优化宇宙远红外背景的未来实验：主成分方法
Optimizing future experiments of cosmic far-infrared background: a principal component approach
摘要：
利用宇宙远红外背景辐射（CFIRB）的各向异性，研究了尘埃星系的恒星形成率（SFR）与暗物质晕质量和红移的关系。我们将探讨未来的CFIRB实验如何能够最佳地改善SFR的约束超出目前的测量普朗克。我们引入了一个独立的模型，分段参数化的SFR作为晕质量和红移的函数，我们计算的Fisher矩阵和这些参数的主成分估计未来实验的SFR约束。我们调查如何SFR的约束取决于角分辨率，频带的数量和范围，调查范围，和仪器的灵敏度。我们发现，角分辨率和仪器灵敏度起关键作用。将角分辨率从20角分提高到4角分可以将SFR约束提高1.5 - 2.5个数量级。以普朗克的角分辨率，灵敏度提高10倍或100倍，可以使SFR约束提高一到两个数量级，频带数加倍也可以使SFR约束提高一个数量级。我们发现，像宇宙起源探测器（CORE）的调查设计是非常接近的最佳设计，以改善SFR约束在所有红移，而调查设计，如LiteBIRD和CMB-S4可以显着改善SFR约束在z>3。
英文摘要：
The anisotropies of cosmic far-infrared background (CFIRB) probe the star formation rate (SFR) of dusty star-forming galaxies as a function of dark matter halo mass and redshift. We explore how future CFIRB experiments can optimally improve the SFR constraints beyond the current measurements of Planck. We introduce a model-independent, piecewise parametrization for SFR as a function of halo mass and redshift, and we calculate the Fisher matrix and principal components of these parameters to estimate the SFR constraints of future experiments. We investigate how the SFR constraints depend on angular resolution, number and range of frequency bands, survey coverage, and instrumental sensitivity. We find that the angular resolution and the instrumental sensitivity play the key roles. Improving the angular resolution from 20 to 4 arcmin can improve the SFR constraints by 1.5 - 2.5 orders of magnitude. With the angular resolution of Planck, improving the sensitivity by 10 or 100 times can improve the SFR constraints by one or two orders of magnitude, and doubling the number of frequency bands can also improve the SFR constraints by an order of magnitude. We find that survey designs like the Cosmic Origins Explorer (CORE) are very close to the optimal design for improving the SFR constraints at all redshifts, while survey designs like LiteBIRD and CMB-S4 can significantly improve the SFR constraints at z>3.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
