Probing the multiwavelength emission scenario of GRB 190114C. (arXiv:2206.11148v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Klinger_M/0/1/0/all/0/1">Marc Klinger</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Tak_D/0/1/0/all/0/1">Donggeun Tak</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_A/0/1/0/all/0/1">Andrew Taylor</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_S/0/1/0/all/0/1">Sylvia J. Zhu</a> (1) ((1) Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, Germany)

Multiwavelength observation of the gamma-ray burst, GRB 190114C, opens a new
window for studying the emission mechanism of GRB afterglows. Its
Very-High-Energy (VHE; $gtrsim 100$ GeV) detection has motivated an inverse
Compton interpretation for the emission, but this has not been tested. Here, we
revisit the early afterglow emission from 68 to 180 seconds and perform the
modeling likelihood analysis with the keV to TeV datasets. We compute for the
first time the statistical preference in the combined synchrotron (syn) and
synchrotron self-Compton (SSC) model over the syn-only model. In agreement with
earlier analyses, between 68 and 110 seconds an unstable preference for the SSC
model can be found, which can also be explained by systematic cross calibration
effect between the included instruments. We conclude that there is no stable
statistical preference for one of the two models.

Multiwavelength observation of the gamma-ray burst, GRB 190114C, opens a new
window for studying the emission mechanism of GRB afterglows. Its
Very-High-Energy (VHE; $gtrsim 100$ GeV) detection has motivated an inverse
Compton interpretation for the emission, but this has not been tested. Here, we
revisit the early afterglow emission from 68 to 180 seconds and perform the
modeling likelihood analysis with the keV to TeV datasets. We compute for the
first time the statistical preference in the combined synchrotron (syn) and
synchrotron self-Compton (SSC) model over the syn-only model. In agreement with
earlier analyses, between 68 and 110 seconds an unstable preference for the SSC
model can be found, which can also be explained by systematic cross calibration
effect between the included instruments. We conclude that there is no stable
statistical preference for one of the two models.

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