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arXiv 2512.04533astro-ph.SRastro-ph.GA
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银河高ADF PNe的形态-动力学研究：基于VLT/UVES深谱观测

A Morpho-kinematic Study of Galactic High-ADF PNe Based on the VLT/UVES Deep Spectroscopy

National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Science（中国科学院大学）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；The University of Hong Kong（香港大学）；Beijing Normal University（北京师范大学）；New Cornerstone Science Laboratory, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台新Cornerstone科学实验室）；Yunnan University（云南大学）

Haomiao Huang, Xuan Fang, Jorge Garcia-Rojas, Zhijun Tu, Jifeng Liu, Xiaowei Liu

备注：
Accepted for publication in ApJS. In total, 49 pages including 35 figures (one in Appendix) and 16 tables (three in Appendix); very careful analysis of the VLT UVES high-dispersion spectra of three Galactic planetary nebulae: Hf2-2, M1-42 and NGC6153
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AI总结：

通过VLT/UVES深谱观测，研究高ADF PNe的形态-动力学特性，发现冷金属丰富气体与暖金属正常气体的双成分结构，重元素在冷气体中富集，影响CEL丰度估计。

摘要：

我们报告了三个银河系行星状星云（PNe）Hf2-2、M1-42和NGC6153的深高分辨率光谱的详细分析，这些光谱是通过8.2米甚大望远镜（VLT）上的紫外和可见光光谱仪（UVES）获得的，具有高丰度不一致因子（ADFs）。这些光谱经过仔细处理，包括严格的绝对通量校准，每个PNe检测到约410-800条发射线。通过星云线进行等离子体诊断和丰度计算。在所有三个PNe中，使用碰撞激发线（CELs）得出的电子温度高于由HI巴尔末和帕森跃迁得出的温度，而由OII和NII光学重新结合线（ORLs）得出的温度非常低，<2000 K，表明重元素ORLs探测冷星云区域。N、O和Ne的ORL丰度系统性高于对应的CEL值，证实了这三个物体的高ADFs。制作了位置-速度（PV）图，空间-动力学研究显示，CELs来自外星云区域，而ORL发射区域接近星云中心。此外，由CEL线分裂指示的速度随着离子化势降低而减少，这在ORLs中不明显。这些空间和动力学差异支持了两种不同的离子化气体成分：一个冷、金属丰富的成分和一个较暖、金属licity正常的成分。重元素在冷气体中强烈富集，而其H+分数较低但仍然产生显著HI发射，影响CEL丰度估计。

英文摘要：

We report detailed analyses of deep, high-resolution spectra of three Galactic planetary nebulae (PNe) with high abundance discrepancy factors (ADFs), Hf2-2, M1-42 and NGC6153, obtained with the Ultraviolet and Visual Echelle Spectrograph (UVES) on the 8.2m Very Large Telescope (VLT). These spectra were carefully reduced, including rigorous absolute flux calibration, yielding detections of ~410-800 emission lines in each PN. Plasma diagnostics and abundance calculations were critically performed using nebular lines. In all three PNe, the electron temperatures derived using the collisionally excited lines (CELs) are higher than those yielded by the HI Balmer and Paschen jumps, while the temperatures yielded by the OII and NII optical recombination lines (ORLs) are very low, <2000 K, indicating that the heavy-element ORLs probe cold nebular regions. The ORL abundances of N, O and Ne are systematically higher than the corresponding CEL values, confirming high ADFs in the three objects. Position-velocity (PV) diagrams were created, and spatio-kinematical studies show that CELs come from the outer nebular regions, while the ORL-emitting regions are close to nebular center. Additionally, the velocity indicated by CEL line-splitting decreases with ionization potential, which was not obvious in ORLs. These spatial and kinematic differences support two distinct components of ionized gas: a cold, metal-rich component and a warmer component with normal metallicity. Heavy elements are strongly enriched in the cold gas, while its H^+ fraction is low but still produces significant HI emission, affecting CEL abundance estimates.

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