应用于太赫兹天文探测的微波动态电感探测器研究进展

石佩玲; 贺青

doi:10.11884/HPLPB202537.250001

应用于太赫兹天文探测的微波动态电感探测器研究进展

doi: 10.11884/HPLPB202537.250001

石佩玲^1,,
贺青^2, ,

1.
中国电子科技集团公司第九研究所，四川绵阳 621010
2.
中国工程物理研究院电子工程研究所，四川绵阳 621900

基金项目: 中国工程物理研究院院长基金自立项目(YZJJZL2023054)、四川省自然科学基金青年基金项目(2024NSFSC1431)

详细信息

作者简介:
石佩玲，zeitlup@qq.com

通讯作者:
贺　青，18583852658@163.com。

中图分类号: P16;P11
计量
- 文章访问数: 55
- HTML全文浏览量: 22
- PDF下载量: 10
- 被引次数: 0
出版历程
- 收稿日期: 2025-01-01
- 修回日期: 2025-03-31
- 录用日期: 2025-03-24
- 网络出版日期: 2025-04-08

Research progress of microwave kinetic inductance detector applied to terahertz astronomical detection

Shi Peiling^1
,,
He Qing^{2
, ,}

1.
China Electronics Technology Group Corporation 9th Research Institute, Mianyang 621010, China
2.
Institute of Electronic Engineering, CAEP, Mianyang 621900, China

摘要

摘要: 太赫兹波是介于微波和远红外区域之间的毫米/亚毫米波，波长从3 mm到30 μm。自宇宙开始以来发射的所有可探测光子中，98%落在太赫兹和远红外区域，其中许多光子来自宇宙微波背景辐射，其他重要的发射来自大量的受激分子，这些分子在太赫兹范围内具有明亮的光谱发射特征。基于太赫兹的天文观测技术在天体物理和宇宙学的研究中扮演着愈加重要的作用，对星际原子、分子和尘埃的太赫兹观测可以洞察宇宙星际介质的内部条件，并提供对恒星、行星、星系和宇宙本身起源和演化的独特观察窗口。近年来，许多大型天文望远镜不断部署基于微波动态电感探测器（MKID）的太赫兹探测器，MKID成为了太赫兹天文探测领域重要的技术手段。本文主要阐述MKID的基础原理和应用在太赫兹探测领域的研究进展，通过MKID在多个太赫兹天文探测项目的应用总结，厘清MKID 探测器的工作原理和架构，梳理MKID取得的突破，并对其发展进行展望。
- 太赫兹 /
- 电感探测器 /
- 天文探测 /
- 超导谐振器
Abstract: Terahertz waves, spanning the millimeter and submillimeter wavelength ranges between the microwave and far-infrared regions (approximately 3 mm to 30 μm), represent a critical spectral range in astrophysical and cosmological research. Of the photons detectable since the beginning of the universe, approximately 98% fall within the terahertz and far-infrared bands. A significant proportion of these photons originate from the cosmic microwave background radiation, while others arise from excited molecules that exhibit bright spectral emissions in the terahertz range. As a result, terahertz-based astronomical observation techniques are becoming increasingly essential for investigating the universe’s fundamental properties. Through the observation of interstellar atoms, molecules, and dust, terahertz astronomy provides valuable insights into the internal conditions of the interstellar medium and offers a unique observational window into the formation and evolution of stars, planets, galaxies, and the universe itself. In recent years, many large astronomical telescopes have begun incorporating terahertz detectors based on microwave kinetic inductance detector (MKID), positioning MKID as a pivotal technology in the field of terahertz astronomical detection. This paper outlines the fundamental principles of MKID, reviews recent advancements in their application to terahertz detection, and discusses future developments in this promising area of research.
- terahertz /
- inductance detectors /
- astronomical detection /
- superconducting resonator

HTML全文

图 1 共面波导和集总式超导微波谐振器结构^[43]

Figure 1. Coplanar waveguide and lumped superconducting microwave resonator structures^[43]

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图 2 MKID工作原理^[20]

Figure 2. Working principle of MKID^[20]

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图 3 天线耦合型MKID^[47]及LEKID^[48]

Figure 3. Antenna-coupled MKID^[47] and LEKID^[48]

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图 4 MKID读出系统^[45]

Figure 4. The readout system of MKID^[45]

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图 5 片上光谱仪结构示意图^[49]

Figure 5. Schematic diagram of the on-chip spectrometer structure.^[49]

