Observational Studies of Cosmie Micro Wave Background Gnisotropy

为了测量宇宙微波背景的各向异性和偏振，我们在东北大学天文研究所设立了一个新的实验室，用于开发毫米-亚毫米波天文仪器。讨论了Martin & Puplett型傅里叶变换光谱仪在孔径综合中的应用。设计并研制了一台新颖的互相关型马丁-普普莱特傅里叶变换光谱仪。该仪器的设计是紧凑的，因为我们可以，这是最小化的光路长度和尺寸等，该仪器的开发是在1999年预算年度内完成。2000年预算年度，柴田和服部在实验室中使用该仪器进行了基础实验。在进行实验时，我们从理论上证明了用这种仪器可以测量宽波段毫米-亚毫米波的四个斯托克斯参量在天空上的角分布。在实验室实验中，我们已经证明我们的仪器实际上能够测量作为干涉信号的4个Stokes参数。毫米-亚毫米波探测器的研制主要是由Matsuo领导的日本国家天文台先进技术中心完成的。研制了用于天文观测的测辐射热计探测器，并进行了性能验证。2000年预算年度完成了亮源测辐射热计探测器的研制和性能验证。用于微弱源的高灵敏度测辐射热计探测器的开发始于2000年。并对SIS直接亚毫米波探测器进行了研制。我们第一次在实验上表明，SIS直接探测器实现了极低的噪声电平NEP=10^<-18>W/mW<Hz>。设计了一种用于亚毫米波与SIS直接探测器有效耦合的专用天线。为SIS直接探测器阵列的研制进行了初步设计。

We have set up a new laboratory for development of mm-submm wave astronomical instruments aiming to measure Cosmic Microwave Background anisotropy and polarization in astronomical institute at Tohoku University. The application of the Martin ＆ Puplett type Fourier transform spectrometer to aperture synthesis was considered. An original mutual correlation type Martin ＆ Puplett Fourier transform spectrometer was designed and developed. The instrument was designed to be compact as possible as we can, that is minimizing the light path length and the size etc. The development of this instrument was completed within 1999 budget year. Shibata and Hattori performed fundamental experiments using this instrument in the laboratory during 2000 budget year. While we were performing the experiments, we have theoretically shown that the angular distribution of the 4 Stokes parameters on the sky can be measured for wide band mm-submm waves with this instrument. In the laboratory experiments, we have shown that our instrument is actually able to measure the 4 Stokes parameters as interference signals.The developments of the mm-submm wave detectors were performed mainly in Advanced Technology Center at National Astronomical Observatory of Japan lead by Matsuo. Bolometer detectors for astronomical observations were developed and performance verifications were done. The development and performance verifications of the bolometer detector for bright sources were completed with 2000 budget year. The development of the high sensitivity bolometer detector for faint sources was started at 2000. The developments of the SIS direct submm detector was also performed. We have at the first time shown experimentally that the SIS direct detector achieves extremely low noise level of NEP=10^<-18>W/√<Hz>. The special antenna for efficient coupling between the submm waves and the SIS direct detector was designed. The fundamental designs for development of array of SIS direct detectors were also done.