极化WMAP发射揭示的北费米泡的磁亚结构
Magnetic substructure in the northern Fermi Bubble revealed by polarized WMAP emission
摘要：
我们报告了巨大的，极化的微波结构出现在银河系中心附近的银河系平面和一些GeV的伽马射线特征，包括最近发现的北部费米泡的东部边缘之间的对应关系。极化微波特征也对应于全天空408 MHz总强度数据中看到的结构，包括银河系中心的支线。在23 GHz的极化数据所揭示的磁场结构表明，无论是与气泡边缘重合的发射，还是银河系中心的毛刺，都不太可能是本地ISM的特征。根据观测到的形态对应，类似的推断光谱，和类似的能量的所有来源，我们建议银河系中心的支线和北部费米泡之间的直接连接。
英文摘要：
We report a correspondence between giant, polarized microwave structures emerging north from the Galactic plane near the Galactic center and a number of GeV gamma-ray features, including the eastern edge of the recently-discovered northern Fermi Bubble. The polarized microwave features also correspond to structures seen in the all-sky 408 MHz total intensity data, including the Galactic center spur. The magnetic field structure revealed by the polarization data at 23 GHz suggests that neither the emission coincident with the Bubble edge nor the Galactic center spur are likely to be features of the local ISM. On the basis of the observed morphological correspondences, similar inferred spectra, and the similar energetics of all sources, we suggest a direct connection between the Galactic center spur and the northern Fermi Bubble.
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