Multi-wavelength observations of afterglow of GRB 080319B and the modeling constraints

TL;DR

This study presents multi-wavelength observations of GRB 080319B's afterglow, analyzing its properties and modeling constraints to understand the burst's environment and emission mechanisms.

Contribution

It provides detailed observational data and modeling analysis that constrain the physical parameters and emission mechanisms of GRB 080319B's afterglow.

Findings

Afterglow fits both ISM and stellar wind models equally well.

Synchrotron frequency $ u_m$ is below optical, $ u_c$ below X-rays at ~10^4 s.

Lorentz factor at peak brightness is approximately 300.

Abstract

We present observations of the afterglow of GRB 080319B at optical, mm and radio frequencies from a few hours to 67 days after the burst. Present observations along with other published multi-wavelength data have been used to study the light-curves and spectral energy distributions of the burst afterglow. The nature of this brightest cosmic explosion has been explored based on the observed properties and it's comparison with the afterglow models. Our results show that the observed features of the afterglow fits equally good with the Inter Stellar Matter and the Stellar Wind density profiles of the circum-burst medium. In case of both density profiles, location of the maximum synchrotron frequency $\nu_m$ is below optical and the value of cooling break frequency $\nu_c$ is below $X-$rays, $\sim 10^{4}$s after the burst. Also, the derived value of the Lorentz factor at the time of naked eye brightness is $\sim 300$ with the corresponding blast wave size of $\sim 10^{18}$ cm. The numerical fit to the multi-wavelength afterglow data constraints the values of physical parameters and the emission mechanism of the burst.