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首页> 外文期刊>The Astrophysical journal >A PHOTOIONIZATION MODEL FOR THE SOFT X-RAY SPECTRUM OF NGC 4151
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A PHOTOIONIZATION MODEL FOR THE SOFT X-RAY SPECTRUM OF NGC 4151

机译：NGC 4151的软X射线光谱的光化模型

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摘要

We present an analysis of archival data from multiple XMM-Newton observations of the Seyfert 1 galaxy NGC 4151. Spectral data from the RGS instruments reveal several strong soft X-ray emission lines, chiefly from hydrogen-like and helium-like oxygen, nitrogen, neon, and carbon. Radiative recombination continua (RRC) from oxygen and carbon are also detected. Our analysis suggests that the emission data are consistent with photoionization. Using the Cloudy photoionization code, we found that, while a two-component, high column density model (10~(23) cm~(-2)) with low covering factor proved adequate in reproducing all detected Lyman series lines, it proved insufficient in modeling the He-like triplets observed (neon, oxygen, and nitrogen). If resonance line data were ignored, the two-component model was sufficient to match flux from intercombination and forbidden lines. However, with the inclusion of resonance line data, He-like triplets could no longer be modeled with only two components. We found that observed oxygen G and R ratios in particular were anomalous in the parameter space investigated. We investigated, and were forced to dismiss, the possibility that a third, purely collisional component could be responsible for enhanced resonance line contributions. We succeeded in modeling the observed spectrum with the addition of a third, lower column density (10~(20.5) cm~(-2)) component with nonzero microturbulence and high covering factor. While sufficient to reproduce observed soft X-ray flux, our model has certain shortcomings, particularly in a less-than-ideal visual fit to the line profile. Two of the three emission model components bear similarities to components determined by Kraemer et al. in their 2005 study of NGC 4151 absorption spectra.
机译：我们对塞弗特1号星系NGC 4151的多个XMM-牛顿观测结果进行了归档数据分析。RGS仪器的光谱数据显示了几条强的软X射线发射谱线，主要来自类氢和类氦的氧，氮，氖和碳。还可以检测到氧和碳的辐射复合连续体（RRC）。我们的分析表明，发射数据与光电离一致。使用云光电离代码，我们发现，虽然覆盖率低的两组分高柱密度模型（10〜（23）cm〜（-2））足以重现所有检测到的Lyman系列谱线，但事实证明这是不够的在建模中观察到的He状三重态（氖，氧和氮）。如果忽略共振线数据，则两成分模型足以匹配来自组合线和禁线的通量。但是，由于包含了共振线数据，像He一样的三元组不再仅用两个分量建模。我们发现，在所研究的参数空间中，观察到的氧气G和R比尤其是异常的。我们调查了第三种纯粹碰撞的成分可能导致共振线增强的可能性，并被迫放弃。我们成功地对观察到的光谱进行了建模，增加了第三个较低的柱密度（10〜（20.5）cm〜（-2））组分，该组分具有非零微湍流和高覆盖因子。虽然足以重现观察到的软X射线通量，但我们的模型仍存在某些缺陷，特别是在对线轮廓的视觉拟合不理想的情况下。三种排放模型成分中的两种与Kraemer等人确定的成分相似。在他们2005年对NGC 4151吸收光谱的研究中。

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