用CORE探索宇宙起源：宇宙微波背景图中的河外源
Exploring Cosmic Origins with CORE: Extragalactic sources in Cosmic Microwave Background maps
摘要：
我们讨论了下一代星载宇宙微波背景（CMB）实验研究河外源的潜力。我们的分析特别关系到未来空间项目CORE的定义，该项目是为了响应欧空局关于作为普朗克卫星后继者的中型任务机会的呼吁而提交的。即使有效的望远镜尺寸将比普朗克的小一些，CORE在其最高频率处将具有相当好的角分辨率，因为与普朗克相反，它在所有频率处都是衍射限制的。改进的分辨率意味着源混淆的显著减少，即显著更弱的检测限。特别是，CORE将探测到分布在整个天空中的数千个强透镜高z星系。这些星系的极端亮度将使人们有可能通过后续观测以非常详细的方式研究它们。此外，CORE的分辨率与高z星系原星团的典型大小相匹配，比普朗克分辨率好得多，从而导致更高的探测效率;这些物体将被捕获在其他波段的调查所无法达到的进化阶段。此外，CORE将提供关于维里化星系群和星系团中恒星形成演化的独特信息，直至最高可能的红移。最后，由于其非常高的灵敏度，CORE将探测到数千个射电源的偏振发射，并首次探测到尘埃星系的偏振发射，分别为毫米和亚毫米波长。
英文摘要：
We discuss the potential of a next generation space-borne Cosmic Microwave Background (CMB) experiment for studies of extragalactic sources. Our analysis has particular bearing on the definition of the future space project, CORE, that has been submitted in response to ESA's call for a Medium-size mission opportunity as the successor of the Planck satellite. Even though the effective telescope size will be somewhat smaller than that of Planck, CORE will have a considerably better angular resolution at its highest frequencies, since, in contrast with Planck, it will be diffraction limited at all frequencies. The improved resolution implies a considerable decrease of the source confusion, i.e. substantially fainter detection limits. In particular, CORE will detect thousands of strongly lensed high-z galaxies distributed over the full sky. The extreme brightness of these galaxies will make it possible to study them, via follow-up observations, in extraordinary detail. Also, the CORE resolution matches the typical sizes of high-z galaxy proto-clusters much better than the Planck resolution, resulting in a much higher detection efficiency; these objects will be caught in an evolutionary phase beyond the reach of surveys in other wavebands. Furthermore, CORE will provide unique information on the evolution of the star formation in virialized groups and clusters of galaxies up to the highest possible redshifts. Finally, thanks to its very high sensitivity, CORE will detect the polarized emission of thousands of radio sources and, for the first time, of dusty galaxies, at mm and sub-mm wavelengths, respectively.
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