Abstract Several large neutrino telescopes, operating at various sites around the world, have as their main objective the first detection of neutrinos emitted by a gravitational collapse in the Milky Way. The success of these observation programs depends on the rate of supernova core collapse in the Milky Way, R. In this work, standard statistical techniques are used to combine several independent results. Their consistency is discussed and the most critical input data are identified. The inference on R is further tested and refined by including direct information on the occurrence rate of gravitational collapse events in the Milky Way and in the Local Group, obtained from neutrino telescopes and electromagnetic surveys. A conservative treatment of the errors yields a combined rate R = 1.63 ± 0.46 (100 yr) − 1 ; the corresponding time between core collapse supernova events turns out to be T = 61 − 14 + 24 yr. The importance to update the analysis of the stellar birthrate method is emphasized.

中文翻译：

---

关于银河系核心坍缩超新星的速率

摘要 在世界各地的不同地点运行的几台大型中微子望远镜的主要目标是首次探测到银河系引力坍缩所释放的中微子。这些观测计划的成功取决于银河系中超新星核心坍塌的速度，R。在这项工作中，标准统计技术被用来结合几个独立的结果。讨论了它们的一致性，并确定了最关键的输入数据。通过包括从中微子望远镜和电磁调查中获得的银河系和本星系群中引力坍缩事件发生率的直接信息，进一步测试和完善了对 R 的推论。对错误的保守处理产生组合率 R = 1.63 ± 0.46 (100 yr) − 1 ；核心坍缩超新星事件之间的相应时间结果是 T = 61 - 14 + 24 年。强调了更新恒星出生率方法分析的重要性。