标题： 全天搜索第四次LIGO-Virgo-KAGRA观测运行第一部分中的短时引力波爆发 显示英文标题

标题： All-sky search for short gravitational-wave bursts in the first part of the fourth LIGO-Virgo-KAGRA observing run

摘要： 我们对来自Advanced LIGO-Virgo-KAGRA第四次观测运行（称为O4a）前八个月数据中的短时引力波瞬变进行了搜索。 我们使用了四种分析方法，这些方法对持续时间长达几秒的广泛潜在信号敏感，频率范围为16-4096 Hz。 排除了已经通过低延迟分析识别出的双黑洞合并候选者后，我们没有发现其他引力波瞬变的统计显著证据。 我们测量了针对代表性信号的搜索灵敏度，包括正弦高斯波形、高斯脉冲和不同频率和持续时间的白噪声爆发，并采用每100年一次误报率为检测阈值。 根据信号类型，我们在应变幅度灵敏度和源速率密度的90%置信上限方面，相比之前的搜索提高了2到10倍。 我们还评估了各种核心坍缩超新星模型，发现对于某些模型，该搜索可能在整个银河系中探测到恒星核心坍缩的引力波。 最后，我们考虑了与脉冲星跳变相关的中子星f模，并发现假设源类似于Vela脉冲星，该搜索可能探测到频率变化比例小至$\sim 2$到$6 \times 10^{-5}$的跳变引力波信号，具体取决于中子星质量。 显示英文摘要

摘要： We present a search for short-duration gravitational-wave transients in data from the first eight months of Advanced LIGO-Virgo-KAGRA's fourth observing run, denoted O4a. We use four analyses which are sensitive to a wide range of potential signals lasting up to a few seconds in the 16-4096 Hz band. Excluding binary black hole merger candidates that were already identified by low-latency analyses, we find no statistically significant evidence for other gravitational-wave transients. We measure the sensitivity of the search for representative signals, including sine-Gaussians, Gaussian pulses, and white-noise bursts with different frequencies and durations, adopting a false alarm rate of 1 per 100 years as detection threshold. Depending on signal type, we find improvements over previous searches by factors of 2 to 10 in terms of sensitivity to strain amplitude and of 90% confidence upper limit on the rate density of sources. We also evaluate a variety of core-collapse supernova models and find that, for some models, the search could have detected gravitational waves from stellar core-collapse throughout the Milky Way. Finally, we consider neutron star f-modes associated with pulsar glitches and find that, assuming a source similar to the Vela Pulsar, the search could have detected a gravitational-wave signal from a glitch with fractional frequency change as small as $\sim 2$ to $6 \times 10^{-5}$ depending on the neutron star mass.