论文标题
Parkes Ultra Wideband接收器
Pulsar polarimetry with the Parkes Ultra-Wideband receiver
论文作者
论文摘要
观察到脉冲星无线电发射及其极化会随频率发展。该频率依赖性是无线电光束发射机制和结构的关键。借助Parkes射电望远镜上的新的超宽接收器（UWL），我们首次能够观察Pulsar概况如何在700-4000 MHz的宽连续带宽上演变。我们在这里描述了一种处理宽带极化观测的技术，以建立有意义的对齐方式并在整个频段中可视化数据。我们将其应用于PSRS J1056-6258和J1359-6038的观察结果，该观察是由于先前未解决的有关其发射频率演变的问题而选择的。我们技术的应用表明，当仅应用于分散和法拉第旋转的校正时，可以在宽频率范围内对齐极化位置角（PA）。但是，这与这两个来源的对齐强度曲线不符。我们发现，可以将这些未对准转换为与已发表和模拟值一致的排放高度范围估计值，这表明它们可以归因于磁层中的相对论效应。我们在无线电束结构的背景下讨论这项工作，并为使用宽带偏振数据进行更广泛的脉冲星排放准备。
Pulsar radio emission and its polarization are observed to evolve with frequency. This frequency dependence is key to the emission mechanism and the structure of the radio beam. With the new Ultra-Wideband receiver (UWL) on the Parkes radio telescope we are able, for the first time, to observe how pulsar profiles evolve over a broad continuous bandwidth of 700-4000 MHz. We describe here a technique for processing broadband polarimetric observations to establish a meaningful alignment and visualize the data across the band. We apply this to observations of PSRs J1056-6258 and J1359-6038, chosen due to previously unresolved questions about the frequency evolution of their emission. Application of our technique reveals that it is possible to align the polarization position angle (PA) across a broad frequency range when constrained to applying only corrections for dispersion and Faraday rotation to do so. However, this does not correspond to aligned intensity profiles for these two sources. We find that it is possible to convert these misalignments into emission height range estimates that are consistent with published and simulated values, suggesting that they can be attributed to relativistic effects in the magnetosphere. We discuss this work in the context of the radio beam structure and prepare the ground for a wider study of pulsar emission using broadband polarimetric data.
