宽吸收线类星体的X-ray研究进展  

RECENT PROGRESS ON THE BAL QSOS RESEARCH FROM X RAY OBSERVATIONS

作　　者：王挺贵[1] 王俊贤[1] 

机构地区：[1]中国科学技术大学天体物理中心,合肥230026

出　　处：《紫金山天文台台刊》1999年第3期248-253,共6页

摘　　要：本文总结最近从Ｘｒａｙ 观测得到的关于宽吸收线类星体一些新结果， 我们和人家的结果都表明吸收物质的柱密度比原来从紫外估计的高三个量级， 在ＰＧ１４１１ ＋ ４４２ 中， 我们发现Ｘｒａｙ 除了吸收成分外， 还有散射成分， 其量级和ＵＶ 吸收的剩余流量一致， 从而说明以前从ＵＶ 推断的结论是有问题的。此外， 对ＰＧ１１２６０４１ 的研究表明从宽吸收线类星体到Ｓｅｙｆｅｒｔ 星系的窄本征吸收线其物理性质是连续过渡的。We summarize the results from recent X ray observations on the BAL QSOs. The results of ours and other's works clearly demonstrated that the absorbing column densities are three order of magnitude higher than previous estimation based on the UV absorption lines. We found a scattered or leaked unabsorbed soft X ray component, in addition to a heavily absorbed power law component at hard X ray band, in PG 1411+442. The fraction of scattering or leakage is coincident with that of residuals in the UV absorption line troughs. This illustrates that the UV absorption trough actually is black saturated. In addition, detailed analysis of UV and X ray absorption in PG 1126 041 highlights that there is a continuous transition from the BAL phenomenon in QSOs to the intrinsic absorption lines in Seyfert galaxies.

关 键 词：类星体 吸收线 SEYFERT星系 X-射线 柱密度 观测 

分 类 号：P158[天文地球—天文学]