Radio data challenge the broadband modelling of GRB 160131A afterglow

M. Marongiu; C. Guidorzi; G. Stratta; A. Gomboc; N. Jordana-Mitjans; S. Dichiara; S. Kobayashi; D. Kopač; C. G. Mundell

doi:10.1051/0004-6361/202140403

Radio data challenge the broadband modelling of GRB 160131A afterglow

M. Marongiu, C. Guidorzi, G. Stratta, A. Gomboc, N. Jordana-Mitjans, S. Dichiara, S. Kobayashi, D. Kopač, C. G. Mundell

Department of Physics

Research output: Contribution to journal › Article › peer-review

7 Citations (SciVal)

Abstract

Context. Gamma-ray burst (GRB) afterglows originate from the interaction between the relativistic ejecta and the surrounding medium. Consequently, their properties depend on several aspects: radiation mechanisms, relativistic shock micro-physics, circumburst environment, and the structure and geometry of the relativistic jet. While the standard afterglow model accounts for the overall spectral and temporal evolution for a number of GRBs, its validity limits emerge when the data set is particularly rich and constraining, especially in the radio band. Aims. We aimed to model the afterglow of the long GRB 160131A (redshift z = 0.972), for which we collected a rich, broadband, and accurate data set, spanning from 6 × 108 Hz to 7 × 1017 Hz in frequency, and from 330 s to 160 days post-burst in time. Methods. We modelled the spectral and temporal evolution of this GRB afterglow through two approaches: (1) the adoption of empirical functions to model an optical/X-ray data set, later assessing their compatibility with the radio domain; and (2) the inclusion of the entire multi-frequency data set simultaneously through the Python package named SAGA (Software for AfterGlow Analysis), to obtain an exhaustive and self-consistent description of the micro-physics, geometry, and dynamics of the afterglow. Results. From deep broadband analysis (from radio to X-ray frequencies) of the afterglow light curves, GRB 160131A outflow shows evidence of jetted emission. Moreover, we observe dust extinction in the optical spectra, and energy injection in the optical/X-ray data. Finally, radio spectra are characterised by several peaks that could be due to either interstellar scintillation (ISS) effects or a multi-component structure. Conclusions. The inclusion of radio data in the broadband set of GRB 160131A makes a self-consistent modelling barely attainable within the standard model of GRB afterglows.

Original language	English
Article number	A11
Number of pages	32
Journal	Astronomy and Astrophysics
Volume	658
Early online date	27 Jan 2022
DOIs	https://doi.org/10.1051/0004-6361/202140403
Publication status	Published - 1 Feb 2022

Bibliographical note

Funding Information:
Acknowledgements. We thank the anonymous referee for helping us improve the paper. Support for this work was provided by Università degli Studi di Ferrara through grant FIR 2018 “A Broad-band study of Cosmic Gamma-Ray Burst Prompt and Afterglow Emission” (PI Guidorzi). M. Marongiu acknowledges financial support from the Italian Ministry of University and Research – Project Proposal CIR01_00010, and the University of Ferrara for the financial support of his PhD scholarship (during the data analysis and the interpretation of the results). M. Marongiu is very grateful to R. Martone for useful conversations about GRB science; moreover, M. Marongiu thanks P. Bergamini and G. Angora for the useful discussion about Python programming language and data analysis. A. Gomboc acknowledges the financial support from the Slovenian Research Agency (grants P1-0031, I0-0033, J1-8136, J1-2460) and networking support by the COST Actions CA16104 GWverse and CA16214 PHAROS. N. Jordana and C.G. Mundell acknowledge financial support from Mr Jim Sherwin and Mrs Hiroko Sherwin. D. Kopac acknowledges the financial support from the Slovenian Research Agency (research core funding No. P1-0188). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc..

Funding

Acknowledgements. We thank the anonymous referee for helping us improve the paper. Support for this work was provided by Università degli Studi di Ferrara through grant FIR 2018 “A Broad-band study of Cosmic Gamma-Ray Burst Prompt and Afterglow Emission” (PI Guidorzi). M. Marongiu acknowledges financial support from the Italian Ministry of University and Research – Project Proposal CIR01_00010, and the University of Ferrara for the financial support of his PhD scholarship (during the data analysis and the interpretation of the results). M. Marongiu is very grateful to R. Martone for useful conversations about GRB science; moreover, M. Marongiu thanks P. Bergamini and G. Angora for the useful discussion about Python programming language and data analysis. A. Gomboc acknowledges the financial support from the Slovenian Research Agency (grants P1-0031, I0-0033, J1-8136, J1-2460) and networking support by the COST Actions CA16104 GWverse and CA16214 PHAROS. N. Jordana and C.G. Mundell acknowledge financial support from Mr Jim Sherwin and Mrs Hiroko Sherwin. D. Kopac acknowledges the financial support from the Slovenian Research Agency (research core funding No. P1-0188). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc..

