% IMPORTANT: The following is UTF-8 encoded.  This means that in the presence
% of non-ASCII characters, it will not work with BibTeX 0.99 or older.
% Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or
% “biber”.

@ARTICLE{Anderson:586748,
      author       = {Anderson, Gemma 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. and Miller-Jones, J. C. A. and Rowell, G.
                      and Sammons, M. W. and Wijers, R. A. M. J. and Galvin, T. J.
                      and Goodwin, A. J. and Konno, R. and Rowlinson, A. and
                      Ryder, S. D. and Schussler, F. and Wagner, S. J. and Zhu, S.
                      J.},
      title        = {{R}apid radio brightening of {GRB} 210702{A}},
      journal      = {Monthly notices of the Royal Astronomical Society},
      volume       = {523},
      number       = {4},
      issn         = {0035-8711},
      address      = {Oxford},
      publisher    = {Oxford Univ. Press},
      reportid     = {PUBDB-2023-03986, arXiv:2211.11212. arXiv:2211.11212},
      pages        = {4992 - 5005},
      year         = {2023},
      note         = {Submitted to MNRAS 13 pages, 6 figures, 2 tables Waiting
                      for fulltext},
      abstract     = {We observed the rapid radio brightening of GRB 210702A with
                      the Australian Telescope Compact Array (ATCA) just 11hr
                      post-burst, tracking early-time radio variability over a 5hr
                      period on ~15min timescales at 9.0, 16.7, and 21.2GHz. A
                      broken power-law fit to the 9.0GHz light curve showed that
                      the 5hr flare peaked at a flux density of 0.4+/-0.1mJy at
                      ~13hr post-burst with a steep rise and decline. The observed
                      temporal and spectral evolution are not expected in the
                      standard internal-external shock model, where forward and
                      reverse shock radio emission evolves on much longer
                      timescales. The early-time (<1day) 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 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 timescales. Using weak ISS
                      relations, we were able to place an upper limit on the size
                      of the blast wave of $\leq6 \times 10^{16}$cm in the plane
                      of the sky, which is consistent with the theoretical forward
                      shock size prediction of $8\times10^{16}$cm for GRB 210702A
                      at ~13h post-burst. This represents the earliest ISS size
                      constraint on a GRB blast wave to date, demonstrating the
                      importance of rapid (<1day) radio follow-up of GRBs using
                      several-hour integrations to capture the early afterglow
                      evolution, and to track scintillation over a broad frequency
                      range.},
      cin          = {ZEU-HESS},
      ddc          = {520},
      cid          = {I:(DE-H253)ZEU-HESS-20140213},
      pnm          = {613 - Matter and Radiation from the Universe (POF4-613)},
      pid          = {G:(DE-HGF)POF4-613},
      experiment   = {EXP:(DE-H253)HESS-20170101},
      typ          = {PUB:(DE-HGF)16},
      eprint       = {2211.11212},
      howpublished = {arXiv:2211.11212},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2211.11212;\%\%$},
      UT           = {WOS:001023895800008},
      doi          = {10.1093/mnras/stad1635},
      url          = {https://bib-pubdb1.desy.de/record/586748},
}