用部分遮蔽的吸积盘模型解释活动星系核移动的宽巴耳末辐射线
partly obscured accretion disk model to explain Shifted broad Balmer emission lines of Active Galactic Nuclei
摘要：
提出了一个新的模型来解释活动星系核（AGN）宽发射线区（BLR）中红/蓝移的宽低电离发射线，特别是光学波段的发射线的出现，这通常被认为是线发射气体径向运动的指示。我们发现，部分模糊的盘状BLR的DBP发射器（AGN与双峰宽低电离发射线）也可以成功地产生移位的标准高斯宽巴耳末发射线。然后，我们计算了两种移动的宽巴耳末发射线的活动星系核的BH质量。我们发现，从M-西格玛关系计算的BH质量系统大于维里BH质量为选定的对象，即使在BLR的内部红化效应的校正。对于宽谱线移动的天体，其维里BH质量比M-σ关系中的BH质量小，这与我们从部分遮蔽的吸积盘模型中所期望的结果相一致。因此，我们提供了一个可选的更好的模型来解释的外观移动广泛的发射线，特别是对于那些对象被低估的维里BH质量。
英文摘要：
We present a new model to explain the appearance of red/blue-shifted broad low-ionization emission lines, especially emission lines in optical band, which is commonly considered as an indicator of radial motion of the line emitting gas in broad emission line regions (BLRs) of Active Galactic Nuclei (AGN). We show that partly obscured disk-like BLRs of dbp emitters (AGN with double-peak broad low-ionization emission lines) can also successfully produce shifted standard Gaussian broad balmer emission lines. Then we calculate two kinds of BH masses for AGN with shifted broad balmer emission lines selected from SDSS. We find that the BH masses calculated from M-sigma relation are systematically larger than virial BH masses for the selected objects, even after the correction of internal reddening effects in BLRs. The smaller virial BH masses than BH masses from M-sigma relation for objects with shifted broad emission lines are coincident with what we expect from the partly obscured accretion disk model. Thus, we provide an optional better model to explain the appearance of shifted broad emission lines, especially for those objects with underestimated virial BH masses.
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