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

Manisha ShresthaSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]David SandSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]K. D. AlexanderSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]O. FoxSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]Griffin HosseinzadehSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]Jeniveve PearsonSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]Mojgan AghakhanlooSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]Jozsef VinkoDepartment of Experimental Physics, University of Szeged, Dóm tér 9, Szeged, 6720, HungaryJennifer E. AndrewsGemini Observatory, 670 North A‘ohoku Place, Hilo, HI 96720-2700, USAJ. E. JencsonDepartment of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USAM. LundquistW.M. Keck Observatory, 65-1120 Māmalahoa Highway, Kamuela, HI 96743-8431, USAS. WyattDepartment of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195-0002, USAD. A. HowellDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USACurtis McCullyDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAEstefania Padilla GonzalezDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAC. PellegrinoDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAG. TerreranDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USADaichi HiramatsuCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USAMegan NewsomeDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAJoseph FarahDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USASaurabh W. JhaDepartment of Physics and Astronomy, Rutgers, the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, USANathan SmithSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; [email protected]J. Craig WheelerUniversity of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259, USAC. E. Martínez-VázquezGemini Observatory, 670 North A‘ohoku Place, Hilo, HI 96720-2700, USAJ. A. Carballo-BelloInstituto de Alta Investigación, Sede Esmeralda, Universidad de Tarapacá, Av. Luis Emilio Recabarren 2477, Iquique, ChileA. Drlica-WagnerDepartment of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USAD. J. JamesASTRAVEO LLC, P.O. Box 1668, MA 01931, USABurçı̇n Mutlu-Pakdı̇lDepartment of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USAGuy S. StringfellowCenter for Astrophysics and Space Astronomy, University of Colorado Boulder, UCB 389, Boulder, CO 80309-0389 USAJ. D. SakowskaDepartment of Physics, University of Surrey, Guildford GU2 7XH, UKNoelia E. D. NoëlDepartment of Physics, University of Surrey, Guildford GU2 7XH, UKClécio R. BomCentro Brasileiro de Pesquisas Físicas, Rua Dr. Xavier Sigaud 150, 22290-180 Rio de Janeiro, RJ, BrazilK. KuehnAustralian Astronomical Optics, Macquarie University, North Ryde, NSW 2113, Australia

2023en

ABI

Annotatsiya

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, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>r</mml:mi> <mml:mo>,</mml:mo> <mml:mi>max</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>19.54</mml:mn> <mml:mo>;</mml:mo> </mml:math> SN 2016jca, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>r</mml:mi> <mml:mo>,</mml:mo> <mml:mi>max</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>19.04</mml:mn> </mml:math> ) 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>r</mml:mi> <mml:mo>,</mml:mo> <mml:mi>max</mml:mi> </mml:mrow> </mml:msub> <mml:mo>≈</mml:mo> <mml:mo>−</mml:mo> </mml:math> 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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DOI: 10.3847/2041-8213/acbd50

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