论文标题
Perseus I的宇宙舞蹈：会员资格，相空间结构，质量和能量分布
The cosmic DANCe of Perseus I: Membership, phase-space structure, mass, and energy distributions
论文作者
论文摘要
语境。恒星形成区域是测试和验证恒星形成和恒星进化理论的绝佳基准。 Perseus恒星形成区域是最年轻的（<10 Myr）之一，最接近的（280-320 PC），并且在文献中研究了最多，是基本的基准。目标。我们旨在使用公共目录（Gaia，Apogee，2 Mass，Panstarrs）研究Perseus Star形成区域的成员资格，相空间结构，质量和能量（动力学和潜力）分布。方法。我们使用考虑灭绝的贝叶斯方法来识别相位空间中的珀尔修斯物理群，检索其候选成员，得出其特性（年龄，质量，3D位置，3D速度和能量），并尝试重建其起源。结果。我们在七个物理组中识别1052个候选成员（其中一个是新成员），年龄在3至10个MYR，动态的超级病毒状态和大量的能量无绑的恒星中。它们的质量分布与质量> 0.1 $ m_ \ odot $的Chabrier广泛兼容，并且在NGC1333中没有显示出关于IC348的低质量恒星的提示。这些组的年龄，空间结构和运动学与至少三代恒星兼容。仍然需要进行未来的工作来阐明最年轻的最年轻的形成是否是最古老的。结论。 The exquisite Gaia data complemented with public archives and mined with comprehensive Bayesian methodologies allow us to identify 31% more members than in previous studies, discover a new physical group (Gorgophone: 7 Myr, 191 members, and 145 $M_\odot$), and confirm that the spatial, kinematic, and energy distributions of these groups support the hierarchical star-formation scenario.
Context. Star-forming regions are excellent benchmarks for testing and validating theories of star formation and stellar evolution. The Perseus star-forming region being one of the youngest (<10 Myr), closest (280-320 pc), and most studied in the literature, is a fundamental benchmark. Aims. We aim to study the membership, phase-space structure, mass, and energy (kinetic plus potential) distribution of the Perseus star-forming region using public catalogues (Gaia, APOGEE, 2MASS, PanSTARRS). Methods. We use Bayesian methodologies accounting for extinction to identify the Perseus physical groups in the phase-space, retrieve their candidate members, derive their properties (age, mass, 3D positions, 3D velocities, and energy), and attempt to reconstruct their origin. Results. We identify 1052 candidate members in seven physical groups (one of them new) with ages between 3 and 10 Myr, dynamical super-virial states, and large fractions of energetically unbound stars. Their mass distributions are broadly compatible with that of Chabrier for masses >0.1 $M_\odot$ and do not show hints of over-abundance of low-mass stars in NGC1333 with respect to IC348. These groups' ages, spatial structure, and kinematics are compatible with at least three generations of stars. Future work is still needed to clarify if the formation of the youngest was triggered by the oldest. Conclusions. The exquisite Gaia data complemented with public archives and mined with comprehensive Bayesian methodologies allow us to identify 31% more members than in previous studies, discover a new physical group (Gorgophone: 7 Myr, 191 members, and 145 $M_\odot$), and confirm that the spatial, kinematic, and energy distributions of these groups support the hierarchical star-formation scenario.
