捕捉一个成年海星行星状星云II。PC 22的等离子体分析和中心星性质
Catching a grown-up starfish planetary nebula II. Plasma analysis and central star properties of PC 22
摘要：
在对行星状星云（PN）PC 22进行了形态运动学分析之后，我们现在介绍它的星云和恒星分析。等离子体调查依赖于与PyNeb代码相关的蒙特卡罗分析的新用途，用于不确定性传播。星云最里面的区域显示电子温度$T_{\rm e}$ $\approx$ 10，800 K（使用[NII]）和13，000 K（使用[OIII]），电子密度$n_{\rm e}$ $\approx$ 600 cm $^{-3}$。我们还首次使用机器学习算法来计算专门适用于PC 22的电离校正因子（ICF）。这使我们能够获得（S $^{+}$ + S $^{++}$）/O $^{++}$、Cl $^{++}$ /O $^{++}$和Ar $^{3+}$ +Ar $^{4+}$的先驱ICF，以及可能的氖总丰度的新测定。对恒星光谱的研究揭示了宽发射线的存在，与Wolf-Rayet类型[WR]分类一致，更确切地说，是基于不同定性和定量标准的[WO 1]亚型。这种分类也与高恒星温度是一致的，该温度是从墨西哥百万模型数据库（3 MdB）的气体电离态的再现和NLTE模型大气代码PoWR获得的最佳拟合模型中得出的。因此，PC 22是[WO 1]-亚型PNe的新成员。
英文摘要：
After performing the morpho-kinematic analysis of the planetary nebula (PN) PC 22, we now present its nebular and stellar analysis. The plasma investigation relies on the novel use of a Monte Carlo analysis associated to the PyNeb code for the uncertainty propagation. The innermost region of the nebula shows electronic temperatures $T_{\rm e}$ $\approx$ 10,800~K using [NII] and $\approx$ 13,000 K using [OIII] and electronic densities $n_{\rm e}$ $\approx$ 600~cm$^{-3}$. We also used for the first time a Machine Learning Algorithm to calculate Ionisation Correction Factors (ICFs) specifically adapted to PC 22. This has allowed us to have pioneer ICFs for (S$^{+}$ + S$^{++}$)/O$^{++}$, Cl$^{++}$/O$^{++}$, and Ar$^{3+}$+Ar$^{4+}$, as well as a possible new determination for the total abundance of neon. The study of the stellar spectrum revealed the presence of broad emission lines consistent with a Wolf-Rayet-type [WR] classification and more precisely a [WO1]-subtype based on different qualitative and quantitative criteria. This classification is also coherent with the high stellar temperature derived from the reproduction of the ionization state of the gas with the Mexican Million Models database (3MdB) and the best fit model obtained with the NLTE model atmosphere code PoWR. PC 22 is therefore a new addition to the [WO1]-subtype PNe.
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