限制高频峰值的性质。II。偏振特性
Constraining the nature of High Frequency Peakers. II. Polarization properties
摘要：
目的：“明亮”高频尖峰样品是耀变体和本质上小而年轻的射电源的混合物。我们调查的极化特性的45个高频峰，从“明亮”的HFP样本，为了有一个更深入的了解每个对象的性质，并构建一个样本的真正年轻的无线电源。研究方法：同时进行的VLA观测在22.2，15.3，8.4和5.0 GHz，连同在1.4 GHz的信息提供的NVSS在较早的时代，已被用来研究线偏振辐射。结果如下：从45个源的偏振特性的分析，我们发现，26（58%）至少在一个频率极化，而17（38%）是完全非极化在所有的频率。我们发现分数偏振和总强度变化之间的相关性。我们证实了星系和类星体的偏振性质之间存在着明显的区别：17个（66%）类星体是高度偏振的，而所有9个星系要么是非偏振的（<0.2%），要么是偏振度小于1%的边缘偏振的。这表明，大多数被类星体识别的HFP候选者可能代表不同于年轻射电天体的射电源群。
英文摘要：
Aims: The ``bright'' High Frequency Peakers (HFPs) sample is a mixture of blazars and intrinsically small and young radio sources. We investigate the polarimetric characteristics of 45 High Frequency Peakers, from the ``bright'' HFP sample, in order to have a deeper knowledge of the nature of each object, and to construct a sample made of genuine young radio sources only. Methods: Simultaneous VLA observations carried out at 22.2, 15.3, 8.4 and 5.0 GHz, together with the information at 1.4 GHz provided by the NVSS at an earlier epoch, have been used to study the linearly polarized emission. Results: From the analysis of the polarimetric properties of the 45 sources we find that 26 (58%) are polarized at least at one frequency, while 17 (38%) are completely unpolarized at all frequencies. We find a correlation between fractional polarization and the total intensity variability. We confirm that there is a clear distinction between the polarization properties of galaxies and quasars: 17 (66%) quasars are highly polarized, while all the 9 galaxies are either unpolarized (<0.2%) or marginally polarized with fractional polarization below 1%. This suggests that most HFP candidates identified with quasars are likely to represent a radio source population different from young radio objects.
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