俄土1.5米望远镜对GRB 060526光学余辉的观测
Observations of GRB 060526 Optical Afterglow with Russian-Turkish 1.5-m Telescope
摘要：
本文介绍了用俄罗斯-土耳其1.5米望远镜（RTT 150，Mt. Bakirlitepe，土耳其）。从γ暴发生后5小时开始，连续5个夜晚进行了余辉光变曲线的详细测量。此外，在观测的第一个晚上的余辉的快速变化的上限，并详细测量了余辉颜色变化的历史。在爆发后6 ~ 16小时的时间间隔内，有一个逐渐的通量衰减，可以近似地描述为指数为-1.14 ± 0.02的幂律。在此之后，观察到时间尺度上的变化δt < t，并且余辉开始更快地衰减。余辉的颜色，V-R=~0.5，在我们所有的观测中大致相同。在ΔF_v/F_v =~ 0.3时，在δt/t =~ 0.0055的时间尺度上探测到了这种变化，这违反了Ioka等人（2005）对观测到的超相对论喷流辐射变化的一些限制。我们建议用发射壳层的运动此时不再是超相对论性的这一事实来解释这种变化。
英文摘要：
We present the results of the photometric multicolor observations of GRB 060526 optical afterglow obtained with Russian-Turkish 1.5-m Telescope (RTT150, Mt. Bakirlitepe, Turkey). The detailed measurements of afterglow light curve, starting from about 5 hours after the GRB and during 5 consecutive nights were done. In addition, upper limits on the fast variability of the afterglow during the first night of observations were obtained and the history of afterglow color variations was measured in detail. In the time interval from 6 to 16 hours after the burst, there is a gradual flux decay, which can be described approximately as a power law with an index of -1.14+-0.02. After that the variability on the time scale δt < t is observed and the afterglow started to decay faster. The color of the afterglow, V-R=~0.5, is approximately the same during all our observations. The variability is detected on time scales up to δt/t =~ 0.0055 at ΔF_ν/F_ν=~ 0.3, which violates some constraints on the variability of the observed emission from ultrarelativistic jet obtained by Ioka et al. (2005). We suggest to explain this variability by the fact that the motion of the emitting shell is no longer ultrarelativistic at this time.
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