Тип публикации: статья из журнала

Год издания: 2023

Идентификатор DOI: 10.1093/mnras/stac3629

Аннотация: <jats:title>ABSTRACT</jats:title> <jats:p>We report on detailed multiwavelength observations and analysis of the very bright and long GRB 210619B, detected by the Atmosphere-Space Interactions Monitor installed on the International Space Station and the Gamma-ray Burst Monitor (GBM) on-board the Fermi mission. Our main goal is to uПоказать полностьюnderstand the radiation mechanisms and jet composition of GRB 210619B. With a measured redshift of z = 1.937, we find that GRB 210619B falls within the 10 most luminous bursts observed by Fermi so far. The energy-resolved prompt emission light curve of GRB 210619B exhibits an extremely bright hard emission pulse followed by softer/longer emission pulses. The low-energy photon index (αpt) values obtained using the time-resolved spectral analysis of the burst suggest a transition between the thermal (during harder pulse) to non-thermal (during softer pulse) outflow. We examine the correlation between spectral parameters and find that both peak energy and αpt exhibit the flux tracking pattern. The late time broad-band photometric data set can be explained within the framework of the external forward shock model with νm < νc < νx (where νm, νc, and νx are the synchrotron peak, cooling-break, and X-ray frequencies, respectively) spectral regime supporting a rarely observed hard electron energy index (p < 2). We find moderate values of host extinction of E(B − V) = 0.14 ± 0.01 mag for the small magellanic cloud extinction law. In addition, we also report late-time optical observations with the 10.4 m Gran Telescopio de Canarias placing deep upper limits for the host galaxy (z = 1.937), favouring a faint, dwarf host for the burst.</jats:p>

Журнал: Monthly Notices of the Royal Astronomical Society

Выпуск журнала: Т. 519, № 3

Номера страниц: 3201-3226

ISSN журнала: 00358711

Издатель: John Wiley &amp; Sons, Incorporated

• Caballero-García M.D. (Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada)
• Gupta Rahul (Department of Physics, Deen Dayal Upadhyaya Gorakhpur University, Gorakhpur-273009, India)
• Pandey S.B. (Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital-263002, India)
• Oates S.R. (School of Physics and Astronomy &amp; Institute for Gravitational Wave Astronomy, University of Birmingham, Birmingham B15 2TT, UK)
• Marisaldi M (National Institute for Astrophysics, Osservatorio di Astrofisica e Scienzia dello Spazio, 40129 Bologna, Italy)
• Ramsli A (Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, N-5020 Bergen, Norway)
• Hu Y-D (Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada)
• Castro-Tirado A.J. (Unidad Asociada al CSIC, Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías, Universidad de Málaga, 29071 Málaga, Spain)
• Sánchez-Ramírez R (Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada)
• Connell P.H. (Image Processing Laboratory, University of Valencia, 46980 Paterna, Valencia, Spain)
• Christiansen F (National Space Institute, Technical University of Denmark, DK-2800 Kgs. Lyngby, Denmark)
• Ror A Kumar (Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital-263002, India)
• Aryan A (Department of Physics, Deen Dayal Upadhyaya Gorakhpur University, Gorakhpur-273009, India)
• Bai J-M (Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China)
• Castro-Tirado M.A. (Unidad Asociada al CSIC, Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías, Universidad de Málaga, 29071 Málaga, Spain)
• Fan Y-F (Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China)
• Fernández-García E (Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada)
• Kumar A (School of Studies in Physics and Astrophysics, Pandit Ravishankar Shukla University, Raipur, Chattisgarh-492010, India)
• Lindanger A (Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, N-5020 Bergen, Norway)
• Mezentsev A (Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, N-5020 Bergen, Norway)
• Navarro-González J (Image Processing Laboratory, University of Valencia, 46980 Paterna, Valencia, Spain)
• Neubert T (National Space Institute, Technical University of Denmark, DK-2800 Kgs. Lyngby, Denmark)
• Østgaard N (Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, N-5020 Bergen, Norway)
• Pérez-García I (Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada)
• Reglero V (Image Processing Laboratory, University of Valencia, 46980 Paterna, Valencia, Spain)
• Sarria D (Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, N-5020 Bergen, Norway)
• Sun T.R. (Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada)
• Xiong D-R (Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China)
• Yang J (School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China)
• Yang Y-H (School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China)
• Zhang B-B (Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China)

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