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图 6 DESHIMA 第一代和第二代的示意图^[52]

Figure 6. Schematic diagrams of DESHIMA1.0 and DESHIMA 2.0^[52]

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图 7 BLAST-TNG 结构^[66]

Figure 7. The structure of BLAST-TNG^[66]

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图 8 TolTEC 结构^[22]

Figure 8. The structure of TolTEC^[22]

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图 9 用于CMB探测的MKID设计示意图^[71]

Figure 9. Schematic diagram of the design of MKID for CMB detection^[71]

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图 10 包含了2100个像元的CORE^[72]

Figure 10. CORE containing 2,100 pixels^[72]

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图 11 DemoCam相机^[82]

Figure 11. The camera of DemnoCam^[82]

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图 12 MACSJ1423.8+2404星团的多波长图像，其中蓝色和黄色线圈区域由NIKA完成^[91]

Figure 12. Multi-wavelength images of the MACSJ1423.8+2404 cluster, where the areas within the blue and yellow coils were completed by NIKA^[91]

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图 13 低温 LED 像素和频率映射的动态电感探测器阵列^[108]

Figure 13. Cryogenic LED pixel-to-frequency mapper for kinetic inductance detector arrays ^[108]

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表 1 基于MKID的片上光谱仪

Table 1. On-chip spectrometers based on MKID

spectrometers	scale (channels/pixels)	frequency/GHz	wavelength/mm	materials	installation
SuperSpec	500	195-310	1.54-0.97	Nb、TiN	LMT
DESHIMA	49	332-377	0.903-0.795	NbTiN、Al	ASTE
DESHIMA2.0	347	220-440	1.36-0.682	NbTiN、A1	ASTE
CAMELS	500	103-114.7	2.9-2.6	NbN、Ta	Greenland Telescope
Micro-Spec	355	540-420	0.555-0.714	Nb、Al	EXCLAIM
WSPEC	54	135-175	2.2-1.7	A1	−
WSPEC	54	190-250	1.6-1.2	A1	−

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表 2 基于MKID的偏振计

Table 2. Polarimeters based on MKID

polarimeters	pixels	frequency/GHz	wavelength/mm	materials	installation(loading mode)
BLAST-TNG	1836/938/544	1200、857、600	0.25、0.35、0.5	TiN	BLAST-TNG
MUSCAT	1600	273	1.1	A1	LMT
ToITEC	1900/950/475	270、214、150	1.1、1.4、2	TiN/Ti/TiN	LMT
CORE	2100	60-600	5-0.5	NbTiN, A1	LiteBIRD
SKIP	2317	150、260-350	2、1.2-0.9	A1	Balloon-borne
B-SIDE	980-1800	400-700	0.75-0.43	Ti、Al	Balloon-borne
GroundBIRD	161(138/23)	145、220	2.1、1.4	Nb、A1	GroundBIRD
BICEP-Array	＞30000	30/40、95、150 、220/270	10/6.5、3.16、2 、1.36/1.1	Nb、A1	South Pole Telescope

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表 3 基于MKID的天文相机

Table 3. Astronomical cameras based on MKID

cameras	pixels	frequency/GHz	wavelength/mm	materials	installation
DemoCam	32	240、350	1.25、0.86	A1、Nb	CSO
MUSIC	2304	150、230、290、350	2、1.3、1.03、0.86	TiN	CSO
NIKA(2009)	72	150	2	A1	IRAM
NIKA(2010)	144	150	2	NbTiN、Al	IRAM
NIKA(2010)	256	220	1.36	NbTiN、Al	IRAM
NIKA2	2280	260	1.15	A1	IRAM
NIKA2	616	150	2	A1	IRAM
MUSCAT	1600	270	1.1	A1	LMT
A-MKID	～1000	350	0.85	NbTiN、Al	APEX
A-MKID	～5000	850	0.35	NbTiN、Al	APEX
MUSICAM	～100	150、225、 288、350	2、1.33、1.04、0.86	A1	ESMT
KISS	316	80-300	3.75-1	Ti、Al	QUIJOTE
CONCERTO	2152	130-310	2.3-0.97	Al	APEX
Prime-Cam	60000	220、280、350、410	1.36、1.07、0.86、0.73	TiN、Al	CCAT-prim
	21000	850	0.353
	31000	250、360	1.2、0.833
MISTRAL	415	77-103	3.896-2.913	Ti、Al	SRT

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