发表机构
National Radio Astronomy Observatory（国家射电天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出开源Julia脉冲星搜索代码，通过重构脉冲轮廓提升脉冲星恢复率，在CPU和GPU上均比riptide、PRESTO的对应算法更快，且阈值不受红噪声影响。
AI 中文摘要
脉冲星具有窄脉冲，因此其信号在傅里叶变换中会分布在多个谐波上。标准脉冲星搜索会将这些谐波的功率相加并丢弃它们的相位，这会丢失脉冲形状和部分信号。对每个试周期进行时间序列折叠可同时保留两者，但即使使用快速折叠算法（FFA），该操作也很昂贵。我们介绍了这是一个开源Julia代码，可直接从傅里叶变换重构每个试自旋频率下的脉冲轮廓。它对典型60个谐波的复振幅进行插值，将其逆变换为轮廓，并针对多种宽度的箱形模板测试该轮廓。由于输入频谱已归一化，每个轮廓中的噪声以闭式形式可知，因此单个阈值可在整个搜索中给出相同的虚警率。在一项包含超过860000个模拟脉冲星的注入研究中，在匹配的虚警率下，新搜索在白噪声中恢复了76%的脉冲星，而riptide的FFA在推荐配置下恢复64%，PRESTO的accelsearch恢复42%，且其阈值在红噪声下不会变化。在单个CPU核心上，它在匹配频率覆盖范围时比riptide快1.4至2.2倍，在48个核心上可扩展到快27倍，现代GPU运行它比20核工作站快达9倍。
英文摘要
Pulsars have narrow pulses, so their signals spread over many harmonics in a Fourier transform. Standard pulsar searches add the powers of those harmonics and discard their phases, which throws away the pulse shape and some of the signal. Folding the time series at each trial period keeps both, but is expensive even with the Fast Folding Algorithm (FFA). We describe CoherentSearch.jl, an open-source Julia code that reconstructs the pulse profile at every trial spin frequency directly from the Fourier transform. It interpolates the complex amplitudes of typically 60 harmonics, inverse transforms them into a profile, and tests that profile against boxcar templates of many widths. Because the input spectrum is normalized, the noise in every profile is known in closed form, so one threshold gives one false-alarm rate across the whole search. In an injection study of over 860,000 simulated pulsars at a matched false-alarm rate, the new search recovers 76% of the pulsars in white noise, against 64% for riptide's FFA in its recommended configuration and 42% for PRESTO's accelsearch, and its threshold does not move under red noise. On one CPU core it is 1.4-2.2 times faster than riptide at matched frequency coverage, it scales to 27 times faster on 48 cores, and modern GPUs run it up to nine times faster than a 20-core workstation.
CommentsCompleted with significant collaboration with Anthropic's Claude. To be submitted to the Astronomical Journal. Comments welcome
