射电暂现源的选择修正光度函数与总脉冲计数的约束
Constraining the selection corrected luminosity function and total pulse count for radio transients
AI总结：
本文提出贝叶斯嵌套采样算法 LuNfit，用于修正射电暂现源的选择偏差，估计单脉冲内禀光度分布与消零比例，并在三个 RRAT 上验证了其稳健性和优于传统按比例放大修正法的表现。
摘要：
在天文大数据时代，研究暂现现象（例如脉冲星的单个脉冲）已引起广泛关注。本研究特别关注旋转射电暂现源（RRATs）、消零脉冲星和间歇脉冲星。本研究引入了一种名为 LuNfit 的新算法，专门用于修正源自望远镜和探测流程的选择偏差。最终，LuNfit 估计脉冲星所发射单脉冲的内禀光度分布和消零比例。LuNfit 依赖贝叶斯嵌套采样，从而能够充分探索参数空间。贝叶斯嵌套采样还提供了额外的好处，即通过贝叶斯比值简化模型比较。通过模拟以及将 LuNfit 应用于已知消零比例的脉冲星，展示了 LuNfit 的稳健性。随后，将 LuNfit 应用于三个 RRAT：J0012+5431、J1538+1523 和 J2355+1523，提取它们的内禀光度分布和爆发率。我们发现它们的消零比例分别为 0.4(2)、0.749(5) 和 0.995(2)。我们进一步发现，对数正态分布很可能能够描述 J0012+5431 和 J1538+1523 的单脉冲光度分布，而 J2355+1523 的贝叶斯比值则略微倾向于指数分布。我们表明，当源的平均光度相对于望远镜灵敏度较暗时，通过“按比例放大”射电暂现源被遗漏部分来修正选择效应的传统方法可能不可靠。最后，我们讨论了 LuNfit 当前实现方式的局限性，同时探讨了潜在的改进方向，这些改进将使 LuNfit 能够应用于具有复杂脉冲形态的源。
英文摘要：
Studying transient phenomena, such as individual pulses from pulsars, has garnered considerable attention in the era of astronomical big data. Of specific interest to this study are Rotating Radio Transients (RRATs), nulling, and intermittent pulsars. This study introduces a new algorithm named LuNfit, tailored to correct the selection biases originating from the telescope and detection pipelines. Ultimately LuNfit estimates the intrinsic luminosity distribution and nulling fraction of the single pulses emitted by pulsars. LuNfit relies on Bayesian nested sampling so that the parameter space can be fully explored. Bayesian nested sampling also provides the additional benefit of simplifying model comparisons through the Bayes ratio. The robustness of LuNfit is shown through simulations and applying LuNfit onto pulsars with known nulling fractions. LuNfit is then applied to three RRATs, J0012+5431, J1538+1523, and J2355+1523, extracting their intrinsic luminosity distribution and burst rates. We find that their nulling fraction is 0.4(2), 0.749(5) and 0.995(2) respectively. We further find that a log-normal distribution likely describes the single pulse luminosity distribution of J0012+5431 and J1538+1523, while the Bayes ratio for J2355+1523 slightly favors an exponential distribution. We show the conventional method of correcting selection effects by "scaling up" the missed fraction of radio transients can be unreliable when the mean luminosity of the source is faint relative to the telescope sensitivity. Finally, we discuss the limitations of the current implementation of LuNfit while also delving into potential enhancements that would enable LuNfit to be applied to sources with complex pulse morphologies.
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