标题： QUIJOTE科学结果 -- VI。 QUIJOTE看到的雾霾 显示英文标题

标题： QUIJOTE scientific results -- VI. The Haze as seen by QUIJOTE

摘要： 雾霾是围绕银河系中心的微波强度辐射过量。 它在空间上与$\gamma$射线费米气泡以及S-PASS射电偏振喷流相关，表明可能存在共同的来源。 用于解释雾霾起源的模型，包括银河系中心的能量事件和银河晕中的暗物质衰变，尚未提供明确的物理解释。 在本文中，我们对雾霾进行了重新分析，包括来自Q-U-I JOint TEnerife（QUIJOTE）实验的多频段仪器（MFI）在11和13 GHz的新观测数据。 我们分析了雾霾的强度和偏振，表征了其光谱。 我们检测到归因于雾霾的弥散强度信号的过量。 在频率11$\,\leq\nu\leq\,$70 GHz处的光谱为幂律，光谱指数为$\beta^{\rm H}=-2.79\pm0.08$，这比同一区域的银河系同步辐射更平坦（$\beta^{\rm S}=-2.98\pm0.04$），但比之前研究得到的光谱更陡峭（$\beta^{\rm H}\sim-2.5$在23$\,\leq\,\nu\leq\,$70 GHz处）。 我们还在雾霾区域的QUIJOTE-MFI图中观察到偏振信号的过量。 这是对偏振雾霾的首次探测提示，或是该区域同步辐射光谱曲率的结果。 最后，我们证明与银河系中心活动相关的极化结构的频谱在低频时较陡($\beta \sim -3.2$在 2.3 $\leq\nu\leq$ 23 GHz)，并在 11 GHz 以上变得较平。 显示英文摘要

摘要： The Haze is an excess of microwave intensity emission surrounding the Galactic centre. It is spatially correlated with the $\gamma$-ray Fermi bubbles, and with the S-PASS radio polarization plumes, suggesting a possible common provenance. The models proposed to explain the origin of the Haze, including energetic events at the Galactic centre and dark matter decay in the Galactic halo, do not yet provide a clear physical interpretation. In this paper we present a re-analysis of the Haze including new observations from the Multi-Frequency Instrument (MFI) of the Q-U-I JOint TEnerife (QUIJOTE) experiment, at 11 and 13 GHz. We analyze the Haze in intensity and polarization, characterizing its spectrum. We detect an excess of diffuse intensity signal ascribed to the Haze. The spectrum at frequencies 11$\,\leq\nu\leq\,$70 GHz is a power-law with spectral index $\beta^{\rm H}=-2.79\pm0.08$, which is flatter than the Galactic synchrotron in the same region ($\beta^{\rm S}=-2.98\pm0.04$), but steeper than that obtained from previous works ($\beta^{\rm H}\sim-2.5$ at 23$\,\leq\,\nu\leq\,$70 GHz). We also observe an excess of polarized signal in the QUIJOTE-MFI maps in the Haze area. This is a first hint detection of polarized Haze, or a consequence of curvature of the synchrotron spectrum in that area. Finally, we show that the spectrum of polarized structures associated with Galactic centre activity is steep at low frequencies ($\beta \sim -3.2$ at 2.3 $\leq\nu\leq$ 23 GHz), and becomes flatter above 11 GHz.