THE OPTICAL LUMINOSITY FUNCTION OF GAMMA-RAY BURSTS DEDUCED FROM ROTSE-III OBSERVATIONS
THE OPTICAL LUMINOSITY FUNCTION OF GAMMA-RAY BURSTS DEDUCED FROM ROTSE-III OBSERVATIONS
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DOI：
10.1088/0004-637x/795/2/103
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发表时间：
2014-09
期刊：
影响因子：
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通讯作者：
Xiao-Hong Cui;Xuefeng Wu;Xuefeng Wu;Jun-Jie Wei;F. Yuan;W. Zheng;E. Liang;E. Liang;C. Aker
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文献类型：
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作者：
Xiao-Hong Cui;Xuefeng Wu;Xuefeng Wu;Jun-Jie Wei;F. Yuan;W. Zheng;E. Liang;E. Liang;C. Aker
我们给出了由机器人光学瞬变搜索实验III(ROTSE-III)观测的58个伽马射线暴的均匀样本估计的伽马射线暴的光学光度函数(LF)。我们的伽玛暴样本分为两个子样本：探测到的余辉(18个伽玛暴)和有上限的余辉(40个伽玛暴)。我们推导了爆发后这两个子样100 S的R波段通量。通过假定同运动的伽玛暴速率跟踪恒星形成速率，对100GRB处的光学旋涡进行了拟合。在利用蒙特卡罗模拟对光学LFS进行拟合的同时，我们考虑了ROTSE-III的探测功能。我们发现，在100点S的光发射的累积分布可以用指数增长和指数衰减、破缺的幂定律和谢克特函数来很好地描述。另一方面，单次幂定律(SPL)低频被高度自信地排除。
We present the optical luminosity function (LF) of gamma-ray bursts (GRBs) estimated from a uniform sample of 58 GRBs from observations with the Robotic Optical Transient Search Experiment III (ROTSE-III). Our GRB sample is divided into two sub-samples: detected afterglows (18 GRBs) and those with upper limits (40 GRBs). We derive R-band fluxes for these two sub-samples 100 s after the onset of the burst. The optical LFs at 100 s are fitted by assuming that the co-moving GRB rate traces the star formation rate. While fitting the optical LFs using Monte Carlo simulations, we take into account the detection function of ROTSE-III. We find that the cumulative distribution of optical emission at 100 s is well described by an exponential rise and power-law decay, a broken power law,and Schechter LFs. A single power-law (SPL) LF, on the other hand, is ruled out with high confidence.