QUIJOTE科学结果——XVIII. 亮银河区域异常微波发射偏振的新约束：$\ ho$蛇夫座、英仙座和W43
QUIJOTE scientific results -- XVIII. New constraints on the polarization of the Anomalous Microwave Emission in bright Galactic regions: $ρ$\,Ophiuchi, Perseus and W43
AI总结：
本研究利用QUIJOTE-MFI及WMAP、Planck数据，通过改进泄漏校正和频率叠加，对蛇夫座ρ、英仙座和W43的异常微波发射偏振分数给出了迄今最严格的上限（<1%）。
摘要：
本研究聚焦于异常微波发射（AME）的研究，这是一种在10至60 GHz频段内的重要辐射机制，其偏振特性尚未被完全理解，因此可能成为未来宇宙微波背景（CMB）偏振观测的潜在污染物。我们利用新的QUIJOTE-MFI 11、13、17和19 GHz巡天图，结合包括WMAP和Planck在内的其他公开辅助数据，研究了三个银河区域：蛇夫座ρ、英仙座和W43的AME偏振特性。\n我们获得了这三个区域在0.4-3000 GHz频率范围内的光谱能量分布（SED），包括强度和偏振两个方面的数据。强度SED可以很好地由自由-自由辐射、热尘埃、AME和CMB各向异性的组合来描述。在偏振方面，我们利用11至353 GHz之间的所有可用数据提取了通量密度。我们实施了一种改进的强度到偏振泄漏校正，这使得首次能够从Planck-LFI数据中获得远低于1%水平的可靠偏振约束。对10-60 GHz范围内的巡天图进行频率叠加，使我们能够降低统计噪声，并提高AME偏振水平的上限。\n我们获得了这三个区域AME偏振分数约为<1%（95%置信水平）的上限。具体而言，在蛇夫座ρ、英仙座和W43中，我们分别得到Pi_AME < 1.1%（在28.4 GHz）、Pi_AME < 1.1%（在22.8 GHz）和Pi_AME < 0.28%（在33 GHz）。在QUIJOTE 17 GHz频段，我们得到蛇夫座ρ的Pi_AME < 5.1%，英仙座的Pi_AME < 3.5%，W43的Pi_AME < 0.85%。我们使用叠加程序得出的最终上限为：蛇夫座ρ的Pi_AME < 0.58%，英仙座的Pi_AME < 1.64%，W43的Pi_AME < 0.31%。总体而言，这些是对这三个恒星形成区域AME偏振分数迄今为止最严格的约束。
英文摘要：
This work focuses on the study of the AME, an important emission mechanism between 10 and 60 GHz whose polarization properties are not yet fully understood, and is therefore a potential contaminant for future CMB polarization observations. We use new QUIJOTE-MFI maps 11, 13, 17 and 19 GHz, together with other public ancillary data including WMAP and Planck, to study the polarization properties of the AME in three Galactic regions: rho-Ophiuchi, Perseus and W43. We have obtained the SEDs for those three regions over the frequency range 0.4-3000 GHz, both in intensity and polarization. The intensity SEDs are well described by a combination of free-free emission, thermal dust, AME and CMB anisotropies. In polarization, we extracted the flux densities using all available data between 11 and 353 GHz. We implemented an improved intensity-to-polarization leakage correction that has allowed for the first time to derive reliable polarization constraints well below the 1% level from Planck-LFI data. A frequency stacking of maps in the range 10-60 GHz has allowed us to reduce the statistical noise and to push the upper limits on the AME polarization level. We have obtained upper limits on the AME polarization fraction of order <1% (95% confidence level) for the three regions. In particular we get Pi_AME < 1.1% (at 28.4 GHz), Pi_AME < 1.1% (at 22.8 GHz) and Pi_AME < 0.28% (at 33 GHz) in rho-Ophiuchi, Perseus and W43 respectively. At the QUIJOTE 17 GHz frequency band, we get Pi_AME< 5.1% for rho-Ophiuchi, Pi_AME< 3.5% for Perseus and Pi_AME< 0.85% for W43. Our final upper limits derived using the stacking procedure are Pi_AME < 0.58% for rho-Ophiuchi, Pi_AME < 1.64% for Perseus and Pi_AME < 0.31% for W43. Altogether, these are the most stringent constraints to date on the AME polarization fraction of these three star-forming regions.
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。
