AI 中文总结
本研究利用GWFish框架结合3D超新星波形等数据，评估了爱因斯坦望远镜单独或与Cosmic Explorer协同探测银河系核心坍缩超新星引力波的能力，明确了其探测视界及覆盖范围。
AI 中文摘要
核心坍缩超新星是星系演化的关键驱动因素，也是引力波的有前途来源，引力波为探测其爆发机制的物理过程提供了独特的探针。第三代探测器如爱因斯坦望远镜（Einstein Telescope，ET）将大幅提升探测这些信号的前景。本研究评估了爱因斯坦望远镜单独使用时，以及与宇宙探索者（Cosmic Explorer，CE）等下一代探测器协同使用时，探测核心坍缩超新星引力波的能力。我们估算了银河系及近邻卫星星系中源的探测视界和预期事件率。我们采用GWFish模拟框架，该框架经过定制以纳入来自最新3D模拟的核心坍缩超新星波形目录，以及通过TRILEGAL生成的恒星族群数据。这种方法使我们能够将引力波可探测性建模为前身星质量、源位置和探测器网络配置的函数。我们的分析表明，爱因斯坦望远镜以90%置信度可探测来自PNS驱动的核心坍缩超新星的引力波，其距离范围约为20至超过100千秒差距（kpc），具体取决于前身星质量和波形；而该探测器与其他探测器组成的网络可在最有利情况下将探测范围扩展至约170千秒差距。对于代表性的15倍太阳质量（M☉）前身星，处于2L配置的爱因斯坦望远镜（ET 2L）实现了约100千秒差距的探测视界，确保了对银河系的基本完全覆盖，并对麦哲伦云实现部分覆盖。
英文摘要
Core-collapse supernovae are key drivers of galaxy evolution and promising sources of gravitational waves, which provide a unique probe of the physics driving their explosion mechanism. Third-generation detectors, such as the Einstein Telescope, will dramatically improve the prospects for detecting these signals. This study assesses the capability of the Einstein Telescope, alone and in synergy with next-generation detectors such as Cosmic Explorer, to detect gravitational waves from core-collapse supernovae. We estimate the detection horizons and expected event rates for sources in the Milky Way and nearby satellite galaxies. We employed the GWFish simulation framework, customized to include core-collapse supernovae waveform catalogs from state-of-the-art 3D simulations and stellar population data generated with TRILEGAL. This approach allows us to model gravitational waves detectability as a function of progenitor mass, source position and detector network configuration. Our analysis shows that the Einstein Telescope can detect gravitational waves from PNS-driven core-collapse supernovae up to distances ranging from ~20 to more than 100 kpc with a 90% confidence level, depending on the progenitor mass and waveform, while a combination of this detector in a network can extend the reach up to ~170 kpc in the most favorable cases. For a representative 15 M_sun progenitor, ET (in its 2L configuration) achieves a detection horizon of ~100 kpc, ensuring essentially complete coverage of the Milky Way and partial coverage of the Magellanic Clouds.
