论文标题
NGC 3227的X射线光谱的组合分析
Combined Analysis of X-Ray Spectra of NGC 3227
论文作者
论文摘要
几个X射线任务观察到了1.5 Seyfert Galaxy NGC 3227。我们通过对来源的最新主要观察结果进行了对数据获得的组合分析：XMM-Newton在2000年和2006年进行了两个观察结果，以及2008年Suzaku进行的六个观察结果。统一模型与两种卫星的观察一致，这是两种卫星的巨大强度和频谱变化，构建了。该模型由伽马硬度= 1.4-1.7的频谱指数组成，该法则被解释为积聚磁盘上方的电晕的构成发射。在高频率状态下，额外的软分成分占主导地位，这与具有较陡峭的功率定律的模型一致，伽马软= 3.3-3.85或温暖的构成组件。中央发动机的这些排放被部分覆盖的材料和温暖的吸收剂所吸收。还存在反射组件和几个发射线。我们检查了内在的光度与吸收器的物理参数（例如色谱柱密度）之间的关系，这表明当软过量大大增强时，源在明亮状态下显着扩展。
The 1.5 Seyfert galaxy NGC 3227 has been observed by several X-ray missions. We carried out a combined analysis of the data obtained by more recent major observations of the source: two observations performed by XMM-Newton in 2000 and 2006 and six observations performed by Suzaku in 2008. A unified model, which is consistent with all eight observations by the two satellites with large intensity and spectral changes, was constructed. The model consists of a hard power law withe the spectral index of Gamma Hard = 1.4-1.7, which is interpreted as the Comptonized emission from the corona above an accretion disk. In the high-flux states, an additional soft excess component dominates, which is consistent with a model with either a steeper power law with Gamma Soft = 3.3-3.85, or the warm Comptonization component. These emissions from the central engine are absorbed by a partial covering material and warm absorbers. A reflection component and several emission lines are also present. We examined the relationship between the intrinsic luminosity and the absorbers' physical parameters such as the column density, which suggests that the source expanded significantly during the bright states when the soft excess is greatly enhanced.
