PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper
PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper
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DOI：
10.1088/1475-7516/2014/02/006
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发表时间：
2013-10
影响因子：
6.4
通讯作者：
Prism Collaboration Philippe Andr'e;C. Baccigalupi;A. Banday;D. Barbosa;B. Barreiro;J. Bartlett;N. Bart
中科院分区：
文献类型：
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作者：
Prism Collaboration Philippe Andr'e;C. Baccigalupi;A. Banday;D. Barbosa;B. Barreiro;J. Bartlett;N. Bart
PRISM（偏振辐射成像和光谱任务）于 2013 年 5 月向欧空局提议，作为一项大型任务，在欧空局宇宙视觉计划的框架内调查一系列重要的科学问题，这些问题需要对从毫米波到远红外波长范围内的天空发射进行高分辨率、高灵敏度、全天观测。棱镜的主要目标是探索遥远的宇宙，探索从很早时期到现在的宇宙历史，以及整个哈勃体积的结构、物质分布和速度流。 PRISM 将在强度和偏振方面对大量频段的全天空进行测量，并将测量天空发射的绝对频谱，其效果比 COBE FIRAS 好三个数量级以上。获得的数据将使我们能够精确测量观测频率范围内天空发射的所有分量的绝对天空亮度和偏振，将原始和河外分量与银河和黄道光发射完全分开。本扩展白皮书的目的是更详细地概述 PRISM 将实现的新科学的亮点，其中包括：(1) 使用 Sunyaev-Zeldovich (SZ) 效应进行终极星系团勘测，检测到大约 106 个延伸到大红移的星系团，包括最亮星系团的气体温度特征（通过对经典 SZ 模板的相对论校正）以及 使用动态 SZ 效应进行的奇特速度测量，包括我们整个哈勃体积； (2) 尘埃星系的性质和演化的详细表征，宇宙中大部分恒星形成都发生在这些星系中，其中最微弱的星团构成了弥漫的 CIB（宇宙红外背景）； (3) 暴胀期间产生的原初重力波和引力透镜的 B 模式特征，以及使用 CMB 偏振对原初非高斯性的最终搜索，与温度各向异性相比，它在小尺度上受前景的污染较少； (4) 从完美的黑体频谱中寻找失真，其中包括一些几乎确定的信号和其他更具推测性但信息量更大的信号； （5）研究磁场在恒星形成中的作用及其与银河系星际介质其他成分的相互作用。这些只是此处介绍的一些要点以及对拟议文书的描述。
PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The data obtained will allow us to precisely measure the absolute sky brightness and polarization of all the components of the sky emission in the observed frequency range, separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM, which include: (1) the ultimate galaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 106 clusters extending to large redshift, including a characterization of the gas temperature of the brightest ones (through the relativistic corrections to the classic SZ template) as well as a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubble volume; (2) a detailed characterization of the properties and evolution of dusty galaxies, where the most of the star formation in the universe took place, the faintest population of which constitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes from primordial gravity waves generated during inflation and from gravitational lensing, as well as the ultimate search for primordial non-Gaussianity using CMB polarization, which is less contaminated by foregrounds on small scales than the temperature anisotropies; (4) a search for distortions from a perfect blackbody spectrum, which include some nearly certain signals and others that are more speculative but more informative; and (5) a study of the role of the magnetic field in star formation and its interaction with other components of the interstellar medium of our Galaxy. These are but a few of the highlights presented here along with a description of the proposed instrument.