NIKA: A millimeter-wave kinetic inductance camera
NIKA: A millimeter-wave kinetic inductance camera
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NIKA：毫米波动感电感相机
DOI：
10.1051/0004-6361/201014727
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发表时间：
2010
影响因子：
6.5
通讯作者：
K. Schuster
中科院分区：
文献类型：
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作者：
A. Monfardini;L. Swenson;A. Bideaud;F. Désert;S. Yates;A. Benoit;A. Baryshev;J. Baselmans;S. Doyle;B. Klein;M. Roesch;C. Tucker;P. Ade;M. Calvo;P. Camus;C. Giordano;R. Guesten;C. Hoffmann;S. Leclercq;P. Mauskopf;K. Schuster
上下文。当前一代毫米波长探测器受到复杂低温读出电子设备施加的定标限制。这些仪器通常使用远低于100的多路复用率。要实现大于一千的多路复用率，必须研究本质上结合了强多路复用的技术。一种可能的解决方案是动态电感检测器(KID)。为了评估这一新兴技术的潜力，建造了一台针对2 mm大气窗口进行优化的原型仪器。它被称为Neel IRAM KID阵列(NICA)，最近在西班牙皮科·维莱塔的毫米射电天文研究所(IRAM)30米望远镜上进行了测试。目标。主要的研究目标有四个：确定开发基于KIDES的巨型阵列仪器的可行性、测量当前的现场像素灵敏度、确定限制噪声源以及对校准和与科学有关的天文学源进行成像。方法：研究方法。探测器由电磁耦合到传输线上的高质量超导谐振器阵列组成，工作在∼100MK。谐振器的阻抗受到入射辐射的调制；两个独立的阵列被测试以评估两种独特的光耦合策略的效率。第一个阵列由集总元件动感探测器(LEKID)组成，它们具有全平面设计，形状适当，可以直接吸收。第二个阵列由天线耦合的KILD组成，每个蓝宝石微透镜与平面缝隙天线对准。这两个探测器都使用了一条传输线和合适的室温数字电子设备来进行连续读出。结果。Nika在2009年10月成功进行了测试，表现符合预期。这项测量导致了许多来源的成像，包括行星、类星体和星系。给出了火星、射电恒星MWC349、类星体3C345和星系M87的图像。根据这些结果，计算出光学净功率约为1×10−15W/Hz1/2。通过改进探测器材料和减少降低性能的杂散辐射，预计10倍的改进是很容易实现的。
Context. Current generation millimeter wavelength detectors suffer from scaling limits imposed by complex cryogenic readout electronics. These instruments typically employ multiplexing ratios well below a hundred. To achieve multiplexing ratios greater than a thousand, it is imperative to investigate technologies that intrinsically incorporate strong multiplexing. One possible solution is the kinetic inductance detector (KID). To assess the potential of this nascent technology, a prototype instrument optimized for the 2 mm atmospheric window was constructed. Known as the Neel IRAM KID Array (NIKA), it has recently been tested at the Institute for Millimetric Radio Astronomy (IRAM) 30-m telescope at Pico Veleta, Spain. Aims. There were four principle research objectives: to determine the practicality of developing a giant array instrument based on KIDs, to measure current in-situ pixel sensitivities, to identify limiting noise sources, and to image both calibration and scientificallyrelevant astronomical sources. Methods. The detectors consisted of arrays of high-quality superconducting resonators electromagnetically coupled to a transmission line and operated at ∼100 mK. The impedance of the resonators was modulated by incident radiation; two separate arrays were tested to evaluate the efficiency of two unique optical-coupling strategies. The first array consisted of lumped element kinetic inductance detectors (LEKIDs), which have a fully planar design properly shaped to enable direct absorbtion. The second array consisted of antenna-coupled KIDs with individual sapphire microlenses aligned with planar slot antennas. Both detectors utilized a single transmission line along with suitable room-temperature digital electronics for continuous readout. Results. NIKA was successfully tested in October 2009, performing in line with expectations. The measurement resulted in the imaging of a number of sources, including planets, quasars, and galaxies. The images for Mars, radio star MWC349, quasar 3C345, and galaxy M 87 are presented. From these results, the optical NEP was calculated to be around 1×10 −15 W/Hz 1/2 . A factor of 10 improvement is expected to be readily feasible by improvements in the detector materials and reduction of performance-degrading spurious radiation.