2007A&A...470..105M

GRB 060614 is a remarkable gamma-ray burst (GRB) observed by Swift with puzzling properties, which challenge current progenitor models. In particular, the lack of any bright supernova (SN) down to very strict limits and the vanishing spectral lags during the whole burst are typical of short GRBs, strikingly at odds with the long (102 s) duration of this event. Here we present detailed spectral and temporal analysis of the Swift observations of GRB 060614. We show that the burst presents standard optical, ultraviolet and X-ray afterglows, detected beginning 4ks after the trigger. An achromatic break is observed simultaneously in the optical and X-ray bands, at a time consistent with the break in the R-band light curve measured by the VLT. The achromatic behaviour and the consistent post-break decay slopes make GRB060614 one of the best examples of a jet break for a Swift burst. The optical and ultraviolet afterglow light curves have also an earlier break at 29.7±4.4ks, marginally consistent with a corresponding break at 36.6±2.4ks observed in the X-rays. In the optical, there is strong spectral evolution around this break, suggesting the passage of a break frequency through the optical/ultraviolet band. The very blue spectrum at early times suggests this may be the injection frequency, as also supported by the trend in the light curves: rising at low frequencies, and decaying at higher energies. The early X-ray light curve (from 97 to 480s) is well interpreted as the X-ray counterpart of the burst extended emission. Spectral analysis of the BAT and XRT data in the ∼80s overlap time interval show that the peak energy of the burst has decreased to as low as 8keV at the beginning of the XRT observation. Spectral analysis of following XRT data shows that the peak energy of the burst continues to decrease through the XRT energy band and exits it at about 500s after the trigger. The average peak energy E_p of the burst is likely below the BAT energy band (<24keV at the 90% confidence level) but larger than 8keV. The initial group of peaks observed by BAT (∼5s) is however distinctly harder than the rest of the prompt emission, with a peak energy of about 300keV as measured by Konus Wind. Considering the time-averaged spectral properties, GRB 060614 is consistent with the E_iso-E_p^rest, E_γ-E_p^rest, and L_p,iso-E_p^rest correlations.