标题： 利用Pystoch潜力：从有趣的超新星遗迹目标中探测连续引力波 显示英文标题

标题： Harnessing PyStoch potential: detecting continuous gravitational waves from interesting supernova remnant targets

摘要： 检测连续引力波（CWs）具有挑战性，因为它们的振幅较弱且计算需求高，尤其是在源参数约束较差的情况下。 使用交叉相关技术的随机引力波背景（SGWB）搜索可以以较低的计算成本识别未解析的天体物理源，包括CWs，尽管灵敏度有所降低。 这促使采用一种混合方法，其中SGWB算法作为第一阶段过滤器，用于识别后续专用CW管道的CW候选者。 我们评估了SGWB分析工具Pystoch检测CWs的发现潜力，使用来自自转减速中中子星的模拟信号。 然后我们将该方法应用于第三LIGO-Virgo-KAGRA观测运行（O3）的数据，覆盖（20-1726）Hz频率范围，并针对四个超新星遗迹：Vela Jr.、G347.3-0.5、Cassiopeia A和与1987A超新星遗迹相关的中子星。 如有必要，使用5向量重采样和带采样数据频率-霍夫技术对显著候选者进行后续研究。 然而，由于在真实的O3分析中没有发现有趣的候选者，我们设定了95%置信水平的CW应变幅度上限$h_0$。 最严格的限制是针对Cassiopeia A获得的，在$201.57$ Hz处为$h_0 = 1.13 \times 10^{-25}$，频率分辨率为$1/32$ Hz。 至于其他目标，已使用相同的频率分辨率设定了最佳上限，分别对应于G347.3-0.5的$h_0 = 1.20 \times 10^{-25} $在$202.16$Hz，Vela Jr.的$1.20 \times 10^{-25}$在$217.81$Hz，以及1987A超新星遗迹中的中子星的$1.47 \times 10^{-25}$在$186.41$Hz。 显示英文摘要

摘要： Detecting continuous gravitational waves (CWs) is challenging due to their weak amplitude and high computational demands, especially with poorly constrained source parameters. Stochastic gravitational-wave background (SGWB) searches using cross-correlation techniques can identify unresolved astrophysical sources, including CWs, at lower computational cost, albeit with reduced sensitivity. This motivates a hybrid approach where SGWB algorithms act as a first-pass filter to identify CW candidates for follow-up with dedicated CW pipelines. We evaluated the discovery potential of the SGWB analysis tool PyStoch for detecting CWs, using simulated signals from spinning down NSs. We then applied the method to data from the third LIGO-Virgo-KAGRA observing run (O3), covering the (20-1726) Hz frequency band, and targeting four supernova remnants: Vela Jr., G347.3-0.5, Cassiopeia A, and the NS associated with the 1987A supernova remnant. If necessary, significant candidates are followed up using the 5-vector Resampling and Band-Sampled Data Frequency-Hough techniques. However, since no interesting candidates were identified in the real O3 analysis, we set 95\% confidence-level upper limits on the CW strain amplitude $h_0$. The most stringent limit was obtained for Cassiopeia A, and is $h_0 = 1.13 \times 10^{-25}$ at $201.57$ Hz with a frequency resolution of $1/32$ Hz. As for the other targets, the best upper limits have been set with the same frequency resolution, and correspond to $h_0 = 1.20 \times 10^{-25} $ at $202.16$ Hz for G347.3-0.5, $1.20 \times 10^{-25}$ at $217.81$ Hz for Vela Jr., and $1.47 \times 10^{-25}$ at $186.41$ Hz for the NS in the 1987A supernova remnant.