GRB 221009A, challenges our understanding of GRB physics. There is no firm consensus on the production mechanisms of these very high-energy photons in the range of GeV to TeV (see further discussions in Balaji et al 2023;Mirabal 2023). Atteia (2022) have predicted that the next event like GRB 221009A has a 10% probability of being observed in the next 50 yr.…”

Section: Introductionmentioning

confidence: 99%

Limit on Supernova Emission in the Brightest Gamma-Ray Burst, GRB 221009A

Shrestha

Sand

Alexander

et al. 2023

ApJL

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We present photometric and spectroscopic observations of the extraordinary gamma-ray burst (GRB) 221009A in search of an associated supernova. Some past GRBs have shown bumps in the optical light curve that coincide with the emergence of supernova spectral features, but we do not detect any significant light-curve features in GRB 221009A, nor do we detect any clear sign of supernova spectral features. Using two well-studied GRB-associated supernovae (SN 2013dx, M r , max = − 19.54 ; SN 2016jca, M r , max = − 19.04 ) at a similar redshift as GRB 221009A (z = 0.151), we modeled how the emergence of a supernova would affect the light curve. If we assume the GRB afterglow to decay at the same rate as the X-ray data, the combination of afterglow and a supernova component is fainter than the observed GRB brightness. For the case where we assume the best-fit power law to the optical data as the GRB afterglow component, a supernova contribution should have created a clear bump in the light curve, assuming only extinction from the Milky Way. If we assume a higher extinction of E(B − V) = 1.74 mag (as has been suggested elsewhere), the supernova contribution would have been hard to detect, with a limit on the associated supernova of M r , max ≈ − 19.54. We do not observe any clear supernova features in our spectra, which were taken around the time of expected maximum light. The lack of a bright supernova associated with GRB 221009A may indicate that the energy from the explosion is mostly concentrated in the jet, leaving a lower energy budget available for the supernova.

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Section: Introductionmentioning

confidence: 99%