Figure 4 - available via license: Creative Commons Attribution 4.0 International
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Proper motion of GRB 170817A relative to 8 d HST measurement. The blue line represents the result obtained from our model, based on the bestfitting parameters, while the shaded areas depict the 68 per cent confidence intervals. The proper motion measured between 8-75, 8-206, and 8-230 d is 2.41 ± 0.38, 4.09 ± 0.42, and 5.07 ± 0.40 mas, respectively (Mooley, Anderson & Lu 2022 ).
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The afterglow of a gamma-ray burst (GRB) has been widely argued to arise from the interaction of a relativistic outflow with its ambient medium. During such an interaction, a pair of shocks are generated: a forward shock that propagates into the medium, and a reverse shock that propagates into the outflow. Extensive studies have been conducted on t...
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... × 10 53 ergs) and initial Lorentz factor ( 0 ≈ 262) imply that the afterglow emission originates from a narrowly collimated jet. GRB 160821B is a short GRB at redshift z = 0.162. In the bottom right-hand panel of Fig. 2 , we present the multi-wavelength observations starting from ∼0.1 d after the bursts, along with the fits derived in our model. Fig. A4 displays the corner plots showing the results of our MCMC parameter estimation. In the study of GRB 160821B conducted by Lamb et al. ( 2019b ), the reverse shock is dominant at 1 d at 5 GHz, a kilonova component emerged in the optical and infrared bands during a time interval of ∼1-5 d. Additionally, an excess in X-ray at 3-4 d ...
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... dimensionless velocity is given by β app = v app / c . In Fig. 4 , we present the angular displacement of flux centroid calculated by our model with the fitting parameters. The consistency between the model and the data suggests that our model can also reproduce the superluminal motion of the flux centroid. The average apparent velocities from 8 to 75 d and from 8 to 230 d, calculated using the ...
