Volume 467, Number 3, June I 2007
|Page(s)||1049 - 1055|
|Published online||19 March 2007|
The prompt to late-time multiwavelength analysis of GRB 060210
Astronomical Institute, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: email@example.com
2 Department of Physics & Astronomy, University of Leicester, LE1 7RH, UK
3 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead, CH41 1LD, UK
4 Faculty of Mathematics and Physics, University of Ljubljana, Jadranska 19, 1000 Ljubljana, Slovenia
5 Present Address: INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate (LC), Italy
6 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
7 Present Address: Institut Néel, CNRS, 25 avenue des Martyrs, 38000 Genoble, France
Accepted: 12 March 2007
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 ~21052 erg, while at the high end of the known energy distribution, is not unprecedented.
Key words: gamma rays: bursts / X-rays: individuals: GRB 060210 / ISM: dust, extinction / radiation mechanisms: non-thermal
© ESO, 2007
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