Using a sample of 96,201 primary red clump (RC) stars selected from the LAMOST and Gaia surveys, we investigate the stellar structure of the Galactic disk. The sample stars show two separated sequences of high-[α/Fe] and low-[α/Fe] in the [α/Fe]-[Fe/H] plane. We divide the sample stars into five mono-abundance populations (MAPs) with different ranges of [α/Fe] and [Fe/H], named as the high-[α/Fe], high-[α/Fe] & high-[Fe/H], low-[Fe/H], solar, high-[Fe/H] MAPs respectively. We present the stellar number density distributions in the R R Z plane, and the scale heights and scale lengths of the individual MAPs by fitting their vertical and radial density profiles. The vertical profiles, the variation trend of scale height with the Galactocentric radius, indicate that there is a clear disk flare in the outer disk both for the low-[α/Fe] and the high-[α/Fe] MAPs. While the radial surface density profiles show a peak radius of 7 kpc and 8 kpc for the high-[α/Fe] and low-[α/Fe] MAPs, respectively. We also investigate the correlation between the mean rotation velocity and metallicity of the individual MAPs, and find that the mean rotation velocities are well separated and show different trends between the high-[α/Fe] and the low-[α/Fe] MAPs. At last, we discuss the character of the high-[α/Fe] & high-[Fe/H] MAP and find that it is more similar to the high-[α/Fe] MAP either in the radial and vertical density profiles or in the rotation velocity.
Mapping the Galactic disk with the LAMOST and Gaia Red clump sample: VIII: Mapping the kinematics of the Galactic disk using mono-age and mono-abundance stellar populations
Mapping the Galactic disk with the LAMOST and Gaia Red clump sample. II. 3D asymmetrical kinematics of mono-age populations in the disk between 6$-14$ \,kpc
我们进行分析的三维运动学的银河系盘星在单年龄人口。从LAMOST DR 4红团巨星和Gaia DR 2自行星表中选取银心距离在$R=6$和14 kpc之间的恒星。我们证实了最近工作的三维非对称运动，并提供了银心距离为14，kpc的反中心方向附近的银河系外盘非对称运动的时间标记。径向银心运动的值达到10公里秒$^{-1}$，这取决于人口的年龄，并提出了一个南北不对称的区域对应的密度和速度的子结构，是敏感的扰动在早期6 \，Gyr。在那之后，在这种不对称结构中的盘星在运动学上变得更热，因此对扰动不敏感，我们发现这种结构是一个相对年轻的种群。通过定量分析，我们发现在平面之上和之下的$R\gtrsim 9$ kpc处的恒星都表现出弯曲模运动，其敏感持续时间约为8 \，Gyr。我们推测，面内不对称可能主要是由快速旋转的酒吧，本质上椭圆形的外盘，长期膨胀的磁盘，或流。螺旋臂动力学、不平衡模型、小型兼并或其他因素都是重要的贡献者。垂直运动可能由复杂的内部或外部扰动引起的弯曲和呼吸模式主导。这些机制中有许多可能是相互关联的。
Identifying Galactic Halo Substructure in 6D Phase-space Using $\sim$13,000 LAMOST K Giants
我们通过结合超过13，000个LAMOST DR 5晕K巨星的位置，距离，径向速度和金属丰度与盖亚DR 2自行，它覆盖了银河系中心距离范围为5-120 kpc。使用位置-速度聚类估计器（6距离），我们统计量化的位置-速度子结构的存在，在高的意义：K巨星有更多的位置-速度空间比一个光滑的恒星晕密切的对。我们发现，在晕的子结构的数量增加，随着距离和金属丰度。利用一种名为Friends-of-Friends（FoF）的逾渗算法来识别星群，我们识别出了人马座（Sgr）星流、麒麟座星环、室女座超密度星、武仙座-天鹰座星云、孤儿星星流以及其他未知的子结构，发现人马座星流在20 kpc以上的星群中占了很大一部分，并增强了子结构随距离和金属丰度的增加。首次在银河南北半球确定了麒麟座环的光谱成员，其自转速率约为185 km s^{-1}，平均金属丰度为-0.66 dex。
Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Stellar-mass black holes in young massive and open stellar clusters -- VII. Comparisons with gravitational-wave events until LVK-O4a and Gaia compact binaries
Helmholtz-Instituts für Strahlen- und Kernphysik (HISKP)（亥姆霍兹射线与核物理研究所）
The structure and evolution of the Galactic high-$α$ disc I. Chemical and age orbital cartography
Institute of Graduate Studies in Science, Istanbul University（伊斯坦布尔大学高等研究院）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Faculty of Science, Department of Astronomy and Space Sciences, Istanbul University（伊斯坦布尔大学理学院天文与空间科学系）
