PCA的光谱能量分布和发射线特性的红色2 MASS AGN
PCA of the spectral energy distribution and emission line properties of red 2MASS AGN
摘要：
利用主成分分析方法分析了Chandra观测到的红色（J-K $_S$ > 2）2 MASS活动星系核的光谱能量分布和发射线性质。根据X射线和SED模拟结果，该样品包括44个低红移活动星系核，具有低或中等的遮蔽度（N_H < 10^{23} cm^{-2}）。活动星系核的遮蔽使我们能够看到较弱的发射成分（宿主星系发射，活动星系核散射光），这些成分通常被活动星系核所掩盖。前四个特征向量解释了样本中70%的方差。样品中的方差的主要原因（特征向量1）是由固有吸收加强的L/Ledd比。特征向量2与宿主星系（相对于观测到的活动星系核）的发射有关，特征向量3和4区分了两种遮蔽源：宿主星系吸收和环核吸收。虽然我们的分析是一致的统一计划，其中倾斜相关的遮蔽是重要的，在确定活动星系核的SEDs，L/Ledd比是最重要的因素，其次是宿主星系的排放。
英文摘要：
We analyze the spectral energy distributions (SEDs) and emission line properties of the red (J-K$_S$ > 2) 2MASS AGN observed by Chandra using principle component analysis. The sample includes 44 low redshift AGN with low or moderate obscuration (N_H < 10^{23} cm^{-2}) as indicated by X-rays and SED modeling. The obscuration of the AGN allows us to see weaker emission components (host galaxy emission, AGN scattered light) which are usually outshone by the AGN. The first four eigenvectors explain 70% of the variance in the sample. The dominant cause of variance in the sample (eigenvector 1) is the L/Ledd ratio strengthened by intrinsic absorption. Eigenvector 2 is related to host galaxy (relative to the observed AGN) emission and eigenvectors 3 and 4 distinguish between two sources of obscuration: host galaxy absorption and circumnuclear absorption. Although our analysis is consistent with unification schemes where inclination dependent obscuration is important in determining the AGN SEDs, the L/Ledd ratio is the most important factor, followed by host galaxy emission.
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