A Reverse Shock in GRB 181201A

Tanmoy Laskar, Hendrik Jan van Eerten, Patricia Schady, C. G. Mundell, Kate D. Alexander, Rodolfo Barniol Duran, Edo Berger, J. Bolmer, Ryan Chornock, Deanne L. Coppejans, Wen Fai Fong, Andreja Gomboc, Núria Jordana-Mitjans, Shiho Kobayashi, Raffaella Margutti, Karl M. Menten, Re'Em Sari, Ryo Yamazaki, V. M. Lipunov, E. GorbovskoyV. G. Kornilov, N. Tyurina, D. Zimnukhov, R. Podesta, H. Levato, D. A.H. Buckley, A. Tlatov, R. Rebolo, M. Serra-Ricart

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Abstract

We present comprehensive multiwavelength radio to X-ray observations of GRB 181201A spanning from ≈150 s to ≈163 days after the burst, comprising the first joint ALMA-VLA-GMRT observations of a gamma-ray burst (GRB) afterglow. The radio and millimeter-band data reveal a distinct signature at ≈3.9 days, which we interpret as reverse-shock (RS) emission. Our observations present the first time that a single radio-frequency spectral energy distribution can be decomposed directly into RS and forward shock (FS) components. We perform detailed modeling of the full multiwavelength data set, using Markov Chain Monte Carlo sampling to construct the joint posterior density function of the underlying physical parameters describing the RS and FS synchrotron emission. We uncover and account for all discovered degeneracies in the model parameters. The joint RS-FS modeling reveals a weakly magnetized (σ ≈ 3 × 10-3), mildly relativistic RS, from which we derive an initial bulk Lorentz factor of Γ0 ≈ 103 for the GRB jet. Our results support the hypothesis that low-density environments are conducive to the observability of RS emission. We compare our observations to other events with strong RS detections and find a likely observational bias selecting for longer lasting, nonrelativistic RSs. We present and begin to address new challenges in modeling posed by the present generation of comprehensive, multifrequency data sets.

Original languageEnglish
Article number121
JournalAstrophysical Journal
Volume884
Issue number2
DOIs
Publication statusPublished - 17 Oct 2019

Funding

Tanmoy Laskar Hendrik van Eerten Patricia Schady C. G. Mundell Kate D. Alexander Rodolfo Barniol Duran Edo Berger J. Bolmer Ryan Chornock Deanne L. Coppejans Wen-fai Fong Andreja Gomboc N�ria Jordana-Mitjans Shiho Kobayashi Raffaella Margutti Karl M. Menten Re’em Sari Ryo Yamazaki V. M. Lipunov E. Gorbovskoy V. G. Kornilov N. Tyurina D. Zimnukhov R. Podesta H. Levato D. A. H. Buckley A. Tlatov R. Rebolo M. Serra-Ricart Tanmoy Laskar Hendrik van Eerten Patricia Schady C. G. Mundell Kate D. Alexander Rodolfo Barniol Duran Edo Berger J. Bolmer Ryan Chornock Deanne L. Coppejans Wen-fai Fong Andreja Gomboc N�ria Jordana-Mitjans Shiho Kobayashi Raffaella Margutti Karl M. Menten Re’em Sari Ryo Yamazaki V. M. Lipunov E. Gorbovskoy V. G. Kornilov N. Tyurina D. Zimnukhov R. Podesta H. Levato D. A. H. Buckley A. Tlatov R. Rebolo M. Serra-Ricart Department of Physics, University of Bath, Claverton Down, Bath, BA2 7AY, UK Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA Department of Physics and Astronomy, California State University, Sacramento, 6000 J Street, Sacramento, CA 95819, USA Department of Astronomy, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA Max-Planck-Institut f�r extraterrestrische Physik, Giessenbachstra�e, D-85748 Garching, Germany Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USA Center for Astrophysics and Cosmology, University of Nova Gorica, Vipavska 13, 5000 Nova Gorica, Slovenia Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK Max-Planck-Institut f�r Radioastronomie, Auf dem H�gel 69, D-53121 Bonn, Germany Racah Institute of Physics, The Hebrew University, Jerusalem 91904, Israel Department of Physics and Mathematics, Aoyama-Gakuin University, Kanagawa 252-5258, Japan M. V. Lomonosov Moscow State University, Physics Department, Leninskie gory, GSP-1, Moscow, 119991, Russia M. V. Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr., 13, Moscow, 119234, Russia Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan, San Juan, Argentina Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE), San Juan, Argentina South African Astronomical Observatory, P.O. Box 9, 7935 Observatory, Cape Town, South Africa Kislovodsk Solar Station of the Main (Pulkovo) Observatory, RAS, P.O. Box 45, ul. Gagarina 100, Kislovodsk, 357700, Russia Instituto de Astrof�sica de Canarias (IAC), Calle V�a L�ctea s/n, E-38200 La Laguna, Tenerife, Spain NHFP Einstein Fellow. Tanmoy Laskar, Hendrik van Eerten, Patricia Schady, C. G. Mundell, Kate D. Alexander, Rodolfo Barniol Duran, Edo Berger, J. Bolmer, Ryan Chornock, Deanne L. Coppejans, Wen-fai Fong, Andreja Gomboc, N�ria Jordana-Mitjans, Shiho Kobayashi, Raffaella Margutti, Karl M. Menten, Re’em Sari, Ryo Yamazaki, V. M. Lipunov, E. Gorbovskoy, V. G. Kornilov, N. Tyurina, D. Zimnukhov, R. Podesta, H. Levato, D. A. H. Buckley, A. Tlatov, R. Rebolo and M. Serra-Ricart 2019-10-20 2019-10-17 15:22:37 cgi/release: Article released bin/incoming: New from .zip NASA HST-HF2-51403.001 National Science Foundation AST-1714498 NASA NNX15AE50G National Science Foundation PHY-1748958 National Science Foundation 1816694 Slovenian Research Agency P1-0031 Slovenian Research Agency I0-0033 Slovenian Research Agency J1-8136 Russian Foundation for Basic Research 17-52-8013 yes We present comprehensive multiwavelength radio to X-ray observations of GRB�181201A spanning from ≈150 s to ≈163 days after the burst, comprising the first joint ALMA–VLA–GMRT observations of a gamma-ray burst (GRB) afterglow. The radio and millimeter-band data reveal a distinct signature at ≈3.9 days, which we interpret as reverse-shock (RS) emission. Our observations present the first time that a single radio-frequency spectral energy distribution can be decomposed directly into RS and forward shock (FS) components. We perform detailed modeling of the full multiwavelength data set, using Markov Chain Monte Carlo sampling to construct the joint posterior density function of the underlying physical parameters describing the RS and FS synchrotron emission. We uncover and account for all discovered degeneracies in the model parameters. The joint RS–FS modeling reveals a weakly magnetized ( σ �≈�3 � 10 −3 ), mildly relativistic RS, from which we derive an initial bulk Lorentz factor of Γ 0 �≈�103 for the GRB jet. Our results support the hypothesis that low-density environments are conducive to the observability of RS emission. 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ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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