The POLARBEAR Cosmic Microwave Background Polarization Experiment and Anti-Reflection Coatings for Millimeter Wave Observations
The POLARBEAR Cosmic Microwave Background Polarization Experiment and Anti-Reflection Coatings for Millimeter Wave Observations
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POLARBEAR宇宙微波背景偏振实验和毫米波观测增透膜
DOI：
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
E. Quealy
中科院分区：
文献类型：
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作者：
E. Quealy
在过去的30年里，新技术迅速地推动了观测宇宙学领域的发展。随着宇宙微波背景（CMB）极化测量技术的发展，这一趋势将继续下去。偏振图的b模分量将限制暴胀的能量尺度和中微子质量的总和。本文介绍了一种能以前所未有的灵敏度测量宇宙微波背景偏振各向异性的\pb仪器。“北极星- 1”目前正在进行观测，未来计划发射升级版“北极星- 2”。该实验的第一个版本，北极星- 1，首次部署了几项新技术。由于它的探测器数量，北极星- 1具有很高的灵敏度。它采用了一个1274探测器过渡边缘传感器（TES）辐射热计阵列。辐射热计与偏振敏感天线的平面阵列耦合。这些天线光刻在与TES探测器相同的衬底上，允许在天线和探测器之间的片上频带定义滤波器。焦平面由七个六边形探测器模块组成。这种模块化方案可以扩展到将来创建更大的焦平面阵列。北极星- 1在150千兆赫附近的单波段观测，这是宇宙微波背景黑体曲线的峰值。透镜天线耦合探测器技术首次应用于polarbear - 1，自然可扩展到具有多同步像素的更大阵列。该宽带技术将具有更高的灵敏度和更好的天文前景污染物去除能力。天线的几何形状可以改变以接收更宽的频率带宽。这个带宽可以用片上的频带定义滤波器分解成多个频带。每个波段将由一个TES探测器读出。一种双频仪器，\ pb2，正在开发中，波段为90 GHz和150 GHz。所有微波背景偏振测量的一个挑战是最小化系统误差。误差的一个来源是接收器内部折射光学的偏振反射。具体来说，天线耦合检测器方案依赖于焦平面上每个像素的高介电小波。本文主要讨论了高曲率透镜表面增透涂层的研究进展。所讨论的AR涂层技术也适用于其他光学元件，如再成像透镜和半波片。单层涂层用于\ phone透镜阵列，两层涂层用于\ pb2。两层涂层方法可以扩展到更宽带宽的AR涂层。
New technology has rapidly advanced the field of observational cosmology over the last 30 years. This trend will continue with the development of technologies to measure the Cosmic Microwave Background (CMB) polarization. The B-mode component of the polarization map will place limits on the energy scale of inflation and the sum of the neutrino masses. This thesis describes the \pb instrument which will measure the CMB polarization anisotropy to unprecedented sensitivity. POLARBEAR-I is currently observing, and an upgraded version, POLARBEAR-II, is planned for the future.The first version of the experiment, POLARBEAR-I, is fielding several new technologies for the first time. POLARBEAR-I has high sensitivity due to its detector count. It employs a 1274 detector Transition-Edge Sensor (TES) bolometer array. The bolometers are coupled to a planar array of polarization sensitive antennas. These antennas are lithographed on the same substrate as the TES detectors, allowing on-chip band defining filters between the antenna and detector. The focal plane is composed of seven hexagonal detector modules. This modular scheme can be extended to create larger focal plane arrays in the future. POLARBEAR-I is observing at a single band near 150 GHz, the peak in the CMB blackbody curve.The lenslet antenna coupled detector technology, fielding for the first time in POLARBEAR-I, is naturally scalable to larger arrays with multi-chroic pixels. This broadband technology will have higher sensitivity and better capability for astronomical foreground contaminant removal. The antenna geometry can be changed to receive a wider frequency bandwidth. This bandwidth can be broken into multiple frequency bands with the on-chip band defining filters. Each band will be read out by one TES detector. A dual band instrument, \pbtwo, is in development with bands at 90 and 150 GHz.One challenge for all CMB polarization measurements is minimization of systematic errors. One source of error is polarized reflections off of the refractive optics inside the receiver. Specifically, the antenna-coupled detector scheme relies on a high dielectric lenslet for each pixel on the focal plane. A large portion of this thesis discusses development of anti-reflection (AR) coatings for the high curvature lenslet surface. The AR coating technologies discussed are also applicable to other optical elements, such as reimaging lenses and half-wave plates. A single layer coating is used on the \pbone lenslet array, and a two layer coating is presented for use in \pbtwo. The two layer coating method can be extended to wider bandwidth AR coatings.
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.