BeyondPlanck XVI. 利用Planck LFI和WMAP对大尺度极化异常微波辐射的限制
BeyondPlanck XVI. Limits on Large-Scale Polarized Anomalous Microwave Emission from Planck LFI and WMAP
AI总结：
本研究在贝叶斯CMB框架下利用Planck LFI和WMAP数据约束大尺度极化AME，发现AME极化分数约束高度依赖同步辐射谱指数先验，并指出结合C-BASS和QUIJOTE等低频实验数据对进一步改善限制至关重要。
摘要：
我们在贝叶斯CMB分析框架内，利用Planck LFI和WMAP极化数据，约束了大角尺度上的极化异常微波辐射（AME）水平。我们用幂律谱能量分布对同步辐射进行建模，并通过与Planck HFI 353 GHz数据的线性回归来对AME和热尘埃辐射之和进行建模。这种基于模板的尘埃辐射模型使我们能够在对其频率依赖性做出最小假设的情况下，约束极化AME的水平。我们忽略了宇宙微波背景涨落，但通过模拟表明这些涨落对结果影响较小。我们发现，由此得到的AME极化分数置信限对极化同步辐射谱指数先验敏感，对于比$β_{\mathrm{s}} = -3.1\pm0.1$更陡的先验，我们得到上限为$p_{\mathrm{AME}}^{\rm max}\lesssim 0.6\\,\\%$（$95\\,\\%$置信度）。相反，对于$β_{\mathrm{s}}=-3.0\pm0.1$，我们发现名义探测值为$p_{\mathrm{AME}}=2.5\pm1.0\\,\\%$（$95\\,\\%$置信度）。因此，这些数据不足以同时稳健地约束极化同步辐射和AME，我们的主要结果是将AME极化分数明确表示为$β_\mathrm{s}$的函数约束。将当前的Planck和WMAP观测与C-BASS和QUIJOTE等高灵敏度低频实验的测量相结合，对于进一步改善这些限制至关重要。
英文摘要：
We constrain the level of polarized anomalous microwave emission (AME) on large angular scales using $\textit{Planck}$ LFI and $\textit{WMAP}$ polarization data within a Bayesian CMB analysis framework. We model synchrotron emission with a power-law spectral energy distribution, and the sum of AME and thermal dust emission through linear regression with the $\textit{Planck}$ HFI 353 GHz data. This template-based dust emission model allows us to constrain the level of polarized AME while making minimal assumptions on its frequency dependence. We neglect cosmic microwave background fluctuations, but show through simulations that these have a minor impact on the results. We find that the resulting AME polarization fraction confidence limit is sensitive to the polarized synchrotron spectral index prior, and for priors steeper than $β_{\mathrm{s}} = -3.1\pm0.1$ we find an upper limit of $p_{\mathrm{AME}}^{\rm max}\lesssim 0.6\,\%$ ($95\,\%$ confidence). In contrast, for $β_{\mathrm{s}}=-3.0\pm0.1$, we find a nominal detection of $p_{\mathrm{AME}}=2.5\pm1.0\,\%$ ($95\,\%$ confidence). These data are thus not strong enough to simultaneously and robustly constrain both polarized synchrotron emission and AME, and our main result is therefore a constraint on the AME polarization fraction explicitly as a function of $β_\mathrm{s}$. Combining the current $\textit{Planck}$ and $\textit{WMAP}$ observations with measurements from high-sensitivity low-frequency experiments such as C-BASS and QUIJOTE will be critical to improve these limits further.
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