发表机构
Center for Computational Relativity and Gravitation, Rochester Institute of Technology; Golisano College of Computing and Information Sciences, Rochester Institute of Technology; Instituto Argentino de Radioastronomía (CCT La Plata, CONICET; CICPBA; UNLP); Facultad de Matemática, Astronomía, Física y Computación, UNC; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（罗切斯特理工学院相对论与引力计算中心; 罗切斯特理工学院戈利萨诺计算机与信息科学学院; 阿根廷射电天文研究所; 科尔多瓦大学数学、天文学、物理与计算学院; 拉普拉塔国立大学天文与地球物理科学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究对2024年船帆座脉冲星glitch进行单脉冲再分析，将机器学习单脉冲流水线扩展至两颗脉冲星观测，发现船帆座脉冲星簇的特性、计时解的影响及另一颗脉冲星的信噪比与精度提升结果。
AI 中文摘要
阿根廷脉冲星监测（PuMA）合作组系统监测南部发生 glitch 的脉冲星，维持船帆座脉冲星的高采样率单脉冲记录。我们利用阿根廷射电天文研究所带宽为 400 MHz 的 ROACH 后端，对 2024 年船帆座脉冲星（PSR J0835−4510）的重大 glitch 进行了逐脉冲再分析，并将我们的机器学习单脉冲流水线——孤立森林（Isolation Forest）异常值剔除、β 变分自编码器（β-Variational-AutoEncoder）去噪及自组织映射（Self-Organizing Map）聚类——扩展至 PSR J1644−4559 与毫秒脉冲星 PSR J0437−4715 的新观测。对于船帆座脉冲星， glitch 前后八天数据的 4 簇与 6 簇分解，以七倍于此前的带宽重现了窄带 ETTUS 接收机观测到的行为：振幅更高的簇在相位上峰值更早、更窄、更偏斜且数量更少。将 glitch 跳变及其两个指数恢复项纳入计时解后，八天内平均轮廓稳定至 1%（ glitch 前后宽度变化为 -0.5±0.9%）；若省略恢复项，将因 10⁻⁷ 量级的折叠频率误差模拟出高达 55% 的 glitch 后展宽。PSR J1644−4559 的簇几乎仅在振幅上存在差异，符合散射主导轮廓的预期。对于 PSR J0437−4715，保留峰值优势评分最高的 10% 脉冲可使信噪比翻倍，五簇分解得到的窄相位有序组比平均轮廓窄 3.6±0.4 倍，表明该脉冲星计时阵列目标的基于簇的计时精度可提升约 3.5 倍，待后续论文确认。
英文摘要
The Pulsar Monitoring in Argentina (PuMA) collaboration systematically monitors southern glitching pulsars, maintaining high-cadence single-pulse records of the Vela pulsar. We present a pulse-per-pulse reanalysis of the 2024 major glitch of Vela (PSR~J0835$-$4510) with the 400~MHz-bandwidth ROACH backend of the Argentine Institute of Radioastronomy, and extend our machine-learning single-pulse pipeline---Isolation Forest outlier rejection, $β$-Variational-AutoEncoder denoising, and Self-Organizing-Map clustering---to new observations of PSR~J1644$-$4559 and the millisecond pulsar PSR~J0437$-$4715. For Vela, the 4- and 6-cluster decompositions of the eight days bracketing the glitch reproduce, with seven times the previous bandwidth, the behavior found with the narrow-band ETTUS receivers: higher-amplitude clusters peak earlier in phase, are narrower, more skewed, and less populated. With the glitch jump and its two exponential recovery terms included in the timing solution, the mean profile is stable to 1\% across all eight days (width change $-0.5\pm0.9$\% from pre- to post-glitch); omitting the recovery terms would mimic a post-glitch broadening of up to 55\% through a folding-frequency error at the $10^{-7}$ level. The clusters of PSR~J1644$-$4559 differ almost exclusively in amplitude, as expected for a scattering-dominated profile. For PSR~J0437$-$4715, retaining the 10\% of pulses with the highest peak-dominance score doubles the signal-to-noise ratio, and a five-cluster decomposition yields narrow, phase-ordered groups a factor $3.6\pm0.4$ narrower than the average profile, suggesting a $\sim$3.5-fold improvement in cluster-based timing precision for this pulsar-timing-array target, to be confirmed in a follow-up paper.
Comments20 pages, 6 figures, 5 tables
