Статья

The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

M. FultonAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]Stephen SmarttAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]Lauren RhodesDepartment of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UKM. E. HuberInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAV. Ashley VillarDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USAT. MooreAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]Shubham SrivastavAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]A. S. B. SchultzInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAK. C. ChambersInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAL. IzzoDARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen, DenmarkJ. HjorthDARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen, DenmarkT. W. ChenMax-Planck-Institut für Astrophysik, Karl-Schwarzschild Straße 1, D-85748 Garching, GermanyM. NichollBirmingham Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UKR. J. FoleyDepartment of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95060, USAA. RestDepartment of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USAK. SmithAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]D. R. YoungAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]Stuart SimAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]Joe BrightDepartment of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UKYossef ZenatiDepartment of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USAThomas de BoerInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAJ. BulgerInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAJ. FairlambInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAHua GaoInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAChien-Cheng LinInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAT. LoweInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAE. A. MagnierInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAI. A. SmithInstitute for Astronomy, University of Hawai’i, 34 Ohia Ku St., Pukalani, HI 96768-8288, USAR. J. WainscoatInstitute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAD. A. CoulterDepartment of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95060, USAD. O. JonesGemini Observatory, NSF’s NOIRLab, 670 N. A’ohoku Place, Hilo, Hawai’i, 96720, USAC. D. KilpatrickCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, 1800 Sherman Ave, Evanston, IL 60201, USAPeter McGillDepartment of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95060, USAE. Ramírez-RuizDepartment of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95060, USAKyoung-Soo LeeDepartment of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, Indiana 47907, USAGautham NarayanCenter for Astrophysical Surveys, National Center for Supercomputing Applications, Urbana, IL 61801, USAVandana RamakrishnanDepartment of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, Indiana 47907, USARyan Ridden-HarperSchool of Physical and Chemical Sciences—Te Kura Matū, University of Canterbury, Private Bag 4800, Christchurch 8140, New ZealandAkriti SinghDepartamento de Ciencias Fisicas, Facultad de Ciencias Exactas, Universidad Andres Bello, Fernandez Concha 700, Las Condes, Santiago, ChileQinan WangDepartment of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USAA. K. H. KongInstitute of Astronomy, National Tsing Hua University, Hsinchu 30013, TaiwanChow‐Choong NgeowGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, 32001 Jhongli, TaiwanY. C. PanGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, 32001 Jhongli, TaiwanS. YangDepartment of Astronomy, The Oskar Klein Center, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenKyle W. DavisDepartment of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95060, USAAnthony L. PiroThe Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USAC. Rojas-BravoDepartment of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95060, USAJulian S. SommerAstrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK; [email protected]S. K. YadavalliDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA

2023en

ABI

Аннотация

Abstract We present extensive optical photometry of the afterglow of GRB 221009A. Our data cover 0.9–59.9 days from the time of Swift and Fermi gamma-ray burst (GRB) detections. Photometry in rizy -band filters was collected primarily with Pan-STARRS and supplemented by multiple 1–4 m imaging facilities. We analyzed the Swift X-ray data of the afterglow and found a single decline rate power law f ( t ) ∝ t −1.556±0.002 best describes the light curve. In addition to the high foreground Milky Way dust extinction along this line of sight, the data favor additional extinction to consistently model the optical to X-ray flux with optically thin synchrotron emission. We fit the X-ray-derived power law to the optical light curve and find good agreement with the measured data up to 5−6 days. Thereafter we find a flux excess in the riy bands that peaks in the observer frame at ∼20 days. This excess shares similar light-curve profiles to the Type Ic broad-lined supernovae SN 2016jca and SN 2017iuk once corrected for the GRB redshift of z = 0.151 and arbitrarily scaled. This may be representative of an SN emerging from the declining afterglow. We measure rest-frame absolute peak AB magnitudes of M g = −19.8 ± 0.6 and M r = − 19.4 ± 0.3 and M z = −20.1 ± 0.3. If this is an SN component, then Bayesian modeling of the excess flux would imply explosion parameters 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>ej</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>7.1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.7</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>2.4</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> M ⊙ , <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>Ni</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.6</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> M ⊙ , and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>v</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>ej</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi mathvariant="normal">33,900</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>5700</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>5900</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> km s −1 , for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of E kin ≃ 2.6–9.0 × 10 52 erg.

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Идентификаторы

DOI: 10.3847/2041-8213/acc101

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Цитирований: 2Использованных источников: 0

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