Keywords

Gamma-ray burst: individual: GRB160131A Methods: data analysis
Radiation mechanisms: non-thermal

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/202140403

Cite this

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title = "Radio data challenge the broadband modelling of GRB 160131A afterglow",

abstract = "Context. Gamma-ray burst (GRB) afterglows originate from the interaction between the relativistic ejecta and the surrounding medium. Consequently, their properties depend on several aspects: radiation mechanisms, relativistic shock micro-physics, circumburst environment, and the structure and geometry of the relativistic jet. While the standard afterglow model accounts for the overall spectral and temporal evolution for a number of GRBs, its validity limits emerge when the data set is particularly rich and constraining, especially in the radio band. Aims. We aimed to model the afterglow of the long GRB 160131A (redshift z = 0.972), for which we collected a rich, broadband, and accurate data set, spanning from 6 × 108 Hz to 7 × 1017 Hz in frequency, and from 330 s to 160 days post-burst in time. Methods. We modelled the spectral and temporal evolution of this GRB afterglow through two approaches: (1) the adoption of empirical functions to model an optical/X-ray data set, later assessing their compatibility with the radio domain; and (2) the inclusion of the entire multi-frequency data set simultaneously through the Python package named SAGA (Software for AfterGlow Analysis), to obtain an exhaustive and self-consistent description of the micro-physics, geometry, and dynamics of the afterglow. Results. From deep broadband analysis (from radio to X-ray frequencies) of the afterglow light curves, GRB 160131A outflow shows evidence of jetted emission. Moreover, we observe dust extinction in the optical spectra, and energy injection in the optical/X-ray data. Finally, radio spectra are characterised by several peaks that could be due to either interstellar scintillation (ISS) effects or a multi-component structure. Conclusions. The inclusion of radio data in the broadband set of GRB 160131A makes a self-consistent modelling barely attainable within the standard model of GRB afterglows. ",

keywords = "Gamma-ray burst: individual: GRB160131A Methods: data analysis, Radiation mechanisms: non-thermal",

author = "M. Marongiu and C. Guidorzi and G. Stratta and A. Gomboc and N. Jordana-Mitjans and S. Dichiara and S. Kobayashi and D. Kopa{\v c} and Mundell, {C. G.}",

note = "Funding Information: Acknowledgements. We thank the anonymous referee for helping us improve the paper. Support for this work was provided by Universit{\`a} degli Studi di Ferrara through grant FIR 2018 “A Broad-band study of Cosmic Gamma-Ray Burst Prompt and Afterglow Emission” (PI Guidorzi). M. Marongiu acknowledges financial support from the Italian Ministry of University and Research – Project Proposal CIR01_00010, and the University of Ferrara for the financial support of his PhD scholarship (during the data analysis and the interpretation of the results). M. Marongiu is very grateful to R. Martone for useful conversations about GRB science; moreover, M. Marongiu thanks P. Bergamini and G. Angora for the useful discussion about Python programming language and data analysis. A. Gomboc acknowledges the financial support from the Slovenian Research Agency (grants P1-0031, I0-0033, J1-8136, J1-2460) and networking support by the COST Actions CA16104 GWverse and CA16214 PHAROS. N. Jordana and C.G. Mundell acknowledge financial support from Mr Jim Sherwin and Mrs Hiroko Sherwin. D. Kopac acknowledges the financial support from the Slovenian Research Agency (research core funding No. P1-0188). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.. ",

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doi = "10.1051/0004-6361/202140403",

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T1 - Radio data challenge the broadband modelling of GRB 160131A afterglow

AU - Marongiu, M.

AU - Guidorzi, C.

AU - Stratta, G.

AU - Gomboc, A.

AU - Jordana-Mitjans, N.

AU - Dichiara, S.

AU - Kobayashi, S.

AU - Kopač, D.

AU - Mundell, C. G.

