船帆座脉冲星前身星的质量与船帆座-船尾座复合体的年龄
The Mass of the Vela Pulsar Progenitor and the Age of the Vela-Puppis Complex
AI总结：
本研究通过测定船帆座脉冲星150 pc内恒星的年龄，推断其前身星性质，发现标准模型预测与观测星群存在不一致，并借助新颖的Stellar Ages算法探讨了双星演化等因素对解决这些差异的作用。
摘要：
船帆座脉冲星与船帆座超新星遗迹的关联长期以来支持了核心坍缩超新星产生中子星的假设，但其周围的恒星群现在为前身星演化提供了新见解。通过对船帆座脉冲星150 pc范围内的恒星进行年龄测定，我们推断出其前身星的性质。这些恒星属于船帆座-船尾座复合体，揭示了该区域的恒星形成历史。虽然采用标准假设的恒星群模型表明了可能的前身星年龄和质量，但这些预测与观测到的星群在内部存在不一致，表明标准建模方法中遗漏了某些因素。在这些假设下，对年龄 $\lesssim$ 10 Myr 的星群仅有非常弱的支持，对 40 Myr 的星群有中等程度支持，而对约 65-100 Myrs 的中等年龄星群则有强烈支持。$\lesssim$ 10 Myr 的信号取决于两颗特殊的 O 型星，它们与船帆座-船尾座复合体中的其他任何恒星都不同，并意味着主序星数量比观测到的多近三倍。40 Myr 的星群由 6 颗红超巨星（RSGs）和几颗 Be 型星支持；但该星群与观测到的主序星分布再次存在边缘性不一致。红巨星（RG）和 MS 的分布与 65-100 Myr 的星群一致。我们讨论了几种可能的解决方案，强调了双星演化和/或极快自转如何解决这些差异。Gaia 视差和 Stellar Ages 促成了这些结果；Stellar Ages 是一种新颖的恒星群建模算法，它结合了个体和星群层面的年龄推断。
英文摘要：
The association of the Vela Pulsar with the Vela Supernova Remnant has long supported the hypothesis that core-collapse supernovae yield neutron stars, but its surrounding stellar population now offers new insights into progenitor evolution. By age-dating stars within 150 pc of the Vela Pulsar, we infer properties of its progenitor. These stars belong to the Vela-Puppis complex, revealing the region's star formation history. While stellar population models with standard assumptions suggest a likely progenitor age and mass, these predictions are internally inconsistent with the observed population, indicating that something is missing in the standard modeling approach. With those assumptions, there is very weak support for a $\lesssim$10 Myr old population, moderate support for a 40 Myr old population, and strong support for an intermediate age population around 65-100 Myrs old. The $\lesssim$10 Myr signal hinges on two peculiar O stars, which are unlike any others in the Vela-Puppis complex and imply nearly three times more main sequence stars than are observed. The 40 Myr-old population is supported by 6 red supergiants (RSGs) and several Be stars; but this population is again marginally inconsistent with the observed distribution of main sequence stars. The red giant (RG) and MS distributions are consistent with a 65-100 Myr old population. We discuss several possible resolutions, emphasizing how binary evolution and/or very rapid rotation could resolve these discrepancies. Gaia parallaxes and {\it Stellar Ages} enable these results; {\it Stellar Ages} is a novel stellar population modeling algorithm that combines individual and population-level age inferences.
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