Multi-wavelength campaign on NGC 7469 V. Analysis of the HST/COS observations: Super solar metallicity, distance, and trough variation models
Multi-wavelength campaign on NGC 7469 V. Analysis of the HST/COS observations: Super solar metallicity, distance, and trough variation models
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NGC 7469 上的多波长活动 V. HST/COS 观测结果分析：超级太阳金属丰度、距离和槽变化模型
DOI：
10.1051/0004-6361/201935342
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发表时间：
2020
影响因子：
6.5
通讯作者：
Arav N
中科院分区：
文献类型：
--
作者：
Arav N
agn的外流被认为会影响其宿主星系及其超大质量黑洞的演化。为了更好地了解这些流出物，我们对NGC 7469进行了深度多波长运动。所得到的数据，结合早期的数据，使我们能够为AGN风构建一个全面的物理、空间和时间图像。目的我们的目的是确定紫外线流出成分与中心源的距离，它们的丰度和总柱密度，以及它们观察到的吸收变化的机制。方法研究了运动期间和之前三个时期（2002-2010）的紫外光谱。我们的主要分析工具是离子柱密度提取技术和基于代码CLOUDY的光电离模型（平衡和时间依赖模型）。对于分量1（在-600 km s−1），我们的发现包括：金属丰度大约是太阳的两倍；一个基于固定总柱密度吸收器的简单模型，对电离照明的变化做出反应，该模型与13年4个光谱时代得出的不同离子柱密度相匹配；和中央电源有一定距离。分量2（在-1430 km s−1处）有浅槽，r大得多。对于分量3（在-1880 km s−1），我们的发现包括：与分量1相似的金属丰度；基于光电离的模型可以解释其复杂的吸收槽变异性和60或150pc / r的上限的主要特征。这个上限与x射线导出的r的12或31 pc的下限是一致和互补的。紫外相的总柱密度分别约为吸热器下部和上部电离组分的1%和0.1%。结论NGC 7469流出物的金属丰度与Mrk 279相似，碳和氮的丰度分别是太阳值的2倍和4倍。与NGC 5548的情况类似，一个简单的模型可以解释流出物的物理特征和变化。
ContextAGN outflows are thought to influence the evolution of their host galaxies and their super massive black holes. To better understand these outflows, we executed a deep multiwavelength campaign on NGC 7469. The resulting data, combined with those of earlier epochs, allowed us to construct a comprehensive physical, spatial, and temporal picture for this AGN wind.AimsOur aim is to determine the distance of the UV outflow components from the central source, their abundances and total column-density, and the mechanism responsible for their observed absorption variability.MethodsWe studied the UV spectra acquired during the campaign as well as from three previous epochs (2002–2010). Our main analysis tools are ionic column-density extraction techniques and photoionization models (both equilibrium and time-dependent models) based on the code CLOUDY.ResultsFor component 1 (at –600 km s−1) our findings include the following: metallicity that is roughly twice solar; a simple model based on a fixed total column-density absorber, reacting to changes in ionizing illumination that matches the different ionic column densities derived from four spectroscopic epochs spanning 13 years; and a distance of pc from the central source. Component 2 (at –1430 km s−1) has shallow troughs and is at a much largerR. For component 3 (at –1880 km s−1) our findings include: a similar metallicity to component 1; a photoionization-based model can explain the major features of its complicated absorption trough variability and an upper limit of 60 or 150 pc onR. This upper limit is consistent and complementary to the X-ray derived lower limit of 12 or 31 pc forR. The total column density of the UV phase is roughly 1% and 0.1% of the lower and upper ionization components of the warm absorber, respectively.ConclusionsThe NGC 7469 outflow shows super-solar metallicity similar to the outflow in Mrk 279, carbon and nitrogen are twice and four times more abundant than their solar values, respectively. Similar to the NGC 5548 case, a simple model can explain the physical characteristics and the variability observed in the outflow.