A Census of the beta Pic Moving Group and Other Nearby Associations with Gaia

K. L. Luhman
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Abstract

I have used the third data release of the Gaia mission to improve the reliability and completeness of membership samples in the beta Pic moving group (BPMG) and other nearby associations with ages of 20-50 Myr (Sco Body, Carina, Columba, chi1 For, Tuc-Hor, IC 2602, IC 2391, NGC 2547). I find that Carina, Columba, and chi1 For are physically related and coeval, and that Carina is the closest fringe of a much larger association. Similarly, Tuc-Hor and IC 2602 form a coeval population that is spatially and kinematically continuous. Both results agree with hypotheses from Gagne et al. (2021). I have used the new catalogs to study the associations in terms of their initial mass functions, X-ray emission, ages, and circumstellar disks. For instance, using the model for Li depletion from Jeffries et al. (2023), I have derived an age of 24.7+0.9/-0.6 Myr for BPMG, which is similar to estimates from previous studies. In addition, I have used infrared photometry from the Wide-field Infrared Survey Explorer to check for excess emission from circumstellar disks among the members of the associations, which has resulted in a dramatic increase in the number of known disks around M stars at ages of 30-50 Myr and a significant improvement in measurements of excess fractions for those spectral types and ages. Most notably, I find that the W3 excess fraction for M0-M6 initially declines with age to a minimum in BPMG <0.015), increases to a maximum in Carina/Columba chi1 For (0.041+0.009/-0.007, 34 Myr), and declines again in the oldest two associations (40-50 Myr). The origin of that peak and the nature of the M dwarf disks at >20 Myr are unclear.
贝塔皮克移动小组及其他与盖亚有关的邻近地区普查
我利用盖亚(Gaia)任务发布的第三次数据,提高了β皮克移动群(BPMG)和其他年龄在20-50 Myr的附近星团(Sco Body、Carina、Columba、chi1 For、Tuc-Hor、IC 2602、IC 2391、NGC 2547)成员样本的可靠性和完整性。我发现船底座、哥伦布和chi1 For在物理上是相关的,而且是共生的,船底座是一个大得多的联合体的最接近的边缘。同样,Tuc-Hor 和 IC 2602 形成了一个在空间和运动学上连续的共生族群。这两个结果都与加涅等人(2021 年)的假设一致。我利用新的目录从初始质量函数、X射线发射、年龄和周星盘等方面对这些联系进行了研究。例如,利用 Jeffries 等人(2023 年)的锂耗尽模型,我推算出 BPMG 的年龄为 24.7+0.9/-0.6 Myr,这与之前研究的估计值相似。此外,我还利用宽视场红外巡天探测器(Wide-field-Infrared Survey Explorer)的红外测光来检查星团成员中是否有来自周星盘的过量发射,结果发现年龄在30-50 Myr的M星周围的已知周星盘的数量急剧增加,对这些光谱类型和年龄的过量分数的测量结果也有了显著改善。最值得注意的是,我发现M0-M6的W3过剩分率最初会随着年龄的增长而下降,到BPMG 20 Myr的最小值还不清楚。
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