Low frequency view of GRB 190114C reveals time varying shock micro-physics

Autor: K Misra, L Resmi, D A Kann, M Marongiu, A Moin, S Klose, G Bernardi, A de Ugarte Postigo, V K Jaiswal, S Schulze, D A Perley, A Ghosh, Dimple Dimple, H Kumar, R Gupta, M J Michałowski, S Martín, A Cockeram, S V Cherukuri, V Bhalerao, G E Anderson, S B Pandey, G C Anupama, C C Thöne, S Barway, M H Wieringa, J P U Fynbo, N Habeeb
Přispěvatelé: Department of Science and Technology (India), European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Centre (Poland), Australian Research Council
Rok vydání: 2019
Předmět:
Astrophysics::High Energy Astrophysical Phenomena
SWIFT-ERA
PRE-SWIFT
FOS: Physical sciences
Individual - GRB 190114C
Astrophysics
Astrophysics::Cosmology and Extragalactic Astrophysics
01 natural sciences
General - gamma-ray burst
Radio observations
Dimple
0103 physical sciences
010303 astronomy & astrophysics
Gamma-ray burst
QC
Astrophysics::Galaxy Astrophysics
OPTICAL AFTERGLOW
QB
Physics
High Energy Astrophysical Phenomena (astro-ph.HE)
010308 nuclear & particles physics
SYNCHROTRON
Astrophysics::Instrumentation and Methods for Astrophysics
Astronomy and Astrophysics
individual-GRB 190114C
GAMMA-RAY-BURST
AFTERGLOW LIGHT CURVES
Shock (mechanics)
general-gamma-ray burst
Space and Planetary Science
HIGH-ENERGY EMISSION
REVERSE SHOCK
RADIO AFTERGLOW
SCINTILLATION
Astrophysics - High Energy Astrophysical Phenomena
Zdroj: Digital.CSIC. Repositorio Institucional del CSIC
instname
Misra, K, Resmi, L, Kann, D A, Marongiu, M, Moin, A, Klose, S, Bernardi, G, de Ugarte Postigo, A, Jaiswal, V K, Schulze, S, Perley, D A, Ghosh, A, Dimple, D, Kumar, H, Gupta, R, Michalowski, M J, Martin, S, Cockeram, A, Cherukuri, S, Bhalerao, V, Anderson, G E, Pandey, S B, Anupama, G C, Thone, C C, Barway, S, Wieringa, M H, Fynbo, J P U & Habeeb, N 2021, ' Low frequency view of GRB 190114C reveals time varying shock micro-physics ', Monthly Notices of the Royal Astronomical Society, vol. 504, no. 4, pp. 5685-5701 . https://doi.org/10.1093/mnras/stab1050
ISSN: 0035-8711
DOI: 10.48550/arxiv.1911.09719
Popis: Full list of authors: Misra, K.; Resmi, L.; Kann, D. A.; Marongiu, M.; Moin, A.; Klose, S.; Bernardi, G.; de Ugarte Postigo, A.; Jaiswal, V. K.; Schulze, S.; Perley, D. A.; Ghosh, A.; Dimple; Kumar, H.; Gupta, R.; Michałowski, M. J.; Martín, S.; Cockeram, A.; Cherukuri, S. V.; Bhalerao, V.; Anderson, G. E.; Pandey, S. B.; Anupama, G. C.; Thöne, C. C.; Barway, S.; Wieringa, M. H.; Fynbo, J. P. U.; Habeeb, N.
We present radio and optical afterglow observations of the TeV-bright long gamma-ray burst 190114C at a redshift of z = 0.425, which was detected by the Major Atmospheric Gamma Imaging Cherenkov telescope. Our observations with Atacama Large Millimeter/submillitmeter Array, Australia Telescope Compact Array, and upgraded Giant Metre-wave Radio Telescope were obtained by our low frequency observing campaign and range from ∼1 to ∼140 d after the burst and the optical observations were done with three optical telescopes spanning up to ∼25 d after the burst. Long-term radio/mm observations reveal the complex nature of the afterglow, which does not follow the spectral and temporal closure relations expected from the standard afterglow model. We find that the microphysical parameters of the external forward shock, representing the share of shock-created energy in the non-thermal electron population and magnetic field, are evolving with time. The inferred kinetic energy in the blast-wave depends strongly on the assumed ambient medium density profile, with a constant density medium demanding almost an order of magnitude higher energy than in the prompt emission, while a stellar wind-driven medium requires approximately the same amount energy as in prompt emission. © 2021 The Author(s).
We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics (NCRA) of the Tata Institute of Fundamental Research (TIFR). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.01410.T, ADS/JAO.ALMA#2018.A.00020.T. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The Australia Telescope Compact Array (ATCA) is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank Gaurav Waratkar, Viraj Karambelkar, and Shubham Srivastava for undertaking the optical observations with the GIT. The GIT is a 70 cm telescope with a 0.7 deg field of view, set up by the Indian Institute of Astrophysics (IIA, Bengaluru) and the Indian Institute of Technology Bombay (IITB) with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. LR and VKJ acknowledge support from the grant EMR/2016/007127 from Dept. of Science and Technology, India. DAK, AdUP, and CCT acknowledge support from the Spanish research project AYA2017-89384-P. AdUP and CT acknowledge support from funding associated to Ramón y Cajal fellowships (RyC-2012-09975 and RyC-2012-09984). DAK also acknowledges support from the Spanish research project RTI2018-098104-J-I00 (GRBPhot). KM, SBP, and RG acknowledge BRICS grant DST/IMRCD/BRICS/Pilotcall/ProFCheap/2017(G) for this work. V. Jaiswal and S. V. Cherukuri thank Ishwara-Chandra C. H. for kindly making GMRT data analysis pipeline available. L Resmi thanks Johannes Buchner for helpful discussions on pyMultinest. Harsh Kumar thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant #1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. The Cosmic Dawn Center is funded by the DNRF. JPUF thanks the Carlsberg Foundation for support. MJM acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208. GEA is the recipient of an Australian Research Council Discovery Early Career Researcher Award (project number DE180100346) funded by the Australian Government.
With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
Databáze: OpenAIRE
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