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: firstname.lastname@example.org
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.