在北冕座延伸区/eROSITA气泡中发现光学细丝
Discovery of Optical Filaments in the North Polar Spur/eROSITA Bubble
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中文总结 AI 辅助
研究在eROSITA气泡的北冕座延伸区发现光学细丝，通过Δ方差和功率谱分析其特征，对比不同模型所需功率，发现AGN喷流等模型合理，恒星形成驱动风模型不成立。
中文摘要 AI 辅助
我报告了在Hα、[O III]和[S II]波段中发现的光学细丝，它们与144MHz结构重合，与eROSITA气泡的北冕座延伸区（NPS）相关。这些光学发射是在北天天文窄带调查中识别出来的，具有独特的结构，且相对于来自温暖电离介质（WIM）的典型高b外流，[S II]/Hα可能升高。对NPS的Hα进行的Δ方差和功率谱分析显示，滞后L≈0.6°尺度上的细丝更受青睐。光学和144MHz发射强度在NPS的内部区域达到峰值，与周围的银河磁化结构对齐，在eROSITA气泡边缘也有较弱的信号。产生背景扣除后的I_Hα = 1.85±1.04R发射所需的功率为P_req≈5 - 12×10^41 erg s^-1，AGN喷流模型轻松超过该值，AGN热吸积流和恒星形成环模型似乎合理，而恒星形成驱动风模型不成立。
英文摘要
I report the discovery of optical filaments in H$α$, [O III], and [S II], coincident with $144\,\mathrm{MHz}$ structure, associated with the North Polar Spur (NPS) region of the eROSITA bubbles. The optical emission is identified in the Northern Sky Narrowband Survey, and contains distinct structure and potentially elevated $\text{[S II]}/\mathrm{H}α$ relative to typical high-$b$ outflows from the warm ionized medium (WIM). $Δ$-variance and power spectrum analysis of the NPS H$α$ shows a preference for filaments on the scale of lag $L\approx0.6^{\circ}$. The optical and $144\,\mathrm{MHz}$ emission peaks in intensity in an interior region of the NPS, aligned with surrounding Galactic magnetized structures, and also shows fainter signal at the eROSITA bubble edge. The required power to produce the background-subtracted $I_{\mathrm{H}α}=1.85\pm1.04\,\mathrm{R}$ emission is $P_\mathrm{req}\approx5\mathrm{-}12\times10^{41}\,\mathrm{erg\,s}^{-1}$, comfortably exceeded by AGN jet models, plausible for AGN hot accretion flow and star formation ring models, and disfavoring star formation driven winds.
