Self consistent grain depletions and abundances II: Effects on strong-line diagnostics of extragalactic H ii regions
Self consistent grain depletions and abundances II: Effects on strong-line diagnostics of extragalactic H ii regions
复制标题
自相一致的颗粒消耗和丰度 II：对河外 H ii 区域强线诊断的影响
DOI：
10.1093/mnras/stad322
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发表时间：
2023
影响因子：
4.8
通讯作者：
Ferland, Gary
中科院分区：
文献类型：
--
作者：
Gunasekera, Chamani M;Ji, Xihan;Chatzikos, Marios;Yan, Renbin;Ferland, Gary
使用任何视线的广义耗尽强度F*以及趋势线参数AX、BX和zX来表征尘埃颗粒上的元素耗尽。参数 AX、BX 和 zX 定义相对耗尽模式，其值已在之前的作品中发布。本研究使用这些参数计算 15 种不同元素的耗尽后气相丰度，同时将 F* 从 0 变化到 1。通过将计算的丰度输入 acloudy 模型获得的对出现的强谱线强度的分析表明，耗尽强度对预测的发射线和电离云的热平衡具有重要影响。元素消耗的量也会影响气体中冷却剂的丰度。此外，还发现每个参数——金属丰度、电离参数U和耗尽强度F*对发射线强度和星际介质（ISM）的热平衡都有简并影响。最后，将我们的结果与使用阿帕奇点天文台附近星系测绘调查 (MaNGA) 获得的数据的 Hiiregions 样本进行比较，结果表明最佳拟合 F* 约为 0.5。然而，这个最佳拟合值并不适用于所有金属度。消除硫消耗并改变氮丰度模式可以改善拟合。因此，需要额外的观测证据来验证参数的选择并更好地限制星系中典型的耗尽强度。
The depletion of elements onto dust grains is characterized using a generalized depletion strengthF*for any sightline, and trend-line parametersAX, BX, andzX. The parametersAX, BX, andzXdefine the relative depletion pattern, for which values are published in previous works. The present study uses these parameters to calculate post-depleted gas-phase abundances of 15 different elements while varyingF*from 0 to 1. An analysis of emergent strong spectral line intensities, obtained by inputting the calculated abundances into acloudymodel, shows that the depletion strength has a non-trivial effect on predicted emission lines and the thermal balance of the ionized cloud. The amount by which elements deplete also affects the coolant abundances in the gas. Furthermore, it was found that each of the parameters – metallicity, ionization parameterU, and depletion strengthF*have degenerate effects on the emission-line strengths, and thermal balance of the interstellar medium (ISM). Finally, comparing our results to a sample of Hiiregions using data obtained from the Mapping Nearby Galaxies at Apache Point Observatory survey (MaNGA) revealed that the best-fitF*was approximately 0.5. However, this best-fitting value does not work well for all metallicities. Removing the sulfur depletion and changing the nitrogen abundance pattern can improve the fit. As a result, extra observational evidence is required to verify the choices of parameters and better constrain the typical depletion strength in galaxies.