用LOFAR进行脉冲星闪烁研究。I.人口普查
Pulsar scintillation studies with LOFAR. I. The census
摘要：
上下文脉冲星辐射的星际闪烁（ISS）既可以作为电离星际介质（IISM）的探测器，又会对脉冲星计时实验造成干扰。特别令人感兴趣的是所谓的闪烁弧，它可以用来直接测量时变星际散射延迟，有可能提高定时精度。目的。本研究的主要目的是进行第一次大规模和自洽普查的衍射脉冲星闪烁和闪烁弧的可探测性在低频率，作为引物的大规模IISM研究和脉冲星定时相关的传播研究与低频阵列射线（LOFAR）高波段探测器（HBA）。结果在最初的31个源中，有15个可以完全确定闪烁特性;其中9个在120-180 MHz处显示出可检测的闪烁弧。八个观测到的源显示未分辨的闪烁，最后八个不显示衍射闪烁。闪烁可探测性与脉冲星亮度和色散测量之间的某些相关性是明显的，尽管没有明确的截止值可以确定。我们的测量在一个大的分数带宽允许一个有意义的测试闪烁参数的频率缩放，不受折射闪烁变化的影响。结论.我们的研究结果表明，强大的优势和巨大的潜力，国际空间站的研究在低频率和复杂的依赖脉冲星亮度和星际色散等参数的闪烁可探测性。这项工作提供了大规模普查和长期监测星际闪烁效应在低频的第一部分。
英文摘要：
Context. Interstellar scintillation (ISS) of pulsar emission can be used both as a probe of the ionised interstellar medium (IISM) and cause corruptions in pulsar timing experiments. Of particular interest are so-called scintillation arcs which can be used to measure time-variable interstellar scattering delays directly, potentially allowing high-precision improvements to timing precision. Aims. The primary aim of this study is to carry out the first sizeable and self-consistent census of diffractive pulsar scintillation and scintillation-arc detectability at low frequencies, as a primer for larger-scale IISM studies and pulsar-timing related propagation studies with the LOw-Frequency ARray (LOFAR) High Band Antennae (HBA). Results. In this initial set of 31 sources, 15 allow full determination of the scintillation properties; nine of these show detectable scintillation arcs at 120-180 MHz. Eight of the observed sources show unresolved scintillation; and the final eight don't display diffractive scintillation. Some correlation between scintillation detectability and pulsar brightness and dispersion measure is apparent, although no clear cut-off values can be determined. Our measurements across a large fractional bandwidth allow a meaningful test of the frequency scaling of scintillation parameters, uncorrupted by influences from refractive scintillation variations. Conclusions. Our results indicate the powerful advantage and great potential of ISS studies at low frequencies and the complex dependence of scintillation detectability on parameters like pulsar brightness and interstellar dispersion. This work provides the first installment of a larger-scale census and longer-term monitoring of interstellar scintillation effects at low frequencies.
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