The exceptionally powerful TeV γ-ray emitters in the Large Magellanic Cloud
The exceptionally powerful TeV γ-ray emitters in the Large Magellanic Cloud
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DOI：
10.1126/science.1261313
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发表时间：
2015-01-23
期刊：
影响因子：
56.9
通讯作者：
Zechlin, H-S.
中科院分区：
文献类型：
--
作者：
Abramowski, A.;Aharonian, F.;Zechlin, H-S.
大麦哲伦星云是银河系的一个卫星星系，利用高能立体观测系统（High Energy Stereoscopic System，H.E.S.S.）超过1000亿电子伏的能量，深度曝光210小时。探测到了三种不同类型的来源：已知能量最高的脉冲星N 157 B的脉冲星风星云;射电噪声最大的超新星遗迹N 132 D;以及最大的非热X射线壳层，超级气泡30 Dor C。SN 1987 A是一个独特的天体，但出人意料的是，它没有被探测到，这限制了非常年轻的超新星遗迹中粒子加速的理论框架。这些探测揭示了外部星系中g射线源群体的最具能量的尖端，并通过30 D或C提供了对超气泡g射线发射的明确探测。
The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known, N 157B; the radio-loud supernova remnant N 132D; and the largest nonthermal x-ray shell, the superbubble 30 Dor C. The unique object SN 1987A is, unexpectedly, not detected, which constrains the theoretical framework of particle acceleration in very young supernova remnants. These detections reveal the most energetic tip of a g-ray source population in an external galaxy and provide via 30 Dor C the unambiguous detection of g-ray emission from a superbubble.