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The Peculiar Short-duration GRB 200826A and Its Supernova*

A. RossiINAF–Osservatorio di Astrofisica e Scienza dello Spazio, via Piero Gobetti 93/3, I-40129 Bologna, Italy; [email protected]Barry RothbergGeorge Mason University, Department of Physics & Astronomy, MS 3F3, 4400 University Dr., Fairfax, VA 22030, USAE. PalazziINAF–Osservatorio di Astrofisica e Scienza dello Spazio, via Piero Gobetti 93/3, I-40129 Bologna, Italy; [email protected]Д. А. КаннInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía, S/N, E-18008 Granada, SpainP. D’AvanzoINAF–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807, Merate (LC), ItalyL. AmatiINAF–Osservatorio di Astrofisica e Scienza dello Spazio, via Piero Gobetti 93/3, I-40129 Bologna, Italy; [email protected]S. KloseThüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, GermanyAlbino PeregoDipartimento di Fisica, Universitá di Trento, Via Sommarive 14, I-38123 Trento, ItalyE. PianINAF–Osservatorio di Astrofisica e Scienza dello Spazio, via Piero Gobetti 93/3, I-40129 Bologna, Italy; [email protected]C. GuidorziDepartment of Physics and Earth Science, University of Ferrara, via Saragat 1, I-44122, Ferrara, ItalyA. PozanenkoMoscow Institute of Physics and Technology (MIPT), 9 Institutskiy per., Dolgoprudny, Moscow Oblast 141701, RussiaS. SavaglioPhysics Department, University of Calabria, I-87036 Arcavacata di Rende, ItalyG. StrattaINAF–Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere 100, I-00133 Roma, ItalyGuido AgapitoINAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125-Firenze, ItalyS. CovinoINAF–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807, Merate (LC), ItalyF. CusanoINAF–Osservatorio di Astrofisica e Scienza dello Spazio, via Piero Gobetti 93/3, I-40129 Bologna, Italy; [email protected]V. D’EliaINAF–Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, ItalyM. de PasqualeDepartment of Astronomy and Space Sciences, Faculty of Science, Istanbul University, 34119 Istanbul, TurkeyM. Della ValleINAF, Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Naples, ItalyO. KuhnLarge Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721, USAL. IzzoDARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen, DenmarkEleonora LoffredoGran Sasso Science Institute, Viale F. Crispi 7, I-67100, L’Aquila (AQ), ItalyN. MasettiDepartamento de Ciencias Físicas, Universidad Andrés Bello, Fernández Concha 700, Las Condes, Santiago, ChileA. MelandriINAF–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807, Merate (LC), ItalyP. Yu. MinaevMoscow Institute of Physics and Technology (MIPT), 9 Institutskiy per., Dolgoprudny, Moscow Oblast 141701, RussiaA. Nicuesa GuelbenzuThüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, GermanyD. ParisINAF–Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, ItalyS. PaianoINAF–Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, via Alfonso Corti 12, I-20133 Milano, ItalyCédric PlantetINAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125-Firenze, ItalyFabio RossiINAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125-Firenze, ItalyR. SalvaterraINAF–Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, via Alfonso Corti 12, I-20133 Milano, ItalyS. SchulzeThe Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE 106 91 Stockholm, SwedenC. VeilletLarge Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721, USAA. VolnovaSpace Research Institute of the Russian Academy of Sciences (IKI), 84/32 Profsoyuznaya St., Moscow 117997, Russia

2022en

ABI

Annotatsiya

Abstract Gamma-ray bursts (GRBs) are classified into long and short events. Long GRBs (LGRBs) are associated with the end states of very massive stars, while short GRBs (SGRBs) are linked to the merger of compact objects. GRB 200826A was a peculiar event, because by definition it was an SGRB, with a rest-frame duration of ∼0.5 s. However, this event was energetic and soft, which is consistent with LGRBs. The relatively low redshift ( z = 0.7486) motivated a comprehensive, multiwavelength follow-up campaign to characterize its host, search for a possible associated supernova (SN), and thus understand the origin of this burst. To this aim we obtained a combination of deep near-infrared (NIR) and optical imaging together with spectroscopy. Our analysis reveals an optical and NIR bump in the light curve whose luminosity and evolution are in agreement with several SNe associated to LGRBs. Analysis of the prompt GRB shows that this event follows the E p,i – E iso relation found for LGRBs. The host galaxy is a low-mass star-forming galaxy, typical of LGRBs, but with one of the highest star formation rates, especially with respect to its mass ( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>8.6</mml:mn> </mml:math> , SFR ∼ 4.0 M ⊙ yr −1 ). We conclude that GRB 200826A is a typical collapsar event in the low tail of the duration distribution of LGRBs. These findings support theoretical predictions that events produced by collapsars can be as short as 0.5 s in the host frame and further confirm that duration alone is not an efficient discriminator for the progenitor class of a GRB.

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DOI: 10.3847/1538-4357/ac60a2

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