Abstract
Abstract Two components of jets associated with the afterglow of the gamma-ray burst (GRB) 160623A were observed with multifrequency observations including long-term monitoring in a submillimeter range (230 GHz) using the Submillimeter Array. The observed light curves with temporal breaks suggest on the basis of the standard forward-shock synchrotron-radiation model that the X-ray radiation is narrowly collimated with an opening angle , whereas the radio radiation originated from wider jets (∼27°). The temporal and spectral evolutions of the radio afterglow agree with those expected from a synchrotron-radiation modeling with typical physical parameters, except for the fact that the observed wide jet opening angle for the radio emission is significantly larger than the theoretical maximum opening angle. By contrast, the opening angle of the X-ray afterglow is consistent with the typical value of GRB jets. Since the theory of the relativistic cocoon afterglow emission is similar to that of a regular afterglow with an opening angle of ∼30°, the observed radio emission can be interpreted as the shocked jet cocoon emission. This result therefore indicates that the two components of the jets observed in the GRB 160623A afterglow are caused by the jet and the shocked jet cocoon afterglows.
Highlights
The Gamma-ray burst (GRB) is believed to be a stellar explosion accompanied with relativistic outflows and narrowly-collimated jets (e.g. Piran 1999)
Since direct imaging of GRB jets is impossible unlike AGN jets, the jet opening angles of GRBs have been measured by identifying a temporal break in the light curve in multi-frequency afterglow monitoring (Sari et al 1999)
The typical value of GRB jet opening-angles is ∼ 3◦.5 (e.g. Racusin et al 2009), which is in the same order with that of AGN jets measured with high-resolution imaging observations (Pushkarev et al 2017)
Summary
The Gamma-ray burst (GRB) is believed to be a stellar explosion accompanied with relativistic outflows and narrowly-collimated jets (e.g. Piran 1999). Since direct imaging of GRB jets is impossible unlike AGN jets, the jet opening angles of GRBs have been measured by identifying a temporal break in the light curve in multi-frequency afterglow monitoring (Sari et al 1999). Racusin et al 2009), which is in the same order with that of AGN jets (median of 1◦.5 among 373 samples) measured with high-resolution imaging observations (Pushkarev et al 2017). We report the long-term monitoring of the GRB160623A afterglow using the Sub-millimeter Array (SMA) in conjunction with multi-frequency observations.
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