GRB 080319 B的肉眼观测：自然界的爆发
Observations of the Naked-Eye GRB 080319B: Implications of Nature's Brightest Explosion
摘要：
第一个伽马射线暴（GRB）被证实足够明亮，可以用肉眼看到，GRB 080319 B的红移z = 0.937，允许在电磁波谱上进行精确的后续观测。我们提出了我们详细的光学和红外观测的余辉，包括超过5000幅图像开始后51秒的GRB触发，与我们自己的分析斯威夫特数据。这一事件不仅在观测性质上极端，而且在本质上也是极端的：它是有史以来在光学和红外波长上记录的最明亮的事件，并且在伽马射线中具有极高的各向同性等效能量释放。在早期，余辉的演变大致上是一致的反向冲击占主导地位，但随后被一个前向冲击在1000秒左右。整个光谱能量分布，从紫外线到近红外波长，显示没有证据表明大量的尘埃消光的主机帧。然而，余辉的演变是高度彩色的：从大约1000秒开始，指数向蓝移，然后在后期移回红色。在我们最深的晚期观测中，我们发现了光学喷流破裂和发光超新星的初步证据。最后，我们研究了当前和未来设施对此类事件的可检测性，发现BAT可以在z = 10.7（8 sigma）的伽马射线中检测到此类事件，而标称EXIST灵敏度将允许检测z ~ 32。在K波段，这个源很容易被米级望远镜检测到z ~ 17。
英文摘要：
The first gamma-ray burst (GRB) confirmed to be bright enough to be seen with the naked eye, GRB 080319B at redshift z = 0.937, allowed for exquisite follow-up observations across the electromagnetic spectrum. We present our detailed optical and infrared observations of the afterglow, consisting of over 5000 images starting 51 s after the GRB trigger, in concert with our own analysis of the Swift data. The event is extreme not only in observed properties but intrinsically: it was the most luminous event ever recorded at optical and infrared wavelengths and had an exceedingly high isotropic-equivalent energy release in gamma-rays. At early times, the afterglow evolution is broadly consistent with being reverse-shock dominated, but then is subsumed by a forward shock at around 1000 s. The overall spectral energy distribution, spanning from ultraviolet through near-infrared wavelengths, shows no evidence for a significant amount of dust extinction in the host frame. The afterglow evolution, however, is highly chromatic: starting at about 1000 s the index shifts blueward before shifting back to the red at late times. In our deepest late-time observations, we find tentative evidence for an optical jet break and a luminous supernova. Finally, we examine the detectability of such events with current and future facilities and find that such an event could be detected in gamma-rays by BAT out to z = 10.7 (8 sigma), while the nominal EXIST sensitivity would allow detection to z ~ 32. At K band, this source would have been easily detected with meter-class telescopes to z ~ 17.
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