11 Mpc以内的核坍缩超新星速率合成
Core-Collapse Supernova Rate Synthesis Within 11 Mpc
摘要：
11 Mpc H-alpha和紫外星系巡天（11 HUGS）追踪了附近星系的恒星形成活动。此外，在本卷中，核心坍缩超新星（CCSNe）的探测完整性很高，因此通过比较这些观察到的恒星出生和死亡，我们可以对我们对恒星如何生存和死亡的理解进行敏感的测试。利用双星星族和光谱合成（BPASS）程序的计算结果，对11个HUGS星系H-α和远紫外（FUV）恒星形成速率指示器（SFRIs）进行了模拟，同时匹配了核心坍缩超新星（CCSN）速率。我们发现，恒星星族，包括相互作用的双星，使总CCSN率的差异不大，但增加了恒定数量的恒星正在形成的H-α和FUV通量。此外，他们显着增加预测的Ibc型超新星（SNe）相对于II型SNe的11 HUGS星系中观察到的水平。我们还发现，而不是假设一个恒定的恒星形成历史（SFH）的星系，我们最好的拟合模型有一个恒星形成率（SFR），超过3百万年前达到峰值。
英文摘要：
The 11 Mpc H-alpha and Ultraviolet Galaxy (11HUGS) Survey traces the star formation activity of nearby galaxies. In addition within this volume the detection completeness of core-collapse supernovae (CCSNe) is high therefore by comparing these observed stellar births and deaths we can make a sensitive test of our understanding of how stars live and die. In this paper, we use the results of the Binary Population and Spectral Synthesis (BPASS) code to simulate the 11HUGS galaxies H-alpha and far-ultraviolet (FUV) star formation rate indicators (SFRIs) and simultaneously match the core-collapse supernova (CCSN) rate. We find that stellar population including interacting binary stars makes little difference to the total CCSN rate but increases the H-alpha and FUV fluxes for a constant number of stars being formed. In addition they significantly increase the predicted rate of type Ibc supernovae (SNe) relative to type II SNe to the level observed in the 11HUGS galaxies. We also find that instead of assuming a constant star formation history (SFH) for the galaxies our best fitting models have a star formation rate (SFR) that peaked more than 3 Myrs ago.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
