What we learn from the afterglow of GRB 021211

Details What we learn from the afterglow of GRB 021211 What we learn from the afterglow of GRB 021211

2003-02-20

arxiv.org/abs/astro-ph/0302429v2

Astrophys.J. 593 (2003) 961-967

Astronomy and Astrophysics

Astrophysics

Figures 4 and 5 replaced by correct figures

Scientific paper

10.1086/376570

The behaviour of the afterglow (AG) of gamma-ray bursts (GRBs) directly provides, in the cannonball (CB) model, information about the environment of their progenitor stars. The well observed early temporal decline of the AG of GRB 021211 is precisely the one predicted in the presence of a progenitor's ``wind'' which resulted in a density profile $\propto 1/r^2$ around the star. The subsequent fast fading --which makes this GRB ``quasi-dark''-- is the one anticipated if, further away, the interstellar density is roughly constant and relatively high. The CB-model fit to the AG clearly shows the presence of an associated supernova akin to SN1998bw, and allows even for the determination of the broad-band spectrum of the host galaxy. GRB 990123 and GRB 021004, whose AGs were also measured very early, are also discussed.

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