论文标题
是由于暗能量还是暗物质引起的宇宙双折射？层析成像方法
Is cosmic birefringence due to dark energy or dark matter? A tomographic approach
论文作者
论文摘要
伪内的“ Axionlike”字段（$ ϕ $）可以解释在宇宙微波背景（CMB）极化数据的$ EB $功率谱中观察到的3σ$ cosmic Birefringence。 $ ϕ $是暗能量还是暗物质？断层扫描方法可以回答这个问题。当今宇宙加速膨胀的有效质量必须小于$ M_DAS \ simeq 10^{ - 33} $ ev。如果$ M_DA \ gtrsim 10^{ - 32} $ eV，$ ϕ $开始在电离时代开始发展，我们应该从低（$ l \ lyssim 10 $）和高倍数的$ eb $ power Spectrum（$ eb $ power Spectrum）观察到不同量的双重折磨。这样的观察结果需要全天候的卫星任务，将排除$ ϕ $是黑暗能源。如果$ M_DA \ gtrsim 10^{ - 28} $ eV，则$ ϕ $在重组时期开始振荡，在高倍数的$ EB $功率谱中留下了独特的签名，可以通过基于地面的CMB观察来精确地测量。我们的层析成像方法依赖于$ eb $ $ $功率谱的形状，并且对极化角度的错误校准不太敏感。
A pseudoscalar "axionlike" field, $ϕ$, may explain the $3σ$ hint of cosmic birefringence observed in the $EB$ power spectrum of the cosmic microwave background (CMB) polarization data. Is $ϕ$ dark energy or dark matter? A tomographic approach can answer this question. The effective mass of dark energy field responsible for the accelerated expansion of the Universe today must be smaller than $m_ϕ\simeq 10^{-33}$ eV. If $m_ϕ\gtrsim 10^{-32}$ eV, $ϕ$ starts evolving before the epoch of reionization and we should observe different amounts of birefringence from the $EB$ power spectrum at low ($l\lesssim 10$) and high multipoles. Such an observation, which requires a full-sky satellite mission, would rule out $ϕ$ being dark energy. If $m_ϕ\gtrsim 10^{-28}$ eV, $ϕ$ starts oscillating during the epoch of recombination, leaving a distinct signature in the $EB$ power spectrum at high multipoles, which can be measured precisely by ground-based CMB observations. Our tomographic approach relies on the shape of the $EB$ power spectrum and is less sensitive to miscalibration of polarization angles.
