Low frequency view of GRB 190114C reveals time varying shock micro-physics. (arXiv:1911.09719v2 [astro-ph.HE] UPDATED)

Low frequency view of GRB 190114C reveals time varying shock micro-physics. (arXiv:1911.09719v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Misra_K/0/1/0/all/0/1">K. Misra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Resmi_L/0/1/0/all/0/1">L. Resmi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kann_D/0/1/0/all/0/1">D. A. Kann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marongiu_M/0/1/0/all/0/1">M. Marongiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moin_A/0/1/0/all/0/1">A. Moin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klose_S/0/1/0/all/0/1">S. Klose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardi_G/0/1/0/all/0/1">G. Bernardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Postigo_A/0/1/0/all/0/1">A. de Ugarte Postigo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaiswal_V/0/1/0/all/0/1">V. K. Jaiswal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulze_S/0/1/0/all/0/1">S. Schulze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perley_D/0/1/0/all/0/1">D. A. Perley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghosh_A/0/1/0/all/0/1">A. Ghosh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dimple/0/1/0/all/0/1">Dimple</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_H/0/1/0/all/0/1">H. Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_R/0/1/0/all/0/1">R. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michalowski_M/0/1/0/all/0/1">M. J. Michałowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_S/0/1/0/all/0/1">S. Martín</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cockeram_A/0/1/0/all/0/1">A. Cockeram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cherukur_S/0/1/0/all/0/1">S. V. Cherukur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhalerao_V/0/1/0/all/0/1">V. Bhalerao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_G/0/1/0/all/0/1">G. E. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_S/0/1/0/all/0/1">S. B. Pandey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anupama_G/0/1/0/all/0/1">G. C. Anupama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thone_C/0/1/0/all/0/1">C. C. Thöne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barway_S/0/1/0/all/0/1">S. Barway</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wieringa_M/0/1/0/all/0/1">M. H. Wieringa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fynbo_J/0/1/0/all/0/1">J. P. U. Fynbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Habeeb_N/0/1/0/all/0/1">N. Habeeb</a>

We present radio and optical afterglow observations of the TeV-bright long
Gamma Ray Burst (GRB) 190114C at a redshift of $z=0.425$, which was detected by
the MAGIC telescope. Our observations with ALMA, ATCA, and uGMRT were obtained
by our low frequency observing campaign and range from $sim1$ to $sim140$
days after the burst and the optical observations were done with three optical
telescopes spanning up to $sim25$ days 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.

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