We present new hard X-ray spectra of three radio-loud active galactic nuclei (AGNs) of moderately high X-ray luminosity (LX ≈ 1045 ergs s-1; PKS 2349-01, 3C 323.1, and 4C 74.26) obtained with ASCA and BeppoSAX. The X-ray continua are described in all three cases with a power-law model with photon indices Γ ≈ 1.85, modified at low energies by absorption in excess of the galactic value, which appears to be due to neutral gas. At higher energies, an Fe Kα emission line is detected in PKS 2349-01 and 4C 74.26 and is tentatively detected in 3C 323.1. The equivalent widths of the lines are consistent, albeit within large uncertainties, with the values for radio-quiet AGNs of comparable X-ray luminosity. The Fe Kα line is unresolved in 4C 74.26. In the case of PKS 2349-01, however, the inferred properties of the line depend on the model adopted for the continuum: if a simple power-law model is used, the line is resolved at more than 99% confidence with a full width at half-maximum corresponding to approximately 50,000 km s-1 and a rest-frame equivalent width of 230 ± 120 eV; however, if a Compton "reflection" model is used, the line is found to be a factor of 2 weaker for an assumed full width at half-maximum of 50,000 km s-1. In 4C 74.26, a strong Compton "reflection" component is detected. Its strength suggests that the scattering medium subtends a solid angle of 2π to the illuminating source. Overall, the spectral indices of these radio-loud quasars are remarkably similar to those of their radio-quiet counterparts. On the other hand, if the absorber is indeed neutral, as our results suggest, this would be consistent with the typical properties of radio-loud AGNs.
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机译：我们提出了使用ASCA获得的三个中等高X射线光度（LX≈1045 ergs s-1; PKS 2349-01、3C 323.1和4C 74.26）的三个放射性大声活跃银河核（AGN）的新硬X射线光谱和BeppoSAX。在所有这三种情况下，均使用幂律模型描述了X射线连续性，该幂律模型的光子指数Γ≈1.85，在低能量下通过吸收超过银河系值而被修改，这似乎是由于中性气体引起的。在较高的能量下，在PKS 2349-01和4C 74.26中检测到FeKα发射线，并在3C 323.1中初步检测到。线的等效宽度是一致的，即使在很大的不确定性内，也与可比较的X射线发光度的无声AGN值一致。 FeKα线在4C 74.26中未解析。但是，在PKS 2349-01的情况下，线的推断属性取决于连续体所采用的模型：如果使用简单的幂律模型，则线的全宽解析度超过99％对应于大约50,000 km s-1的一半最大值和230±120 eV的静止帧等效宽度;但是，如果使用康普顿“反射”模型，则对于假定最大宽度为50,000 km s-1的一半时，发现该线弱2倍。在4C 74.26中，检测到强康普顿“反射”分量。它的强度表明，散射介质与光源的对角为2π。总的来说，这些无线电大类星体的光谱指数与无线电类静星的光谱指数非常相似。另一方面，如我们的结果所示，如果吸收器确实是中性的，则这与无线电响AGN的典型特性是一致的。
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