Curran 2007 GRB060210的多波段观测

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astro-ph/0701087 [abs, ps, pdf, other] :

Title: The prompt to late-time multiwavelength analysis of GRB 060210
Authors: P.A. Curran (1), A.J. van der Horst (1), A.P. Beardmore (2), K.L. Page (2), E. Rol (2), A. Melandri (3), I.A. Steele (3), C.G. Mundell (3), A. Gomboc (4), P.T. O'Brien (2), D.F. Bersier (3), M.F. Bode (3), D. Carter (3), C. Guidorzi (3,5), J.E. Hill (6), C.P. Hurkett (2), S. Kobayashi (3), A. Monfardini (3,7), C.J. Mottram (3), R.J. Smith (3), R.A.M.J. Wijers (1), R. Willingale (2) ((1)Astronomical Institute, University of Amsterdam, (2)Department of Physics & Astronomy, University of Leicester, (3)Astrophysics Research Institute, Liverpool John Moores University, (4)Faculty of Mathematics and Physics, University of Ljubljana, (5)INAF - Osservatorio Astronomico di Brera, (6)NASA Goddard Space Flight Center, (7)Institut Neel, CNRS)
Comments: 8 pages, 4 figures, submitted to Astronomy & Astrophysics

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. All available optical data underwent a simultaneous temporal fit, while X-ray and gamma-ray observations were analysed temporally & spectrally. The results were compared to each other and to possible GRB models. The X-ray afterglow is best described by a smoothly broken power-law with a break at 7.4 hours. 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. We find that the flaring gamma-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 ~ 2x10^52 erg, while at the high end of the known energy distribution, is not unprecedented.