N1 - Funding Information: Acknowledgements. We thank the anonymous referee for helping us improve the paper. Support for this work was provided by Università degli Studi di Ferrara through grant FIR 2018 “A Broad-band study of Cosmic Gamma-Ray Burst Prompt and Afterglow Emission” (PI Guidorzi). M. Marongiu acknowledges financial support from the Italian Ministry of University and Research – Project Proposal CIR01_00010, and the University of Ferrara for the financial support of his PhD scholarship (during the data analysis and the interpretation of the results). M. Marongiu is very grateful to R. Martone for useful conversations about GRB science; moreover, M. Marongiu thanks P. Bergamini and G. Angora for the useful discussion about Python programming language and data analysis. A. Gomboc acknowledges the financial support from the Slovenian Research Agency (grants P1-0031, I0-0033, J1-8136, J1-2460) and networking support by the COST Actions CA16104 GWverse and CA16214 PHAROS. N. Jordana and C.G. Mundell acknowledge financial support from Mr Jim Sherwin and Mrs Hiroko Sherwin. D. Kopac acknowledges the financial support from the Slovenian Research Agency (research core funding No. P1-0188). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc..

PY - 2022/2/1

Y1 - 2022/2/1

N2 - Context. Gamma-ray burst (GRB) afterglows originate from the interaction between the relativistic ejecta and the surrounding medium. Consequently, their properties depend on several aspects: radiation mechanisms, relativistic shock micro-physics, circumburst environment, and the structure and geometry of the relativistic jet. While the standard afterglow model accounts for the overall spectral and temporal evolution for a number of GRBs, its validity limits emerge when the data set is particularly rich and constraining, especially in the radio band. Aims. We aimed to model the afterglow of the long GRB 160131A (redshift z = 0.972), for which we collected a rich, broadband, and accurate data set, spanning from 6 × 108 Hz to 7 × 1017 Hz in frequency, and from 330 s to 160 days post-burst in time. Methods. We modelled the spectral and temporal evolution of this GRB afterglow through two approaches: (1) the adoption of empirical functions to model an optical/X-ray data set, later assessing their compatibility with the radio domain; and (2) the inclusion of the entire multi-frequency data set simultaneously through the Python package named SAGA (Software for AfterGlow Analysis), to obtain an exhaustive and self-consistent description of the micro-physics, geometry, and dynamics of the afterglow. Results. From deep broadband analysis (from radio to X-ray frequencies) of the afterglow light curves, GRB 160131A outflow shows evidence of jetted emission. Moreover, we observe dust extinction in the optical spectra, and energy injection in the optical/X-ray data. Finally, radio spectra are characterised by several peaks that could be due to either interstellar scintillation (ISS) effects or a multi-component structure. Conclusions. The inclusion of radio data in the broadband set of GRB 160131A makes a self-consistent modelling barely attainable within the standard model of GRB afterglows.

AB - Context. Gamma-ray burst (GRB) afterglows originate from the interaction between the relativistic ejecta and the surrounding medium. Consequently, their properties depend on several aspects: radiation mechanisms, relativistic shock micro-physics, circumburst environment, and the structure and geometry of the relativistic jet. While the standard afterglow model accounts for the overall spectral and temporal evolution for a number of GRBs, its validity limits emerge when the data set is particularly rich and constraining, especially in the radio band. Aims. We aimed to model the afterglow of the long GRB 160131A (redshift z = 0.972), for which we collected a rich, broadband, and accurate data set, spanning from 6 × 108 Hz to 7 × 1017 Hz in frequency, and from 330 s to 160 days post-burst in time. Methods. We modelled the spectral and temporal evolution of this GRB afterglow through two approaches: (1) the adoption of empirical functions to model an optical/X-ray data set, later assessing their compatibility with the radio domain; and (2) the inclusion of the entire multi-frequency data set simultaneously through the Python package named SAGA (Software for AfterGlow Analysis), to obtain an exhaustive and self-consistent description of the micro-physics, geometry, and dynamics of the afterglow. Results. From deep broadband analysis (from radio to X-ray frequencies) of the afterglow light curves, GRB 160131A outflow shows evidence of jetted emission. Moreover, we observe dust extinction in the optical spectra, and energy injection in the optical/X-ray data. Finally, radio spectra are characterised by several peaks that could be due to either interstellar scintillation (ISS) effects or a multi-component structure. Conclusions. The inclusion of radio data in the broadband set of GRB 160131A makes a self-consistent modelling barely attainable within the standard model of GRB afterglows.

KW - Gamma-ray burst: individual: GRB160131A Methods: data analysis

KW - Radiation mechanisms: non-thermal

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Radio data challenge the broadband modelling of GRB 160131A afterglow

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

Access to Document

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