发表机构
Shanghai University; Asia Pacific Center for Theoretical Physics; Max Planck Institute for Astrophysics; Ludwig-Maximilians-Universitat München; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, The University of Tokyo（上海大学; 亚太理论物理中心; 马克斯·普朗克天体物理学研究所; 慕尼黑路德维希-马克西米利安大学; 东京大学宇宙物质与引力起源研究前沿机构（ Kavli 宇宙物理数学研究所））
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过计算EB功率谱，区分宇宙双折射的不同起源（暗能量、暗物质、中微子不对称性），发现暗能量无低多极抑制，可用于区分，并利用重组期演化特征区分中微子与轴子暗物质。
AI 中文摘要
宇宙双折射，即来自宇宙学距离光源的光子线性偏振平面的各向同性旋转，可由不同的宇称破坏机制产生。虽然单个偏振源的总旋转角携带的关于其物理起源的信息很少，但不同红移$z$处的源可用于区分不同的起源。在大角尺度和小角尺度上测量的宇宙微波背景的$E$模和$B$模偏振场的宇称敏感相关性，分别探测$z\simeq 10$和$1100$处的源。因此，$EB$功率谱的详细形状对双折射源的红移演化敏感。在本文中，我们计算了由中微子不对称流引起的$EB$功率谱，并使用共同的Chern--Simons框架将其与轴子暗能量和暗物质进行比较。我们发现，由中微子不对称性引起的$EB$功率谱在低多极矩$\ell\lesssim 20$处被抑制，类似于暗物质的情况。这可以与暗能量情况清楚地区分开，暗能量情况没有这种抑制。包括\textit{LiteBIRD}在内的大尺度偏振测量，因此可以区分晚期暗能量双折射与由轴子暗物质或中微子不对称性在更高红移处产生的双折射。我们还发现，重组期间中微子密度的演化改变了高多极矩处$EB$功率谱的形状。这一特征可用于区分中微子和轴子暗物质的解释，使用诸如Simons Observatory之类的地面实验。
英文摘要
Cosmic birefringence, the isotropic rotation of the plane of linear polarization of photons from sources at cosmological distances, can be generated by different parity-violating mechanisms. While the net rotation angle of a single polarized source carries little information about its physical origin, sources at various redshifts $z$ can be used to distinguish between different origins. Parity-sensitive correlations of the $E$- and $B$-mode polarization fields of the cosmic microwave background measured on large and small angular scales probe sources at $z\simeq 10$ and $1100$, respectively. Thus, the detailed shape of the $EB$ power spectrum is sensitive to the redshift evolution of the birefringence source. In this paper, we calculate the $EB$ power spectrum due to a neutrino-asymmetry current, and compare it to axion dark energy and dark matter using a common Chern--Simons framework. We find that the $EB$ power spectrum due to a neutrino asymmetry is suppressed at low multipoles, $\ell\lesssim 20$, similar to the dark matter case. This can be clearly distinguished from the dark energy case, which has no such suppression. Large-scale polarization measurements, including \textit{LiteBIRD}, can therefore distinguish late-time dark energy birefringence from that generated at higher redshifts by axion dark matter or neutrino asymmetry. We also find that the evolution of the neutrino density during recombination alters the shape of the $EB$ power spectrum at high multipoles. This signature can be used to distinguish between the neutrino and axion dark matter interpretations, using ground-based experiments such as the Simons Observatory.
