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

Shrestha, Manisha and Sand, David J. and Alexander, Kate D. and Bostroem, K. Azalee and Hosseinzadeh, Griffin and Pearson, Jeniveve and Aghakhanloo, Mojgan and Vinkó, József and Andrews, Jennifer E. and Jencson, Jacob E. and Lundquist, M. J. and Wyatt, Samuel and Howell, D. Andrew and McCully, Curtis and Gonzalez, Estefania Padilla and Pellegrino, Craig and Terreran, Giacomo and Hiramatsu, Daichi and Newsome, Megan and Farah, Joseph and Jha, Saurabh W. and Smith, Nathan and Wheeler, J. Craig and Martínez-Vázquez, Clara and Carballo-Bello, Julio A. and Drlica-Wagner, Alex and James, David J. and Mutlu-Pakdil, Burçin and Stringfellow, Guy S. and Sakowska, Joanna D. and Noël, Noelia E. D. and Bom, Clécio R. and Kuehn, Kyler (2023) Limit on Supernova Emission in the Brightest Gamma-Ray Burst, GRB 221009A. The Astrophysical Journal Letters, 946 (1). L25. ISSN 2041-8205

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Abstract

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 }\approx -$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.

Item Type: Article
Subjects: Bengali Archive > Medical Science
Depositing User: Unnamed user with email support@bengaliarchive.com
Date Deposited: 18 Apr 2023 07:24
Last Modified: 17 Jun 2024 07:16
URI: http://science.archiveopenbook.com/id/eprint/843

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