来自极化苏尼亚耶夫-泽尔多维奇效应的对远程四极场的限制
Constraints on the remote quadrupole field from the polarized Sunyaev Zel'dovich effect
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中文总结 AI 辅助
研究通过CMB-CMB-星系三谱评估极化苏尼亚耶夫-泽尔多维奇效应，利用普朗克和ACT的CMB数据等。虽未显著检测到该效应，但给出相关限制，预测未来测量可收紧限制，有助于确认低CMB四极和再电离光学深度。
中文摘要 AI 辅助
极化苏尼亚耶夫-泽尔多维奇（pSZ）效应是由非线性结构中自由电子的汤姆逊散射引起的宇宙微波背景（CMB）极化各向异性。pSZ信号由追踪宇宙网的电离气体分布和自由电子位置处的CMB四极——远程四极场决定。测量pSZ效应可对再电离的光学深度进行一致性检验，并揭示大规模CMB温度各向异性的异常性质，如观测到的低CMB温度四极。本文表明，CMB-CMB-星系三谱总结了几种现有的pSZ统计量，且在可观测宇宙中，检测pSZ的理想星系样本处于z~1-2。我们使用普朗克和ACT的CMB数据、unWISE星系红移目录中的星系密度以及普朗克宇宙红外背景（CIB）地图来评估三谱。我们未对pSZ效应进行具有统计显著性的检测，这与该数据组合预期的O(1)信噪比一致。测量的pSZ三谱幅度对与大规模结构相关的光学深度偏差（pSZ信号幅度）、再电离光学深度和张量与标量比r给出了限制。我们预测未来测量可将这些量的限制收紧约3倍，足以独立确认低CMB四极和再电离光学深度。
英文摘要
The polarized Sunyaev Zel'dovich (pSZ) effect is a cosmic microwave background (CMB) polarization anisotropy induced by Thomson scattering from free-electrons in non-linear structure. The pSZ signal is determined by the distribution of ionized gas tracing the cosmic web and the CMB quadrupole at the location of free-electrons - the remote quadrupole field. Measuring the pSZ effect provides a consistency check of the optical depth to reionization and sheds light on the anomalous nature of the large-scale CMB temperature anisotropies, such as the low observed CMB temperature quadrupole. In this paper, we demonstrate that a CMB-CMB-galaxy bispectrum summarizes several existing pSZ statistics, and that in our observable Universe the ideal galaxy sample to detect pSZ is at $z \sim 1-2$. We evaluate the bispectrum using CMB data from Planck and ACT with galaxy density from the unWISE galaxy redshift catalog as well as Planck cosmic infrared background (CIB) maps. We do not make a statistically significant detection of the pSZ effect, which is consistent with the expected O$(1)$ signal-to-noise from this data combination. The measured amplitude of the pSZ bispectrum provides constraints on the optical depth bias associated with large-scale structure (the amplitude of the pSZ signal) of $b_q=1.02 \pm 2.64$, the optical depth to reionization of $τ_{\rm rei} = -0.01 \pm 0.14$, and the tensor-to-scalar ratio $r$ of $σ_r \sim 150$ ($n_t = 0$) or $σ_r \sim 3$ ($n_t = -1$). We forecast that future measurements could tighten the constraints on these quantities by roughly a factor of 3, which is sufficient to provide independent confirmation of the low CMB quadrupole and the optical depth to reionization.
