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A study of multifrequency polarization pulse profiles of millisecond pulsars

机译:毫秒脉冲星的多频极化脉冲分布研究

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摘要

We present high signal-to-noise ratio, multifrequency polarization pulse profiles for 24 millisecond pulsars that are being observed as part of the Parkes Pulsar Timing Array project. The pulsars are observed in three bands, centred close to 730, 1400 and 3100 MHz, using a dual-band 10 cm/50 cm receiver and the central beam of the 20-cm multibeam receiver. Observations spanning approximately six years have been carefully calibrated and summed to produce high S/N profiles. This allows us to study the individual profile components and in particular how they evolve with frequency. We also identify previously undetected profile features. For many pulsars we show that pulsed emission extends across almost the entire pulse profile. The pulse component widths and component separations follow a complex evolution with frequency; in some cases these parameters increase and in other cases they decrease with increasing frequency. The evolution with frequency of the polarization properties of the profile is also non-trivial. We provide evidence that the pre- and post-cursors generally have higher fractional linear polarization than the main pulse. We have obtained the spectral index and rotation measure for each pulsar by fitting across all three observing bands. For the majority of pulsars, the spectra follow a single power-law and the position angles follow a λ^2 relation, as expected. However, clear deviations are seen for some pulsars. We also present phase-resolved measurements of the spectral index, fractional linear polarization and rotation measure. All these properties are shown to vary systematically over the pulse profile.
机译:我们提出了24毫秒脉冲星的高信噪比,多频极化脉冲分布图,这是Parkes Pulsar Timing Array项目的一部分。使用双频10 cm / 50 cm接收器和20厘米多波束接收器的中心波束,可以在三个中心(接近730、1400和3100 MHz)观察脉冲星。仔细观察校准了大约六年的观测值,并将其汇总以产生高信噪比。这使我们能够研究各个轮廓分量,尤其是它们如何随频率变化。我们还将识别以前未检测到的配置文件功能。对于许多脉冲星,我们证明了脉冲发射几乎遍及整个脉冲轮廓。脉冲成分的宽度和成分的分离随频率而变化。在某些情况下,这些参数会增加,而在其他情况下,它们会随着频率的增加而减小。轮廓的偏振特性随频率的变化也是不平凡的。我们提供的证据表明,前体和后体通常具有比主脉冲更高的分数线性极化。通过拟合所有三个观测频带,我们获得了每个脉冲星的光谱指数和旋转测量。对于大多数脉冲星,光谱遵循单个幂律,而位置角遵循λ^ 2关系。但是,对于某些脉冲星,可以看到明显的偏差。我们还提出了光谱指数,分数线性极化和旋转测量的相位分辨测量。所有这些特性都显示在脉冲轮廓上系统地变化。

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    Dai S.; Burke-Spolaor S.;

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  • 年度 2015
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