太周探测(V)

结 语

近代天文观测从六十年代的四大发现到后来的冲出地球和走向极致，体现了人类无尽的探索欲望。在从射频到紫外乃至X射线等的宽广频谱范围内人们已采用了多种技术来实现苛刻的天文观测要求，包括从无线和红外两个方面向太赫兹间隙逼近直至将其完全填充。新的技术不断取代旧的技术，例如早期用于微波接收的脉泽和参量放大等已被InP基HEMT等器件取代；然而，旧的甚至“古老”的技术也还在继续使用并不断更新迭代，在性能和规模上走向极致，典型如红外波段的InSb和MCT器件，以及从红外延伸到THz波段的IBC和Bolometer器件等；此外，也时有新型器件加入，如超导混频器以及可具有宽响应波长范围和极高灵敏度的超导相变光电探测器等。IBC、Bolometer和超导相变器件本身都可具有高性能或者说高量子效率，但都需要极低的工作温度，有些需要2 K以下甚至更低，而天文观测本身也不得不使仪器乃至航天器本体也保持在足够低的对应温度，因此采用这样的器件是匹配的；然而，电子学器件及其系统为避免载流子冻结则不能有过低的工作温度，系统中电子和光电二类器件需要综合考虑兼顾。目前，地面上单个射电望远镜的主反射天线口径已达500米（FAST），空间红外望远镜的主反射镜口径已达6.5米（JWST），功能也越来越趋于专门化。天文观测一甲子的发展丰富多彩可圈可点，也需要各抱地势勾心斗角，回顾过往了解一些“常识”并进行纵向和横向的比较，将有利于开展新的探索。

Teracycle detection: Starting from the four major 

astronomical discoveries in 1960s

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