O i Line Emission in the Quasar PG 1116+215
O i Line Emission in the Quasar PG 1116+215
复制标题
类星体中的 O i 线发射 PG 1116 215
DOI：
10.1093/pasj/57.4.563
复制
发表时间：
2005
影响因子：
2.3
通讯作者：
Y. Yoshii
中科院分区：
文献类型：
--
作者：
Y. Matsuoka;S. Oyabu;Y. Tsuzuki;K. Kawara;Y. Yoshii
通过观测类星体PG 1116+215在z = 0.176处的近红外光谱，并结合HST/FOS光谱，我们首次获得了类星体中三条允许的OI谱线（{lambda}1304，{lambda}8446和{lambda}11287）的相对强度。类星体的OI线的光子通量比与先前在Seyfert 1和6个窄线Seyfert 1 s中测量的光子通量比进行了比较。没有发现显着差异的类星体和其他Seyfert之间的OI线的流量比，这表明在类星体的OI和FeII线发射区的气体密度是在低光度活动星系核的数量级相同。还发现OI {λ}11287的线宽明显窄于Ly{alpha}的线宽，这与在速度小的宽线区域的最外部分处的部分电离区域中发生的OI和Fe II发射一致。
By observing the near-infrared spectrum of the quasar PG 1116+215 at z = 0.176 and combining with the HST/FOS spectrum, we obtained the relative strengths of three permitted OI lines ({lambda}1304, {lambda}8446, and {lambda}11287) in a quasar for the first time. The photon flux ratios of the OI lines of the quasar were compared with those previously measured in a Seyfert 1 and six narrow-line Seyfert 1s. No significant differences were found in the OI line flux ratios between the quasar and the other Seyferts, suggesting that the gas density in the OI and FeII line-emitting regions in the quasar is of the same order as those in low-luminosity AGNs. It was also found that the line width of OI {lambda}11287 is significantly narrower than that of Ly{alpha}, which is consistent with OI and FeII emission occurring in the partly ionized regions at the outermost portion of the broad-line region where velocities are small.