卫星CMB实验的带通失配误差I：寄生信号的估计
Bandpass mismatch error for satellite CMB experiments I: Estimating the spurious signal
摘要：
未来的宇宙微波背景（CMB）卫星任务旨在使用$B$模式偏振来测量张量标量比$r$，灵敏度约为$10^{-3}$。实现这一目标不仅需要足够的探测器阵列灵敏度，而且需要对CMB偏振测量固有的所有系统误差进行前所未有的控制。由于偏振测量值来自不同时间和不同传感器的观测值之间的差异，因此检测器响应失配会引入从强度到偏振的泄漏，从而导致伪$B$模式信号。因为预期的原始$B$模式偏振信号被已知的非偏振强度信号所矮化，所以这种泄漏可能实质上对用于测量$r.$的最终误差预算有贡献。使用模拟，我们估计由不同检测器之间的带通失配引起的伪$B$模式信号的幅度和角谱。这里假设检测器被校准，例如使用CMB偶极子，使得它们对原始CMB信号的灵敏度已经完美匹配。因此，在探测器之间的频带通形状的不匹配引入银河系发射组件的相对校准的差异。我们模拟使用一系列的扫描模式正在考虑未来的卫星任务。我们发现，假的贡献$r$从大角度尺度上的再电离凸块（$\ell < 10$）是$\approx 10^{-3}$假设大型探测器阵列和20%的天空掩盖。我们展示了泄漏的幅度如何取决于从扫描图案产生的每像素的角度覆盖。
英文摘要：
Future Cosmic Microwave Background (CMB) satellite missions aim to use the $B$ mode polarization to measure the tensor-to-scalar ratio $r$ with a sensitivity of about $10^{-3}$. Achieving this goal will not only require sufficient detector array sensitivity but also unprecedented control of all systematic errors inherent to CMB polarization measurements. Since polarization measurements derive from differences between observations at different times and from different sensors, detector response mismatches introduce leakages from intensity to polarization and thus lead to a spurious $B$ mode signal. Because the expected primordial $B$ mode polarization signal is dwarfed by the known unpolarized intensity signal, such leakages could contribute substantially to the final error budget for measuring $r.$ Using simulations we estimate the magnitude and angular spectrum of the spurious $B$ mode signal resulting from bandpass mismatch between different detectors. It is assumed here that the detectors are calibrated, for example using the CMB dipole, so that their sensitivity to the primordial CMB signal has been perfectly matched. Consequently the mismatch in the frequency bandpass shape between detectors introduces difference in the relative calibration of galactic emission components. We simulate using a range of scanning patterns being considered for future satellite missions. We find that the spurious contribution to $r$ from reionization bump on large angular scales ($\ell < 10$) is $\approx 10^{-3}$ assuming large detector arrays and 20 percent of the sky masked. We show how the amplitude of the leakage depends on the angular coverage per pixels that results from the scan pattern.
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。
