The age-velocity dispersion relation of the Galactic discs from LAMOST-Gaia data

Abstract

We present the age-velocity dispersion relation (AVR) in three dimensions in the solar neighbourhood using 3,564 commonly observed sub-giant/red-giant branch stars selected from LAMOST, which gives the age and radial velocity, and \emph{Gaia}, which measures the distance and proper motion. The stars are separated into metal-poor ($[Fe/H]<-0.2$\,dex and metal-rich ($[Fe/H]>-0.2$\,dex) groups, so that the metal-rich stars are mostly $\alpha$-poor, while the metal-poor group are mostly contributed by $\alpha$-enhanced stars. Thus, the old and metal-poor stars likely belong to the chemically defined thick disc population, while the metal-rich sample is dominated by the thin disc. The AVR for the metal-poor sample shows an abrupt increase at $\gtrsim 7$\,Gyr, which is contributed by the thick disc component. On the other hand, most of the thin disc stars with $[Fe/H]>-0.2$\,dex display a power-law like AVR with indices of about 0.3--0.4 and 0.5 for the in-plane and vertical dispersions, respectively. This is consistent with the scenario that the disc is gradually heated by the spiral arms and/or the giant molecular clouds. Moreover, the older thin disc stars ($>7$\,Gyr) have a rounder velocity ellipsoid, i.e. ${\sigma }_{\varphi }/{\sigma }_{\mathrm{z}}$ is close to 1.0, probably due to the more efficient heating in vertical direction. Particularly for the old metal-poor sample located with $|z|>270$\,pc, the vertical dispersion is even larger than its azimuthal counterpart. Finally, the vertex deviations and the tilt angles are plausibly around zero with large uncertainties.

arXiv comment11 pages, 7 figures, 2 tables, accepted for publication in MNRAS

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