平衡度指数BI =0的致密宽吸收线（BAL）类星体的VLBI观测
A VLBI survey of compact Broad Absorption Lines (BAL) quasars with BALnicity Index BI=0
摘要：
我们提出了高分辨率的观测，使用欧洲VLBI网络（EVN）在1.7 GHz的，和甚长基线阵列（VLBA）在5和8.4 GHz的图像无线电结构的14个紧凑的来源分类为宽吸收线（BAL）类星体的吸收指数（AI）的基础上。所有的来源，但一个解决，与大多数显示核心喷流形态典型的射电响亮类星体。我们将详细讨论最有趣的案例。观测到的天体具有高的射电光度和小的线性尺寸，表明它们是强的年轻活动星系核。然而，更大样本的AI类星体的射电响度参数log（Ri）的分布表明，我们观察到的物体构成了AI种群中最明亮的小子群。此外，我们报告的射电响度参数，分布AI类星体和那些使用传统的balnicity指数（BI），BI类星体的选择显着不同。强吸收与较低的log（Ri）有关，因此可能与较大的视角有关。由于AI类星体的平均对数（Ri）更大，因此方向可能会导致我们看到它们被吸收的程度更低。然而，我们认为，方向不是唯一的参数，影响检测到的吸收。强吸收与弱射电辐射相关联的事实同样重要，值得探索。
英文摘要：
We present high-resolution observations, using both the European VLBI Network (EVN) at 1.7-GHz, and the Very Long Baseline Array (VLBA) at 5 and 8.4-GHz to image radio structures of 14 compact sources classified as broad absorption line (BAL) quasars based on the absorption index (AI). All source but one were resolved, with the majority showing core-jet morphology typical for radio-loud quasars. We discuss in details the most interesting cases. The high radio luminosities and small linear sizes of the observed objects indicate they are strong young AGNs. Nevertheless, the distribution of the radio-loudness parameter, log(Ri), of a larger sample of AI quasars shows that the objects observed by us constitute the most luminous, small subgroup of AI population. Additionally we report that for the radio-loudness parameter, the distribution of AI quasars and those selected by using the traditional balnicity index (BI), BI quasars differ significantly. Strong absorption is connected with the lower log(Ri), and thus probably with larger viewing angles. Since, the AI quasars have on average larger log(Ri), the orientation can cause that we see them less absorbed. However, we suggest that the orientation is not the only parameter that affects the detected absorption. The fact that the strong absorption is associated with the weak radio emission is equally important and worth exploring.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
