论文标题
500 Myr Old Open Cluster M37中的行星星云
The Planetary Nebula in the 500 Myr old Open Cluster M37
论文作者
论文摘要
我们报告了一个大型，进化的，双极行星星云及其蓝色，白色矮人中央之星，是〜500 Myr旧的银河开放式星团M37（NGC 2099）的成员。这只是银河开放群集中行星星云的第三个已知例子，是通过我们正在进行的识别和研究行星星云的持续计划找到的。对该关联的置信度很高，来自盖亚（Gaia）确认的中央恒星和簇星的一致径向速度以及适当的运动，在潮汐群集边界内良好的行星星云的红色一致性和位置。有趣的是，所有三个银河系示例均具有双极形态和可能的I型化学，这都是较高质量祖细胞的特征。在这种情况下，祖细胞星质量处于〜2.8 msun的中间距离。它在关键的恒星初始质量关系上提供了一个有价值的，附加的点，与群集白矮人估计无关，并且在抽样较差的质量区域的间隙中也落在一个间隙中。这个行星星云似乎也具有有史以来最大的运动年龄，这意味着当它们位于簇中时，可见度寿命提高。
We report confirmation of a large, evolved, bipolar planetary nebula and its blue, white dwarf central star as a member of the ~500 Myr old Galactic open star cluster M37 (NGC 2099). This is only the third known example of a planetary nebula in a Galactic open cluster and was found via our on-going program of identifying and studying planetary nebulae - open cluster associations. High confidence in the association comes from the consistent radial velocities and proper motions for the confirmed central star and cluster stars from Gaia, reddening agreement and location of the planetary nebula well within the tidal cluster boundary. Interestingly, all three Galactic examples have bipolar morphology and likely Type I chemistry, both characteristics of higher mass progenitors. In this case the progenitor star mass is in the mid-range of ~2.8 Msun. It provides a valuable, additional point on the key stellar initial-to-final mass relation independent of cluster white dwarf estimates and also falls in a gap in the poorly sampled mass region. This planetary nebula also appears to have the largest kinematical age ever determined and implies increased visibility lifetimes when they are located in clusters.
