光学/紫外/X射线透视RL -- RQ二分法
Optical/UV/X-ray Insights into the RL--RQ Dichotomy
摘要：
我们利用一组与射电测量无关的光学/UV/X射线测量方法研究射电强（RL）类星体和射电静（RQ）类星体之间的关系。我们发现RL源显示出更大的平均半高宽H-β，更弱的FeII发射，没有软X射线过剩，也没有CIV蓝移-所有这些特征都表现在大部分RQ类星体（我们称之为种群A）上。我们发现log L（1.4Ghz）= 31.6 [ergs/s/Hz]（或R=70）是RL类星体具有FRII形态的下限。我们没有发现低于这个水平的隐藏FRII人口的证据。我们的结论是，RL源是一个独特的类星体群体，也可能包括30- 40%的RQ源，显然表现出类似的几何形状和运动学（我们称之为人口B）。这种RQ重叠，如果不是巧合的话，可能包括不活跃的RL类星体以及几何/运动学类似于RL源的类星体，但其中RL活动以某种方式被抑制（例如宿主形态，BH自旋）。
英文摘要：
We explore the relationship between radio-loud (RL) and radio-quiet (RQ) quasars using a set of optical/UV/X-ray measures that are quite independent of radio measures. We find RL sources to show larger average FWHM H-beta, weaker FeII emission, no soft X-ray excess and no CIV blueshift - all characteristics manifested by a large fraction of RQ quasars (that we call Population A). We find that log L (1.4Ghz) = 31.6 [ergs/s/Hz] (or R=70) is the lower limit for RL quasars showing FRII morphology. We find no evidence for a hidden FRII population below this level. We conclude that RL sources are a distinct quasar population that may also include 30-40 percent of RQ sources which apparently show similar geometry and kinematics (what we call Population B). This RQ overlap, if not coincidental, may include inactive RL quasars as well as quasars with geometry/kinematics similar to RL sources but where RL activity is inhibited in some way (e.g. host morphology, BH spin).
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