A Multi-Frequency Bolometer Array for Sunyaev-Zel'dovich Astronomy at the Caltech Submillimeter Observatory

摘要 9503226 LANGE，Andrew E. 宇宙微波背景辐射（CMB）为可观测宇宙提供了极其均匀的背景光。通过宇宙微波背景辐射光子与引力束缚在星系团中的热电离等离子体的光子-电子（康普顿）散射，一种被称为Sunyaev-Zel'dovich（SZ）效应的扭曲改变了宇宙微波背景辐射的光谱。团簇内介质中电子的热速度和体速度产生不同的光谱畸变，这些畸变可以通过在100至300 GHz范围内的多频观测来彼此区分。这两个组件的分离允许直接确定的特殊速度的集群相对于准惯性CMB静止框架。具有红移的SZ效应的表面亮度的不变性允许这种技术被扩展到仅由丰富的团簇的存在所限制的红移。此外，结合测量的X射线表面亮度的集群的集群内介质的热分量的测量产生一个非常基本的哈勃常数，Ho值。 PI将构建一个新的多频阵列（SuZIE II），该阵列采用频率相关性和增加的像素数量，以大大提高观测对SZ效应和角分尺度上CMB各向异性的灵敏度。SuZIE II将测量许多高红移星系团的特殊速度场，高精度地测量CMB的弧分尺度各向异性，并根据大量精心挑选的星系团样本确定Ho值。 ***

ABSTRACT 9503226 LANGE, Andrew E. The Cosmic Microwave Background (CMB) radiation provides an extremely uniform back light to the observable universe. Through photon-electron (Compton) scattering of the CMB photons with the hot, ionized plasma that is gravitationally bound in clusters of galaxies a distortion known as the Sunyaev-Zel'dovich (SZ) effect alters the spectrum of the CMB when viewed through a cluster. The thermal and bulk velocities of the electrons in the intra-cluster medium produce distinct spectral distortions that can be distinguished from one another by multifrequency observations in the 100 to 300 GHz range. Separation of these two components allows the direct determination of the peculiar velocity of the cluster relative to the quasi-inertial CMB rest frame. The invariance of the surface brightness of the SZ effect with red shift allows this technique to be extended to red shifts limited only by the existence of rich clusters. Also, measurements of the thermal component of the intra-cluster medium combined with measurements of the X-ray surface brightness of the cluster yields a value of the very fundamental Hubble constant, Ho. The PI will construct a new, multi-frequency array (SuZIE II) which employs frequency correlation and an increased number of pixels to greatly increase the sensitivity of observations to the SZ effect and to CMB anisotropy on arcminute scales. SuZIE II will measure the peculiar velocity field of many high red shift clusters, measure the arcminute scale anisotropy of the CMB with high precision, and determine a value for Ho based on a large and carefully selected sample of clusters. ***