AI 中文总结
该研究利用Gaia星团样本的轨道积分等方法，重建了太阳近邻50百万年的恒星形成与核心坍缩超新星历史，得到了时间分辨的近邻超新星活动图，为研究大质量恒星反馈与本地星际介质的关联提供了经验框架。
AI 中文摘要
我们通过年轻星团的过去轨迹，重建了太阳近邻区域近期的恒星形成历史与核心坍缩超新星（ccSN）历史。利用基于盖亚（Gaia）的星团样本，该样本包含新推导的年龄、质量和整体三维速度，我们在假设的轴对称银心势中向后积分轨道，并结合初始质量函数（IMF）采样与恒星寿命，推断出过去50百万年（Myr）内的ccSN发生时间与位置。研究结果得到了全天球、三维、时间分辨的近邻ccSN活动图，可用于与本地星际介质的高分辨率三维视图进行对比。0-15 Myr的图显示，猎户座、船帆座、天蝎座-半人马座（Sco-Cen）和仙王座方向存在强烈的ccSN增强，许多增强区域位于现今的空洞和壳层内。更早时期，主要的增强区域对应科林德135（Collinder 135）、梅西耶6（Messier 6）和英仙座α星团家族，展现了大质量恒星形成区的遗迹如何塑造了近期本地反馈历史。我们恢复了爆发式的恒星形成历史，随后是延迟、更平缓的ccSN历史。在过去40 Myr中，平均恒星形成率为823倍太阳质量每百万年（\u0024823~M_\u0026#8857;~\u0026#926;Myr\u0026#8722;1\u0024），平均ccSN率为7.7每百万年（\u00247.7~\u0026#926;Myr\u0026#8722;1\u0024），对应银河系的ccSN率为0.55±0.03每世纪（\u00240.55\u0026#177;0.03~\u0026#926;century\u0026#8722;1\u0024）。现今的OB星表得出的ccSN率范围，从与星团重建结果一致到高出数倍不等。由于这些星表重叠度低且需要不同的校正，我们未对ccSN图进行缩放。我们的重建提供了一个经验框架，用于将大质量恒星反馈的近期历史与近邻银河系中气体的三维结构和生命周期联系起来。
英文摘要
We reconstruct the recent star formation and core-collapse supernova (ccSN) histories of the Solar Neighborhood from the past trajectories of young star clusters. Using a \textit{Gaia}-based cluster sample with newly derived ages, masses, and bulk 3D velocities, we integrate orbits backward in an assumed axisymmetric Galactic potential and combine the trajectories with IMF sampling and stellar lifetimes to infer ccSN times and locations over the past 50 Myr. The result is an all-sky, 3D, time-resolved map of nearby ccSN activity for comparison with high-resolution 3D views of the local interstellar medium. The 0--15 Myr map shows strong enhancements toward Orion, Vela, Sco--Cen, and Cepheus, many within present-day cavities and shells. At earlier times, the dominant enhancements trace the Collinder 135, Messier 6, and Alpha Persei cluster families, showing how the remnants of massive star-forming complexes have shaped the recent local feedback history. We recover a bursty star formation history followed by a delayed, smoother ccSN history. Over the last 40 Myr, the mean star formation and ccSN rates are \(823~M_\odot~\mathrm{Myr}^{-1}\) and \(7.7~\mathrm{Myr}^{-1}\), respectively, corresponding to a Milky Way rate of \(0.55\pm0.03~\mathrm{century}^{-1}\). Present-day OB-star catalogs yield rates ranging from agreement with the cluster reconstruction to several times higher. Because the catalogs overlap weakly and require different corrections, we do not rescale the ccSN map. Our reconstruction provides an empirical framework for connecting the recent history of massive-star feedback to the 3D structure and life cycle of gas in the nearby Milky Way.
Comments27 pages, 9 figures. Submitted to ApJ. Comments are welcome. An interactive 3D version of Figures 2 and 3 is available at https://cswigg.github.io/cam_website/oviz_figures/oviz_supernovae.html
