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    Rapid radio brightening of GRB 210702A

    96268.pdf (1.963Mb)
    Access Status
    Open access
    Authors
    Anderson, Gemma E.
    Russell, T.D.
    Fausey, H.M.
    van der Horst, A.J.
    Hancock, Paul J.
    Bahramian, Arash
    Bell, M.E.
    Miller-Jones, James C. A.
    Rowell, G.
    Sammons, Mawson W.
    Wijers, R.A.M.J.
    Galvin, Timothy J.
    Goodwin, Adelle J.
    Konno, R.
    Rowlinson, A.
    Ryder, S.D.
    Schüssler, F.
    Wagner, S.J.
    Zhu, S.J.
    Date
    2023
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Anderson, G.E. and Russell, T.D. and Fausey, H.M. and van der Horst, A.J. and Hancock, P.J. and Bahramian, A. and Bell, M.E. et al. 2023. Rapid radio brightening of GRB 210702A. Monthly Notices of the Royal Astronomical Society. 523 (4): pp. 4992-5005.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/stad1635
    ISSN
    0035-8711
    Faculty
    Faculty of Science and Engineering
    School
    School of Elec Eng, Comp and Math Sci (EECMS)
    Curtin Institute for Data Science (CIDS)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/DE180100346
    http://purl.org/au-research/grants/arc/DP200102471
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2023 The Author(s Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/96504
    Collection
    • Curtin Research Publications
    Abstract

    We observed the rapid radio brightening of GRB 210702A with the Australia Telescope Compact Array (ATCA) just 11 h post-burst, tracking early-time radio variability over a 5 h period on ∼15 min time-scales at 9.0, 16.7, and 21.2 GHz. A broken power law fit to the 9.0 GHz light curve showed that the 5 h flare peaked at a flux density of 0.4 ± 0.1 mJy at ∼13 h post-burst. The observed temporal and spectral evolution is not expected in the standard internal–external shock model, where forward and reverse shock radio emission evolves on much longer time-scales. The early-time (<1 d) optical and X-ray light curves from the Neil Gehrels Swift Observatory demonstrated typical afterglow forward shock behaviour, allowing us to use blast wave physics to determine a likely homogeneous circumburst medium and an emitting electron population power-law index of p = 2.9 ± 0.1. We suggest that the early-time radio flare is likely due to weak interstellar scintillation (ISS), which boosted the radio afterglow emission above the ATCA sensitivity limit on minute time-scales. Using relations for ISS in the weak regime, we were able to place an upper limit on the size of the blast wave of ≤6 × 1016 cm in the plane of the sky, which is consistent with the theoretical forward shock size prediction of 8 × 1016 cm for GRB 210702A at ∼13 h post-burst. This represents the earliest ISS size constraint on a gamma-ray burst (GRB) blast wave to date, demonstrating the importance of rapid (<1 d) radio follow-up of GRBs using several-hour integrations to capture the early afterglow evolution and to track the scintillation over a broad frequency range.

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