UFFO（超快闪光观测站）探路者
The UFFO (Ultra-Fast Flash Observatory) Pathfinder
摘要：
自从发现光学余辉以来，已经测量了数百个伽马射线暴（GRB）紫外光变曲线，然而，即使在SWIFT天文台运行近5年后，也只有少数测量在伽玛射线信号之后不久（一分钟内）进行。这种早期观测的缺乏未能解决与爆发事件和祖先相关的短时间尺度的爆发物理学。由于缺乏亚分钟数据，短硬型伽玛暴和快速上升伽玛暴的紫外-光学光变曲线的特征，这可能占所有伽玛暴的~30%，仍然是实际未知的。我们已经制定了在适合于在微型卫星上发射的小型航天器观测站中达到亚分钟和亚秒时标的方法。我们不是旋转整个航天器来将紫外光学仪器对准伽玛射线暴的位置，而是使用快速移动的镜子来重新定向我们的光束。我们的合作已经产生了一个独特的MEMS（微机电系统）阵列，它可以在1毫秒内指向和解决目标。这项技术已经得到了证明，在2009年9月作为MTEL（极端闪电的MEMS望远镜）在Tatiana-2航天器上成功飞行，并在2008年4月作为KAMTEL在国际空间站上成功飞行。对每年数十个γ暴紫外光辐射的亚分钟测量将对现有的内激波模型进行更严格的检验，探测体洛伦兹因子的极值，并提供第一个早期和详细的快速上升和短型γ暴紫外光光变曲线的测量。
英文摘要：
Hundreds of gamma-ray burst (GRB) UV-optical light curves have been measured since the discovery of optical afterglows, however, even after nearly 5 years of operation of the SWIFT observatory, only a handful of measurements have been made soon (within a minute) after the gamma ray signal. This lack of early observations fails to address burst physics at the short time scales associated with burst events and progenitors. Because of this lack of sub-minute data, the characteristics of the UV-optical light curve of short-hard type GRB and rapid-rising GRB, which may account for ~30% of all GRB, remain practically unknown. We have developed methods for reaching the sub-minute and the sub-second timescales in a small spacecraft observatory appropriate for launch on a microsatellite. Rather than slewing the entire spacecraft to aim the UV-optical instrument at the GRB position, we use rapidly moving mirrors to redirect our optical beam. Our collaboration has produced a unique MEMS (microelectromechanical systems) micromirror array which can point and settle on target in only 1 ms. This technology is proven, flying successfully as the MTEL (MEMS Telescope for Extreme Lightning) on the Tatiana-2 Spacecraft in September 2009 and as the KAMTEL on the International Space Station in April 2008. The sub-minute measurements of the UV-optical emission of dozens of GRB each year will result in a more rigorous test of current internal shock models, probe the extremes of bulk Lorentz factors, and provide the first early and detailed measurements of fast-rise and short type GRB UV-optical light curves.
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