Aims. We present our analysis of the multiwavelength photometric & spectroscopic observations of GRB 060210 and discuss the results in the overall context of current GRB models. Methods. All available optical data underwent a simultaneous temporal fit, while X-ray and γ-ray observations were analysed temporally & spectrally. The results were compared to each other and to possible GRB models. Results. The X-ray afterglow is best described by a smoothly broken power-law with a break at 7.4 h. The late optical afterglow has a well constrained single power-law index which has a value between the two X-ray indices, though it does agree with a single power-law fit to the X-ray. An evolution of the hardness of the high-energy emission is demonstrated and we imply a minimum host extinction from a comparison of the extrapolated X-ray flux to that measured in the optical. Conclusions. We find that the flaring γ-ray and X-ray emission is likely due to internal shocks while the flat optical light curve at that time is due to the external shock. The late afterglow is best explained by a cooling break between the optical and X-rays and continued central engine activity up to the time of the break. The required collimation corrected energy of ∼2 × 1052 erg, while at the high end of the known energy distribution, is not unprecedented.
- Gamma rays: bursts
- ISM: dust, extinction
- Radiation mechanisms: non-thermal
- X-rays: individuals: GRB 060210
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science