Age–metallicity dependent stellar kinematics of the Milky Way disc from LAMOST and Gaia. Issue 4 (19th January 2021)

• Record Type: Journal Article
• Authors: Wu, Yaqian; Xiang, Maosheng; Chen, Yuqin; Zhao, Gang; Bi, Shaolan; Li, Chengdong; Li, Yaguang; Huang, Yang
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 501:Issue 4(2021)
• Page Start: 4917
• Page End: 4934
• Publication Date: 2021-01-19
• Subjects: catalogues -- disc -- galaxy: fundamental parameters -- galaxy: kinematics and dynamics; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa3949
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We investigate the stellar kinematics of the Galactic disc in 7 < R < 13 kpc using a sample of 118 945 red giant branch (RGB) stars from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and Gaia . We characterize the median, dispersion and skewness of the distributions of the three-dimensional stellar velocities, actions and orbital parameters across the age–metallicity and the disc R – Z plane. Our results reveal abundant but clear stellar kinematic patterns and structures in the age–metallicity and the disc R – Z plane. The most prominent features are the strong variations of the velocity, action and orbital parameter distributions from the young, metal-rich thin disc to the old, metal-poor thick disc; a number of smaller-scale structures (such as velocity streams, north–south asymmetries, and kinematic features of spiral arms) are clearly revealed. Particularly, the skewness of V ϕ and J ϕ reveals a new substructure at R ≃ 12 kpc and Z ≃ 0 kpc, possibly related to dynamical effects of spiral arms in the outer disc. We further study the stellar migration by analysing the stellar orbital parameters and stellar birth radii. The results suggest that the thick disc stars near the solar radii and beyond are mostly migrated from the inner disc of R ∼ 4−6 kpc as a result of their highly eccentrical orbits. Stellar migration resulting from dynamical processes with angular momentum transfer (churning) is prominent for both the old, metal-rich stars (outward migrators) and the young metal-poor stars (inward migrators). The spatial distribution in the R – Z plane for the inward migrators born at a Galactocentric radius of >12 kpc shows clear age stratifications, possibly evidence that these inward migrators are consequences of splashes triggered by merger events of satellite galaxies that have lasted the past few Gyr.